ReaB)-t:o
better»T»ea3
Jj ije - Natuve-all tmn3s.
STAR ATLAS CONTAINING Maps
of all the Stars from 1 to 6.5 Magnitude between the North Pole and 34"
South Declination, and of
all
Nebul$ and Star Clusters in the same region whicli are
visible in
telescopes of moderate powers.
mit\)
Cjcjplanatorj)
Cejrt
BY
DR.
HERMANN
J.
KLEIN.
TRANSLATED, AND BROUGHT UP TO DATE BY
EDMUND MCCLURE,
M.A.,
M.R.LA.,
F.L.S.
WITH EIGHTEEN MAPS. BY
PE/IlsTTBD
B.
.A.,
IFUITKE, XjEIE'SIC.
PUBLISHED UNDER THE DIRECTION OF THE COMMITTEE OF GENERAL LITERATURE AND EDUCATION APPOINTED BY THE SOCIETY FOR PROMOTING CHRISTIAN KNOWLEDGE.
lonlian SOCIETY FOR PROMOTING CHRISTIAN KNOWLEDGE, NORTHUMBERLAND AVENUE,
W.C.
BRIGHTON:
NEW YORK
:
E.
QUEEN VICTORIA STREET, 43, NORTH STREET. & J. B. YOUNG & CO.
135,
1893.
E.C
NOTICE OF THE TRANSLATOR TO THE SECONI> ENGLISH EDITION.
Translator has in this second English Edition
ipT^iHE
endeavoured to bring up
date
to
Dr. Klein's descriptions of the more interesting Fixed Stars, Star Clusters, and Nebula}. matter
additional
All
been
has
included in
brackets,
anything like completeness has not been aimed the most helpful
Note is
recent researches
to
p.
iii.]
further
of
allow
me
The to
Astronomy
disposal
on
notice
to
for
fact
the
benefit
the
those
of
the
the
31st
present in the sky, were Klein's 'Star
While
notes.
has examined records of
further
details
which have
discovery
Nature,
was
made by
my
your readers, that
of
meagrest ult.,
Atlas'
been
may be
as
when
My
was
is
—"You one
knowledge of the
description I
case
;
and
sure
all
that
the
of
aid
and
and
added,
the
February 18th, 1892, says:
even the humblest amateurs. of
such
furnishing
among
that
(o
the Translator
as
recently discovered JTova in Auriga [p. 25
of the
writing
unfortunately,
morning
of
important
least
from the
state,
is,
the
the
discoverer
encouragement
afford
of
not
is
interest
"Star Atlas." also
The
the student.
to
with the view
at,
appended
or
it
this
might
that
can
technicalities
means
a strange
at
my
body was
and a small pocket telescope which magnifies
ten times."
Odohcr, 1892.
k:553
TABLE OF CONTENTS.
—
IV Page
39 Double Star
£ 1919 „ £ 192G „ ^ l^
"
.
Canis major, The Great Dog.
48 48 48 48 48 49
Triple Star
(Sheet VIII.)
a Sirius 1454 Star Cluster Double Star 1479 Star Cluster
/J,
^
Camelopardalis, The Giraffe.
62 Double Star i) 385 „ 2 390 „ 2 396
1
.
.
5
Ji Variable
801 Is'ebula
2d
S
S
20
a Procyon
21
14 Triple Star
22 22 22 23 29 33 34 34
1617 Nebula
485 Double Star
7 Triple Star 940 Star Cluster 2 634 Double Star 2 780 Triple Star 2 1051 „ 1541 Nebula 2 1127 Triple Star 1691 Nibulii .
.
.
.
.
.
.
.
.
„
.
a'
a.'
Double Star
TT
„
.
,,
.
.
64 64 64 64 66
.
68
.
.
.
(p-
•
Double Star
1681 Star Cluster iS'
Variable
.
Double Star 1712 Star Cluster r Double Star 1
.
a
,,
66 67
2
1311 „
(Sheet
Canes venatici, The Hounds.
y
2
3002 Nebula 3041
"
.
.
.
.
.
.
3042 „ 3165 (Sheet XVIII.) ,, 3258 ,, £ 1692 Double Star
43 43 44 44
17
„
3437 Nebula 3474 ,,
.
,,
.
.
XVI.) .
.
45
.45
... .
(Sheet 25 Double Star 3636 Star Cluster 13572
.
46 46
.46 .
47
361
.
.
a Variable
120 Star Cluster. Double Star .
y
.
Variable 250 Star Cluster
.
.
XVII.)
(Sheet
.
.14 .14 .14
.
Triple Star 341 Star Cluster.
r|/
.
.
.
(Sheet XVII.)
,,
Triple Star 5031 Star Cluster
15
.17
i
.
H
....71
c-
.
(Sheet
71
Variable Double Star
.
.
.
.
.71
Centaurus, The Centaur. (Sheet X.) [^Important stars are heyond the
.
I.,
Z7 Variable
II., v., .
.
S 460 Double Star
.
X
.
,,
Variable
.13 .20 .
...
4590 Star Cluster
T
VI.)
X 2780 Double Star
.
.
.
.
64 65 67 67
.17 .17
.
.
17
.
.
.70
.
.
.
.
Double Star 4957 Star Cluster .
70 70
Columba, The Dove. (Sheet VIII.)
Coma
Berenices, Berenice's Hair. (Sheet IV., X.)
... ... ....42 .42 ... ...
2 Double Star 2752 Star Cluster
.
2786 Nebula 2838 „ 12 Double Star 2890 Nebula 2946 ,, 2972 „ 17 Double Star 3043 Nebula 24 Double Star 3101 Nebula 3106 „ S 1678 Double Star .
.
.
;
.
.
.
.
42 42 42 42
42 43 43
.43 ... ... ... ....45 .
„
.
(Sheet
17 17
.
3342 Nebula 42 Double Star 3453 Star Cluster
Cepheus.
.
.
a Triple Star
35
scope of this Atlas.']
.
69 69 69 69
S 2872 „ 2 2883 „ S 2893 ,,
13
„
S
.15 .16
.
....18 ... ... ... ... .69
„
1
.13 .13
.
....14
»
1.5
.
.
.
.
.
,
11
.
.
.
.
.
70
14 14
„
^ Variable
11
.
544 Planetary Nebula * Double Star . 600 Nebula 604 „ 94 Double Star
VI.)
.11 .11
.
Star (Mira) Variable
.11 ....12
63 Star Cluster 68 „
.
15,
.
.
Variable.
XVII.) 42 42 42
.43 ... ... ....45
,,
II., III., v.,
Novaofl572 (ShcetXVIII.)
(Sheet III., IV., V.)
...
I.,
B Double Star
392
2723 Nebula 2 1606 Double Star
.
.
13
X Double
64 64
•
/3
.
.
....11 .13 ... ... ...
42 342 Nebula
E .
.70 .70
(Sheet VII.)
Goat.
.
.
68 68 69
The Whale.
Variable 138 Nebula 26 Double Star
(Sheet XII.)
(Sheet III., IV., IX.)
„
Cetus,
.
.
.
.
He
.
67 67 68
.68
.
Triple Star . Double Star 4957 Star Cluster
35
.
.
.
TT
....36
Capricornus, The
Cancer, The Crab.
^
33
.
.
„ 4709 Star Cluster Z 2840 Double Star
.33 .34 .34
„
36 36 36 36 36 36 36 36 36 37 37 37 37 37 37
.
.
...
.
S
4608 Star Cluster 4687 „ Cassiopeia.
^ Triple Star
3;5
.
.
Variable
/x
(Sheet VIII.)
36
Ji Variable.
.
„ „
Canis minor, The Little Dog.
18 18 19
1
.
1511 Nebula (Sheet XVIII. ) 1512 Star Cluster 1513
VI.)
III., lY.,
I., ir.,
.
.
.
.
S
32 32 32 33 33 33
.
.
„
B 2 2816
31
.
.
7 Variable
(Sheet
2 2790 Double Star
.
.
.
.
.
43 43 43 44 45 45
.
.
.
45
Corona borealis,The Northern Crown. (Sheet IV., V., VI.)
X
U
1
932 Double Star
Variable
.
. .
.
49
.49
—
V
—
»)
49 49 50 50 50 50 50
Variable Double Star
2 1964 „ y
).
Jt Variable
T
Nova
a-
Double Star
V
Multiple Star
51 51
CorYUS, The Crow.
Crater,
.
.
.
.
50 52 52
Multiple Star X Double Star
16, 17
52 54
T
.42 .
43
b
„
4415 Nebula (p Double Star X 2403 „ 4517 Star Cluster Double Star E
The Cup. Equuleus, The Foal. (Sheet XII.)
Cygnus, The Swan. I., II., .
.
„ 4614 Nebula 17 Double Star S-
v.,
.
.
:Z' Variable. ^ Triple Star 59 Double Star /' Triple Star 61 Double Star
Nebula
.
.
.
.
.
.
65 65 65 66
66 66
.
.
.
.
67 67 68
.68
.
.
.
68
(Sheet v., XII.) .
a Multiple Star
T
Variable y Double Star .
4625 Nebula
.
G4
.
.
.
.
.
.
.
.
.65 .65 .65 .65
.
.
.
66
Draco, The Dragon. (Sheets
I.,
2024 Nebula 4029 „
III., IV., v., VI.)
.39
... .
.
48
Hercules. (Sheet
IV., v., VI., XI.)
I.,
2 2007 Double Star
30,
m
</
„
.
Double Star
.
42
4230 Star Cluster (Sheet XVII., XVIII.) 4234 Nebula S 2101 Double Star 4244 Nebula S 2104 Double Star
S
Variable
Double Star 4294 Star Cluster i
.18 .18
.
....19
692 Nebula 709 „ S 422 Double Star 32 „ A „ 826 Nebula .
.
18
.
.
.
19
.
.
20
.20 ....22 .
Triple Star 55 Double Star 0^
„
b
•
21
.
.
.
,
.
(Sheet
II., III.,
fi.
„ Triple Star
4343 Nebula 95 Double Star Z 2277 „ 100
r
Variable
/*
Double Star
Double Star
.
.
.
.
.
.
.
38 „ 1467 Star Cluster ^ Variable
.
.
Jc
110
.
.
.
.
.
.
1490 Star Cluster 1508 „ X Double Star i „ 1534 Star Cluster «, Double Star 1 549 Star Cluster
... ... ...
S
Variable
(Sheet IX., X.)
29 29 30 30 30
32
....
,,
.
.
.
.
.... .
67
57 59
Star
22
....31 ....31 .
57 57
Hydra.
... ....
«
.
Variable.
2 2289 Double
VIII.) .
54 55 55 55 55 56 56 56 66
Double Star 2190 ,,
Gemini, The Twins. 1325 Star Cluster 1360 ,,
(Sheet
.
83 2215
•£
53 53 53 53 53 53
54 54
.
f
(Sheet VII., VIII.) .
52 52 52 52 52 52
U Variable
7.
12 Double Star
51 51
68, u Variable
Eridanus, The River Eridanus.
c
.
Multiple Star
15 „ y Triple Star
Delphinus, The Dolphin. 4)86 Nebula g Triple Star
,,
Variable
XV.)
.66 .67
.
4681 Star Cluster Nova 1870 ^ Quadruple Star .
64 65
.
... ...
„
j3
63 63
.64
.
.
.
.4345 Star Cluster T Double Star V
Triple Star
....65 ... ... ... ... ... ...
.
.
2744
62
.62 .62 .63
.
.
.
4600 Nebula 52 Double Star
61
.
.
F
.
62 62
. X Variable 4. Double Star 4544 Stai- Cluster 32 0- Double Star Variable . 4575 Star Cluster 49 Double Star
Triple Star Double Star
.
.
66 66 66 66 67 67 67
2735 Double Star
VI.)
....61 .62 ... ...
B Variable „ 4511 Star Cluster 16 Double Star
li
55 56 56 57 57 58 58 58 59 62 62
4373 Nebula 40, 41 Double Star
(Sheet Xir.)
(Sheet
85 35 35 35 35
Z 1984 Double Star 99
39
(Sheet IX., X.) i? Variable i Double Star
Paga
rage
Page
S
.
32
2 6 ]
1245 Double Star Multiple Star 5 Triple Star
S
'N'ariable
36 37 37 37 37 37 38 39 41 44 46
.
.
T S Double Star 2102 Nebula Double Star 3128 Nebula
ir2
33 33 33 33 33 34 34 34 34
2i Variable
Lacerta, The Lizard. (Sheet
4755
Star
II.,
XVII.)
V.)
....69
Cluster
(Sheet
69
4773 „ 8 Quadruple Star
.
.
.
.
69
VI
— rage
Page
Lynx.
Lepus, The Hare. (Sheet
R •
«
(Sheet
Vin.) 22 23 23 24 24 25 25 28 29
Variable Double Star
„
5 Triple Star 1112 Star Cluster ^ Multiple Star a. Double Star .
.
45 Multiple Star y Double Star
12
„
£ 958 Double Star 14 19
„ „ „
2 1333
„
2 1009
38 „ 1811 Nebula 39 Double Star
IV.)
... ... ...
II., III.,
I.,
4 Double Star 5 Triple Star
.
.
.
.
.
.
.
.
.
.
... ... .
.
30 30 31 31
32 32 33 38 38 38 38
Leo, The Lion.
Lyra, The Lyre.
(Sheet III., IV., IX.)
38 38 38 38 38 38 39 39
u Double Star
1861 Nebula 1863 „ 6 Double Star " Variable a. Eegulus y Double Star 49 7
R
,
.
.
39 39
2184 Nebula 2194 „ 2203 2207 „ 54 Double Star 2279 Nebula 2301 „ 2352 „ 2373 „ 2377 „ Double Star
40 40 40 40 40 40 40 41 41
41 41 41 41 41 41
.
T
1!
88 90 93
g Multiple Star
Leo minor, The
Little Lion.
(Sheet III., IV.)
....38 ....39 ...-40
1713 Nebula
R
37
Variable
2104 Nebula 2178 „ 2271 „ 2287-
.
.
.
.
•
•
39
40
„
Libra,
The Balance.
(Sheet X., XI.)
a Double Star Multiple Star I Variable 1 Triple Star B Variable .
2 1962 Double Star
Lupus, The Wolf. (Sheet X., XT.)
48 48
48 48 49 49
(Sheet IV., v., VI.)
a Vega and 5 Double Stars I Double Star .
.
6
.
g Variable 4447 Ring Nebula XVI.) .
Multiple Star Variable 17 Double Star
R „
.
.
.
.
.
.59 .59 .69 .60
... ... ....61 ....61 (Shrct
60
60
60
.
.
61
4485 Star Cluster S Double Star .
.
.
.61
Monoceros, The Unicorn. (Sheet VIIT., IX.)
—
VII
— Page
Page
816 Double Star 1310 Star Cluster
29 29
i;
Variable
a.
29
.
1361 Star
Cluster
XV.) S 855 Double
29 29 30
Star
1376 Star Cluster
307 Nebula
E
(Sheet
Variable
372 Nebula a Double Star
(Sheet XII.)
(Sheet II., VI., XII.) 11
30 67 67 68 68 68 69 69 69 70 70 70 70 70
3
^0 33 Triple Star 37 Double Star ).
481 5 Nebula I Double Star
Variable
S
„
.
.
5023 Star Cluster
71
Sagitta,
The Arrow
(Sheet v., VI., XII.)
Double Star
I
61
62 62 63 63 64
^ Triple Star 4520 Star Cluster 13 Double Star S Triple Star .
.
.
4572 Nebula
The Archer. XL, XII.)
Sagittarius, (Sheet
X
Variable
.
.
III., v.,
I., II.,
385 Nebula 422 „ 612 Star Cluster
.
XVII.)
§
Variable
IS
„
16 16 17 17 18 18 18 18 18 19 19 19 19
.
.
.
.
658 Star Cluster S 369 Double Star i? Variable
717 Star Cluster
Double Star 775 Star Cluster f Quintuple Star Double Star £ 809 Star Cluster
20 20 20 20
^ Triple Star 820 Star Cluster 831 i: 533 Double Star
Pisces, (Sheet
jA
(Sheet
„ 584 Star Cluster. n Double Star
21 21 21 21
The Fish.
II., VI.,
VII
XII.)
35 Double Star
11
51 65 65
11
66 ^^>
77
.,
.
.
...
XVII
521
.56
(Sheet XV.) 4355 Nebula 4359 Star Cluster 4361 „ 4367 ,, 7F Variable 4376 Star Cluster 4388 „ .
Perseus. (Sheet
The
Southern Fish
y Double Star 1383 Star Cluster 1 Double Star 4070 „
(3
15
austrinus,
Piscis
Pegasus.
"
14 14 14 14 15
Double Star
<p
12 13 13 13 14 14
Quintuple Star
.
.
.
.
.
.
.
56 56 56 56 57 57 57
.57
57 4397 Star Cluster 58 4401 „ 4403 Nebula (Sheet XVI.) 58 58 4406 Star Cluster .68 21 Double Star .
.
.
.
.
58
Z7 Variable
Star Cluster
4424 „ 4442 Nebula 54 Double Star 4510 Nebula 4543 „ Scorpio,
.
....58
.
M 25
.
.
.
.
,.
....63 .
.
.
.
61
The Scorpion.
(Sheet X., XI.) 1 Triple Star
.59 .60 .61
viir 1157 Nebula 1191
(Sheet XVI.) ^25 .
.
1199 Star Cluster
.
.27 .'
27
Triangulum, The Triangle. (Sheet
II., VI.,
352 Nebula f Double Star 6
„
.
XII.) .
.14 .16
... .
.
16
Ursa major, The Great Bear. (Sheet
I.,
II.,
III., IV.,
v., XII.)
1711
Nebula
.
—
INTEODUCTION, rriHE -*-
starry heaven seems to an observer to be a hollow sphere of
The
the other below the horizon.
make with upon the
it
stars
seem
a daily revolution around the earth.
celestial vault, certain
imaginary lines
To ai-e
fix
of the earth,
As
fi.Ked
above and
lies
and
use of. The principal lines employed and meridians of longitude upon the sphere
and give the Right Ascension (longitude) and Declination
heavenly
(latitude) of all
the meridians of longitude are reckoned eastwards round the earth from a conventionally
meridian (Greenwich), and divide the circumference of the earth into 360°, so the celestial similarly divided by the meridians of Eight Ascension,
sphere
is
Aries,
and reckoned
in
an eastward direction, divide the
which
celestial
start
from the
equator into 360°.
first
point of
Further, as
places on the earth north or south of the terrestrial equator are reckoned by degrees of latitude to
to
the position of any of the heavenly bodies
made
for this purpose correspond with the parallels of latitude
bodies.
which one-half
to be attached to this hollow sphere,
90° towards either pole, so the Declination of heavenly bodies
is
up
reckoned in degrees north or
which have south of the celestial equator to the northern or southern celestial poles, each 90° of Declination. Thus, just as one is enabled to determine the position of a spot
upon the earth by its latitude and longitude, so one can heavenly body by its Right Ascension and Declination.
The term Right Ascension the addition of the
+
sign
is
is
further
find on the celestial sphere the place of a
expressed shortly by R.A., and Declination by D, which by
meant
to designate northerly Declination,
and by the sign
—
southerly Declination.
The time
required for a complete revolution of the celestial sphere
This day begins at the instant in which the
first
is
called a Sidereal day,
point of Aries passes the meridian of the place of
—
The sidereal day is divided into 24 hours. (Numbered 1, 2, 3, to 24), each hour into 60 minutes, each minute into 60 seconds. The sidereal day is 3™ 5o'9^ shorter than the mean solar day, and, therefore, the first observation.
point of Aries, or any fixed star, passes the meridian daily about four minutes earlier than
day previously.
mean is
The beginning
of the sidereal day
is
not, therefore, fixed to
time, but during the year runs through all the hours of the civil day.
about four minutes shorter than the
mean solar
As
it
definite
did the
hour of
the sidereal day
day, so the hours and minutes of the sidereal day
are shorter than the corresponding periods of the civil day, as this table shows
Hours.
any
— If on any day the
first
2
—
point of Aries, uf which the H. A.
observer at noon, an hour after noon a point of the heaven of R.A. after
two hours a point of R.A. 30°,
star, or its distance
indicated
from the
first
is 0°,
passes the meridian of an
15° will he on the meridian,
after three hours a point of 45°, etc.
The Right Ascension
by the number of hours, minutes, and seconds, which have elapsed from the time
nation of the
of a
point of Aries, instead of being expressed in degrees, can thus be of culmi-
Thus Vega by 277° 30' we may say that 18 SO"- For, as 360° pass the meridian in 24 hours, in one hour 15° will time minute 15 minutes of arc, and in 1 time second, 15 arc seconds. Thus 277° point of Aries until the time this star passes the meridian, or culminates.
first
instead of expressing the Right Ascension 01 the bright star it
amounts
pass,
and
to
in 1
30' turned into time are equal to 18*" 30"-
In
many
star
maps Right Ascension
of astronomers, however, without exception,
is
is to
expressed in degrees of an arc only.
reckon the R.A. in time only.
The
practice
'Therefore in the
present atlas the [arallels for Right Ascension are given in hours and parts of an hour.
In case
it is
required to turn time into arc measurement, the following table will readily
serve the purpose.
Table for Turning Sidereal Time into Degrees.
Hours.
â&#x20AC;&#x201D;
3
Table for Turning Degrees into Sidereal Time. Degrees.
other words
it is equal to the E. A. of the point of the celestial sphere then passing the meridian. Conversely the Right Ascension of a fixed star expressed in hours and parts of an hour is equal to the sidereal time of its passage through the meridian.
In most cases the observer requires which he
is at
This can
the
easily
moment when be
a certain
ascertained
with
to find out the
mean
or civil time of the place in
star,
whoso Right Ascension
the
help
of
the
is
following
given,
on the Meridian. which gives the
is
table,
apprommcde sidereal time of mean noon
for every day in the year. If the exact sidereal time be required, the Nautical Almanack for the year must be consulted.
Sidereal
Time
at the
moment
of
Mean Noon.
^ h
5 6
7 8 9
18 45 20 47 22 38 18 49 20 51 22 42 18 53 20 55 22 46
40 44 48
2 38 2 42 2 46
4 41
18 57 19 1
52 56
4 52 4 56
1
2 50 2 54 2 58
4 8 1 12 1 16
20 59 22 50 3 22 54 21 21 7 22 58
19 9 21 11 19 13 21 15 19 17 21 19
23 23 23
1
1
5
1
9
21 23 23 13 21 27 23 17 21 31 23 21
10 11 12
19 21 19 25 19 29
13 14 15
19 33 21 35 23 25 19 36 21 39 23 29 19 40 21 43 23 33
IG 17 18
19 44 19 48 19 52
19 20 21
19 56 21 58 23 49 20 22 2 23 53 20 4 22 6 23 57
1
22 23 24
20 8 22 10 20 12 22 14 20 16 22 18
1
25 26 27
28 29 30
20 20 20 20
31
6 39 6 43 6 47
8 45 8 49
6 51
8 53
5
6 55 6 59
3 2 3 6 3 10
4 5 5 8 5 12 5 16
10 43 10 47 10 61
12 42 12 45 12 49
8 57 9 1
10 65 10 59 11 3
12 53 12 57 13 1
7 2 7 6 7 10
9 5 9 9 9 13
11 7 11 11 11 15
13 5 13 9 13 13
5 20
7 14 7 18
5 24
7 22
9 17 9 20 9 24
11 19 11 23 11 27
13 17 13 21 13 25
7 26 7 30 7 34
9 28 9 32 9 36
11 31
13 29 13 33 13 37
7 38
9 40 9 44 9 48
11
11 46 11 60
13 46 13 49
9 52 9 56
10
11 64 11 58 12 2
13 62 13 56 14
10 4 10 8 10 12
12 6 12 10 12 14
4 44 4 48
1
19
1
23
3 14 3 18 3 22
27 31 1 35
3 26 3 30 3 34
5 28 5 32
39 43 47
3 37 3 41 3 45
5 40 5 44
51 55 1 59
3 49 3 53 3 57
5 52
2 3 2 7 2 11
4
1
6
5 8
4 4
5
6
9
6 11
8
20 20 22 22 20 24 22 26 20 28 22 30
12 16 20
2 15 2 19 2 23
4 13 4 17 4 21
6 15 6 19 6 23
8 13 8 17 8 21
32 22 34 36 40
24 28 32 36
2 26 2 30 2 34
4 25 4 29 4 33 4 37
6 27 6 31 6 35
8 8 8 8
43
21 47 23 37 21 51 23 41 21 54 23 45
1
1
1
1
5 36
5 48
7 42 7 46
50 54 58
5 55 5 69
3 7
2 6
9
25 29 33 37
8 41
11 35 11 38
42 13 41
10 16 10 20
12 18 12 22 10 24 12 26 10 27 10 31 10 35 10 39
12 30 12 34 12 38
For
instance, if
be required to find out at what hour of the day on the 15th April,
it
the Star Castor, whose Right Ascension
is
7^ 27",
Sidereal time of Meridian passage
=
mean noon on 15th
Sidereal time at
on the Meridian
is
Right Ascension April
.
.
.
.
= =
I''
27™ 35™
5"^
52™
7''
Difference:
must be borne in mind that the difference is expressed in sidereal hours, 24 of which 3™ 55.9^ shorter than 24^ of mean time. It follows, therefore, that 5'' 52™ sidereal time are 57', or speaking roughly, 1™ shorter than the corresponding mean time, and this must be subtracted from the result given above. Castor will therefore be on the It
are
Meridian at 6^ 51™-
Names
Constellations and the Already in the configurations,
In
constellations.
with regard even
introduced
the
to
the
in
earliest
last
16th
the
chief fixed
natural
when
century,
had received names, and many
stars
mythical
or
more
were
objects,
grouped
had
information
exact
been
several
new
were
constellations
That there was whose names they bore, maps.
no
added
to
resemblance
great
;
number,
the
into
obtained
southern heavens, constellations were duly marked out there also century
astronomical
into
ages the
representing
fancifully
of Stars.
nay,
and
between the
constellations and the objects it is needless to say. The practice which obtained in the old star-atlases, of surrounding the stars composing a constellation with an outline of the person or object which the constellation was supposed to represent,
was, therefore, purely fanciful. only It
with
was
regard
to
The
the
however,
finallj',
which are
to
Until quite
boundaries,
decided
but
that
be found in Argelander's
recently
even
only
JVeiie
the
as
greatest uncertainty
the
to
those
number
constellations
the
should
prevailed,
not
constellations.
be
recognised
Uranometrie.
present atlas will therefore be found to contain only those constellations which
are given by Argelander, the fantastic figures suggested by their
The
of
following
is
a
list
names being omitted.
of the constellations visible from our hemisphere, which are to be
found in Argelander's Uranometrie.
Andromeda, Andromeda.
Cetus,
Aquarius, The Water-carrier.
Cohimba, The Dove.
The Eagle. Argo navis, The Ship Argo. Aries, The Ram. Auriga, The Waggoner.
Coma
Aquila,
Bootes, Bootes.
The Giraffe. The Crab. Canes vcnatici, The Hounds.
Camelojjardnlis,
Cancer,
Canis major.
Canis minor. Capricornus,
The Great Dog. The Little Dog. The Goat.
Cassiopeia, Cassiopeia.
Centaurus,
The Centaur.
Cepheus, Cepheus.
The Whale. Berenices,
The Hair
of Berenice.
Corona horcaUs, The Northern Crown.
The Crow. The Cup. Cygnus, The Swan. Belphinas, The Dolphin. Draco, The Dragon. Eqimleus, The Foal. Eridanus, The River Eridanus. Gemini, The Twins. Cormis, Crater,
Heicules, Hercules.
Hgdra, The Hydra. Lacerta,
Leo,
The
The
Lizard.
Lion.
Leo minor, The
The Arrow. The Archer. Scorpio, The Scorpion. Scutum Sobieslii, The Shield of Serpens, The Serpent. Sextans, The Sextant. Taurus, The Bull. Triangulum, The Triangle. fT/'sfl major. The Great Bear. J7}-sa minor. The Little Bear. Virgo, The Virgin. VuJpecula, The Little Fox.
Little Lion.
Sagitta,
The Hare. Libra, The Balance. Lupus, The Wolf. Lynx, The Lynx. Lyra, The Lyre. Monoccros, The Unicorn. Lepwi,
Sagittarius,
Ophiuchus, Ophiuchus. Orion, Orion.
Pegasus, Pegasus. Perseus, Perseus.
The
Pisces,
Fish.
Piscis ausirinus,
The
The Southern
stars of the greatest
guished by individual is
called Sirius
At
on.
by
the
;
Thus
Sirius
generally
is
use
Flamsteed's
Thus,
however,
day,
by the
stars
their
which
Eistoria
the
Waggoner
individual stars in
are
visible
naked
the
to
which
is
called Capella,
Dog
and so
each constellation are indicated
accordance with a system introduced by Bayer.
in
/3
numbers assigned to them in Right Ascension and Declination.
CceJestis
distin.
the star of the greatest magnitude in the Great
described as a in the Great Dog, Pigcl as
indicated
for
magnitude in each constellation were in former times
Greek or Latin alphabet
positions are given by
in
Fish.
the star of the greatest magnitude in the
present
letters of the
names.
Sobieski.
appeared
in
eye,
is
1725.
The
in Orion.
lesser
stars
are
which their The catalogue most generally
a
that
The
mnjority of the stars in the present work are those of Flamsteed.
catalogue,
of
second
the
figures
At
in
edition
affixed
to
of
the
the same time, there
are many stars faintly visible to the naked eye which have not been catalogued by either These stars are to be found in other catalogues, but they are not Bayer or Flamsteed. specially numbered in this atlas, except where they occur in Struve's catalogue of Double In the case of these stars, the number assigned to each in Struve's catalogue stars.
has been inserted, the letter
2
being prefixed.
Magnitudes of the Stars. The
stars
are divided into various classes of magnitude according to
their
apparent
thus the most brilliant stars are said to be of the first magnitude the least brilliant of those that can be discerned by the naked eye on a clear night are said to be of the sixth magnitude. The arrangement of all the stars visible to the naked eye into these six magnitudes brilliancy
;
;
principally based on the estimates formed
by Argelander, Heis, Behrmann, Gould, and Houzeau. by the aid of photometrical apparatus have proved that the estimate of magnitudes by Argelander's method is fairly trustworthy, and that in general, for the stars visible to the naked eye, each succeeding magnitude after the first
is
Light
measurements
recently
carried
out
indicates the possession of two-fifths of the light of the preceding one.
By
the aid of the telescope, and
magnitude become
visible.
According to
according to
test
its
optical powers, stars of
still
lower
experiments, a telescope with an objective glass of
an inch aperture will show stars of the 7th magnitude. An objective of 1 in., stars of the 9th magnitude; one of 2 in., stars of lOi magnitude; one of 3 in., stars of the 11th magnitude; one of 4 in., stars of ll^ magnitude of 5 in., those of the 12th magnitude of 6 in., those of 12J J
;
magnitude, &c., &c.
;
It
is to
be remarked, however, that the estimation of the magnitude of faint stars
Thus Struve designates the
very uncertain.
faintest
companions of double
stars
which according
see through the 1'2-inch refracting telescope of Dorpat as of the 12th magnitude, to
is
which he could
Argelander's scale would be of the 14th magnitude, and judged by John Herschel would be
classified
observers
These discrepancies among observers arc not very
with stars of the 20tli magnitude.
perceptible in regard to stars
who
up
to the
10th magnitude, and they
may
therefore
be disregarded by
emjjloy telescopes of only moderate power.
Number
of the Fixed Stars.
The most cursory survey of the heavens shows that, generally, the fainter the more numerous they appear. From Argelander's observations it appears that in
stars are, the
the celestial sphere north of the equator there are Stars 1
Magnitude
to 6.5
„
6.6 „ 7.0
„
„
7.1 „ 7.5
„
= =
4120 3887 == 6054
Stars 9.1 to 9.5
Stars 7.6 to 8.0
Magnitude
„
8.1
„
8.5
„
„
8.6
„
9.0
„
Magnitude
= 213973.
= 11168 = 22898 = 52852
Beyond the 9.5 magnitude the stars increase in number so much that it is no Isinger them individually or to number them. The desire and the need to place upon our star maps the faintest stars, has in the meantime led to the employment of photography for the purpose, and as a result we are now able to map out the celestial spaces and to give therein
possible to observe
stars
which approach and even exceed the
The
first
experiments
visibility in
in this line
Paris Observatory by the brothers Henri. expressly constructed for this purpose,
which
stars
to
attended by successful results
With
were carried out
they were able to photograph several star clusters, in
These results 340 millimetres aperture and 3 to 4 metres a large ordinary telescope which served during the time of exposure
of a larger instrument of
This was applied to
keep one and the same point of the heavens continually in the
The
field.
expectation, for stars up to the 16th magnitude were successfully photographed so faint that
might
at the
the aid of an object glass of 6 in. aperture,
even of the 12th and 13th magnitude became visible upon the plate.
led to the construction focus.
our greatest telescopes.
it
was impossible
to see
them by
say, in the proper sense of the word,
the eye through the
was an astronomy of the
same
surpassed
result
—
stars
telescope.
invisible,
and
it
all
which were Here, one
must have
been with a peculiar joy that the observers saw upon the photographic plate pictures of stars In order to photowhich since the beginning of things had never been revealed to human eye.
graph such
faint stars long
exposure was necessary, namely one hour and
twenty minutes,
while
magnitude gave forth their image in the 200th part of a second. [The limit of this method is the limit of exposure. If a point in the heavens could be kept an unlimited length of time upon a definite point of the photographic plate, any source of light there will reveal itself. stars of the first
Mr. Eobcrts has adopted, with some
success, exposure to the
same region on successive
nights.]
Variable Stars. Certain fixed stars exhibit a periodical change in their brightness which in some cases occurs with great regularity, but in the majority of instances first
star
discovery of this variability was in the
Whale.
made by David Fabricius
was
first
irregularly.
in the case
The of the
This star appeared on the 13th August of that year to be of the 3rd
magnitude, whilst in the October following variability
more or less 1596
in the year
it
was no longer
visible.
That
this
was a case of
recognised by Ilolwarda in the year 1636, and the star received, therefore, the
—
8
—
name Mira,
the wonderful. Since this time numerous variable stars have been discovered, the drawn up by C. Pickering, embracing somewhere about 200. According to the kind and manner of variability these stars have been divided into five classes. 1. The so-called new stars {Nome) which burst out suddenly and vanish away slowly. latest
list,
Stars of great variability within the space of several months.
2.
maximum
several magnitudes, being often visible in
to the
naked
These
stars
vary by
minimum they
eye, whilst in
are frequently not within the scope of powerful telescopes. 3. Stars of slight
and irreguLir variability which have no recognisable fixed period. whose periods are of a few weeks only.
4.
Stars of fairly regular variability
5.
Stars whose variability
the
is
confined to a few hours, and which
shine
during long
These are called variables of the Algol type, Algol having been
periods with a constant light.
discovered of the class.
first
In the
and upon the
lists
star
maps the
variables are distinguished by the letter
R>
provided they had not already been indicated by Greek letters before they were found to be variable.
In reference to the causes which bring about lu
the
case
of a dark
[An
star
of
any
star
Algol type
of the
phmet between the
and
star
orbital notion of Algol has
one
us, in other
this variability there is great obscurity.*
led
is
words
to
think of the
periodical
passage
to regard it as a partial eclipse of
the been determined (Vogel, Astron. Nach. No. 2947, and report of
Astronomer Royal, Greenwich, May, ly90), and Professor Vogel has given provisional data for the system made up by it and its dark companion.] Where the periods of variability are long and irregular the causes are very obscure.
away
fading
of
any one of these seem
As
to the
to indicate
new
some
sudden outbursts and slow
stars (None), the
kind of great catastrophe, probably a collision
with another cosmical mass.
Distances of the Fixed Stars. The
distances of the fixed stars from our earth are without exception so considerable
that up to the present
this it appears
and one must
miles away,
can be
has been possible only in a few instances
it
From
parallax.
their
seen
a substantial value for
to obtain
that even the nearest fixed star
is
still
four billions of
conclude, on the ground of analogy, that the faintest stars which
by the improved telescopes of to-day are many hundreds, or even thousands of
billions of miles distant.f
Double Stars. If one survey the heaven with a telescope one meets frequently twin stars which
near
to
lie
so
each other that they can be separated only by a glass of a very high power. These are called
In the Bakei-ian Lecture delivered at the Royal Society, April 13th, 1888, b}' J. Norman Lockyer, F.R.S., and afterwards published in Nature, a new theory is advanced to account for variability. Mr, Lockyer considera that " new stars " are produced by the collision of meteor swarms, and that the more or less regular variables are owing to the periastron passage of one swarm through another (see Natun; May 24, 1888, p. 79). In this Lecture Mr. Lockyer endeavours to show that the heavenly bodies are all formed from meteoric dust, and that the differences between them are simjily owing to the different degrees of condensation of the dust, and the consequently greater or fewer number of collisions of the particles the slight condensation and comparatively few collisions giving rise to the weak light of the fainter nebulre, while the closely condensed swarms show, through =^'
;
all their stages,
bright nebulee, nebular stars, and real suns.
Editoii.
In the Thirteenth Annual Report of tlio Savilian Professcn' of Astronomy, road June (Ith, 18SH, Dr. Pritcliard j^ives a verj' interesting account of his later operations for stellar parallax, by photographing small portions of the lieavens. He is satistied, not only with the convenience of this method, but also with its unimpeachable accuracy. The following are the results obtained so far •f
:
61'
61^ /i
Cygni Cygni
.
.
0--128'J
.
.
0-4353 ±0-0152
Cassioiieia)
Polaris
±0-0180
.
.
.... .
.
0-0356
±00250
0-052
±0-0314
«Cassiopeia3
^
Cassioiieia3
yCassiopeia3
.
.
.
.
.
.
0072+0-042* 0-187 +0-039*'
<
0-05
±0-047*
Later reports of Professor Pritcliard give us the parallax of |S Andromeda) as 0'092. aArietis as 0-08. 0-115. e Cygni, a Persoi, 0-074. a Cephei, 0-061, but see tlio Seventeenth Annual Eeport of the Savilian Professor of Astronomy (Prof. Pritcbard) for a complete liistory up to date (1892) of all [Edit.] effective researches in stellar parallax.
Double
The
Stars.
brightest of the pair
primary
is
The
distance
The
is
meant merely the apparent space which
iippearance of nearness
is
often
owing
to the
are,
however, numerous instances in which there
position angle varies in such a centre.*
manner
two
separates the
stars
is
may
many
In these cases the
as to indicate a motion of revolution round a
double or multiple stars
W.
common
Ilerschel and F.
connection
physical
a
possess
its
be immensely great.
a real propinquity.
Recent observations, especially those made since the time of
Struve, have proved that
companion from
being in almost the same line
from each other
in regard to the spectator, while their real distance
There
"companion."
its
place of the companion in relation to the
expressed by distance and angular position.
By primary.
"primary," the other
called the
is
Frequently, however, both stars are equally bright.
W.
with
each other.
The
position angle
is
the angle which a lino
forms with the latter's circle of Declination. east to south
is
to its
primary
calculated from north through
and west.
The number time.
drawn from the companion
The, position angle
There are
of
Double Stars
is
quadruple and quintuple
also triple,
The primary and companion
known number is not
about 7,000 being
considerable,
stars,
but their
are not infrequently of different colours
yellow and blue, and green and blue stars being found together. these colours are only faintly visible, and
it
requires a certain
Except
amount
in a
at the present large.
white and blue,
;
few
cases,
however,
of practice and a powerful
telescope to be able to distinguish them.
Star Clusters. Groups of clusters.
Some few
stars collected
more or
for instance, the Pleiades in
Taurus and a cluster
seen through the telescope only.
together in a small space are called star-
less closely
star-clusters can be distinguished, in
though imperfectly, with the naked eye,
Indeed many of them appear misty and nebulous oven in
telescopes of ordinary size, a powerful instrument being required to resolve them. clusters
seem
as,
Cancer, but generally thej' can be clearly
with a strong condensation towards the centre.
to be globular in shape,
Most
star-
Frequently
the stars in the centre of a cluster are crowded so closely together that they seem a nebulous mass,
around which the external stars are
The
collected.
relative positions of the various stars in these star-clusters
exact measurement in a few cases only;
have been decided by
but the recent strides that have been Tnade in the
application of photography to astronomical observations lead us to hope that
able to obtain records of their most minute details.
graphs taken at intervals of
We
shall
sufficient time, arrive at valuable information
motions of the component stars of these
we
shall ere
long bo
thus by the comparison of photo-
with regard
to
the relative
clusters,
Nebulae. Nebulae are among the most remarkable objects to be found in space, but the majority of them cannot be studied in detail except by the aid of the most powerful telescopes. At the present day upwards of G,000 NebulaB are known to astronomers. John Herschel prepared a general catalogue containing 5,079 NebuUe and Star-clusters.
For the sake of brevity the Nebula) are usually distinguished by the numbers assigned to them in Ilerschel's catalogue, and this course has been followed in the present work, where the numbers are accompanied by the letters G. C. (General Catalogue). â&#x20AC;˘
Sou Editorial Nolo,
p. 71,
—
—
10
"Whilst most Nebultc cannot be clearly observed except with a powerful telescope, there
may
are several hundreds, however, which if
some round
some
or elliptical,
be studied on a clear night with an ordinary glass,
Viewed
the weakest power bo employed.
in detail,
it
will
be seen that their shapes are various
;
spindle-shaped, some like planetary disks {Phtnetary Nehulee), others
ring shaped {Annular Nehulce), others spiral [Spiral Nehulce), while
many
are
quite irregular in
outline.
The Spectroscope shows us the germs of future worlds, or
it
are masses
that the Ncbulcc
hydrogen and nitrogen play an important part.
may
of incandescent gas*
Possibly in these glowing masses
in
we have
which before
be in some cases the disintegrated remains of former solar
systems.
Explanation of the Maps. The general maps central Europe,
in this atlas include that portion of the heavens
and they cover as
far as
SS"-"
The
South Declination.
which
is
stars are divided
visible
of conventional signs into six classes of magnitude according to their apparent brilliancy.
system of numbering adopted
is,
as a general rule, that of Bayer,
Such variable
the Greek and Latin alphabets. is
A
by means of the small
stars as are not given
in
by a system
The
letters of
by Bayer, are marked, as word Yar being added.
usual, by the capital letters of the Latin alphabet, beginning with R, the
number
interesting variable stars,
of especially
catalogued by Struve as Double Stars,
which
at their
maximum
do not attain to
These stars are distinguished by a small
the sixth magnitude, are also given. if
they have not been noted by Bayer, bear the
possess in Struve's catalogue with the letter
i)
prefixed
;
all
circle.
Stars
number they
other numbers attached to stars are
those of Flamsteed's catalogue. Star clusters and Nebulro are distinguished by small circular groups of dots, and the
accompanying number
boundary
is
that assigned to each
lines of the various constellations are
Ilerschel's General Catalogue.
in
Lastly, the
taken from Argelander.
Description Of the more interesting Fixed Stars, Star Clusters, and Nebulae contained in the Maps of this Atlas.
The
following
list,
in
which the various
Ascension, gives a fairly complete account of what object
upon the Maps, f
To
find
in this list
stars, etc., are
is scientifically
any
arranged in order of Right
known
at the present time of each
star or nebula contained in the
only necessary to take the approximate Right Ascension of the object from the
Map
Maps,
and
it is
also its
number or letter. These will indicate, without trouble, the object in the descriptive Catalogue. The Right Ascension and Declination here given are those for the year 1880, North Declination is shown by the sign +, South Declination by the sign The Nautical Almanack furnishes the annual variation in Right Ascension of the
—
principal stars,
'1-
But
and from
see
Note
this the
p.
Right Ascension
H.— [Edit.]
f
for
The Editor
any year can be readily calculated.
lias
eiKleavourcd to bring this up to 1S02
11
Kight Ascension
Declination 1880.
18»0.
Oh
3m
+
58° 29'
/3
This
Cassiopeise.
Burnham, who observed
panion of 11 mag.
primary than
stars nearer to the
ym 4- 14° 31'
with the 18-inch
this star
Chicago, states that he saw more than a dozen very faint
refractor at
Qh
2.5 mag., has at 5' distance a faint com-
star,
companion.
{Sec iwfe p. 8.)
11 and 11.5 mag.
2.5 mag., with two faint companions,
7 Pegasi.
The primary
respectively.
this
is
red in colour, and probably to a slight extent
variable. 0''
9"
+
8°
9'
A
35, Piscium.
11.5" distance.
at
double
primary 6 mag., companion
star,
Position angle,
150°.
No
7.8. mag.,
change in the position of
the companion has been observed. 0"
17'
+
55°
T
8'
at 0''
18™
+
R
red- coloured
It varies
The
minimum.
37° 55'
A
Cassiopeiae.
Kriiger in 1870.
variable
by 11
period of variation
A
Andromedae.
star,
is
it is
invisible,
Its
18"
— 10°
0'
S
Ceti.
about 430 days.
According to Schocnfeld
magnitude at
maximum
even with a most powerful telescope.
but variable: improbably identified. Qh
be
to
variable star with a period of about 405 day.^,
noted as such by Argelander in 1858. a rich orange colour.
found
from about G.5 mag. at maximum, to
is
5.5,
and
at
it
is
minimum
[Spectrum, bright lines
Greenwich, Obsermtori/, 1889.]
This star was found to be variable by Borelly in 1872.
vaiies from 7 mag. to 11 mag.
Its
of
supposed period of 324 days
is
It
very
uncertain. 0"
19"
+
63° 24'
Place of the 11 Nov., 1572, list
of
till
New
the stars in
all
Star in Cassiopeia, which Tycho observed from
March, 1574, the
as a star of 1
mag.
D'Arrest has made a
neighbourhood of Nova, with the aid of the
and states that any star not yet set down which may appear within a radius of 10' from the place of Nova, may be considered as either new or variable. D'Arrest's Chart will be found at Sheet xvi. of this Atlas. The most brilliant star in this Chart large refractor at Copenhagen, in his Chart,
is
C
23™
+
59° 10'
8.9 mag., the faintest 16
mag.
63, Star Cluster in Cassiopeia. The stars composing this cluster, which was discovered by W. Herschel 16 Dec, 1788, are coarsely scattered.
The cluster is nearly round in shape, and is from 15' to 20' in diameter. Near the centre may be seen a star of 8.5 mag., and one or two others of 9 mag. the rest are fainter, some of them being scarcely visible. ;
C
25"
+
60° 51'
68, Star Cluster in Cassiopeia,
very minute
by him
stars.
about
1' in
diameter, and rich in
Discovered by Herschel 26 Nov., 1788, and described
as but little
densely massed
is
removed from a resolvable nebula.
together
towards
the centre of this
The
cluster,
stars are
which
is
globular in shape. 0" 20"
+
6°
18'
51, Piscium, 5 mag., has a
change has been
companion of 9 mag.
observed in the position of this
accurate measurement.
at 27" distance.
No
latter since the first
— Kight Ascension
Declination 1880.
1880.
0'"
O'-
84"
34"'|
+
20° 47'
4- 55°
colour.
The companion
colour.
Two
53'
a.
40° 35'
at
distance
G.3'
very beautiful
is
5 mag., and yellow in
is
8 mag. and of a deep blue
stars.
Cassiopeise, a reddish-coloured star, 2.2 mag., found to be slightly
by Birt and John Herschel
at 60" distance.
+
The primary
55, Piscium, a double star.
variable
0"
—
12
companion 9 mag.
{See note p. 8.)
The Great Nebula
116,
It has a
in 1831.
in
Andromeda. In
fine weather, if there
moonlight, this nebula can be clearly seen with an opera-glass.
be no It
is
mentioned as early as the 10th century by the Persian astronomer Sufi. In the "West it seems to have been first noticed by Simon Marius, 15 Dec,
On examining
1612.
it
with the naked eye
it
appeared to him
to
be
merely a small cloud, and on applying the telescope he could discover no evidence that
it
was
of a stellar nature
;
it
seemed nothing more than a
patch of whitish light of greater brilliancy at the centre and fainter at the
Marius compared it to a light seen from a great distance through some semi-transparent medium. Ilalley described the nebula as triangular, but Messier contends that it is formed in the shape of two luminous pyramids iippHcd on opposite sides of a common base, the diagonal passing from apex to apex pointing from N.W. to S.E. The distance between the edges.
apices
is
two-thirds of a degree, and the length of the
quarter of a degree. increase
Jlessier
saw no
of brilliancy towards the
examined the nebula through
common
Later on F.
centre.
base one
but noticed an
star in the nebula,
W.
Herschel
Tlie luminous central
his great telescope.
portion he, too, found to be of a nebulous character, but with indications of its
being resolvable into separate
stars.
The middle,
or the so-called nucleus
of the nebula, has not a starry appearance, but viewed through a very powerful telescope it its stellar
has a certain flaky look which confirms llerschel's opinion of
character.
Finally, an examination
made
in 1848,
with the aid of
the great Refractor at Cambridge, (U.S.A.), proved the existence of
upwards
of 1,500 minute stars within the nebula, while the nebulous character of the still apparent. Two thin, dark parallel streaks, somewhat like two cracks, were found to run through the mass of stars, and have since been noticed by other observers. In the spectroscope this nebula gives clearly a continuous spectrum, thus proving that it is not a mass of incan-
whole was
descent gas, but rather a highly condensed star-cluster, at least in the central parts.
With a powerful glass down over the nebula, one
several faint stars of
of August, 1885, a star of 6.5
them being
may be
of 10.5
seen scattered up and
mag.
About the end
mag. suddenly appear(;d near the centre of
the nebula which gave a continuous spectrum containing, probably, a few bright lines.
down
to 8.5
By
it had dwindled 1886 had disappeared entirely,
the middle of the following September
mag., and in the
summer
of
even the great Refractor at Washington failing to discover
was
it.
This new star
not, probably, a condensation of the central portidn of the nebula,
but
seems on the contrary to have had no relation to it. Probably it has always been in the place where it ajipeared, and is one of the countless faint stars observed there
by Bond.
The sudden
increase in brilHancy which
— Eight Ascension
—
13
Declination I
1880.
I88O;
took place towards tho end of August, 1885, was probably not owing to a great eruption of incandescent gas, but rather to other circumstances.
Of the
phenomenon
various possible theories, that which attributes the
the conversion of probable.
cosmic motion into heat
[Roberts' photograph,
and light
the
seems
to
most
taken in December, 1888 (fourliours'
The numer-
exposure), gives clearer details than any previously attained.
ous stellar points in the nebula seem physically connected with it, lying " along the edges of the dark refts, following all their sinuosities." Banyard.
From
Kno)ck'(hje, 1889.
1885 and 1890 0"
SG"
+
40°
13'
it is
a series of photographs taken bylloberts
inferred that the nucleus of the nebula
Companion of the great Nebula
117,
in
between
variable.]
is
Andromeda.
Viewed
through a telescope of low power this has the appearance of a nebulous star. In reality it is a star-cluster, but a very powerful instrument is required to distinguish the separate stars.
Oh
37m
+
Gl°
8'
The Qh
42m
— 25°
in diameter,
57
42m
+
57°
IV
it is
;
and range from 9
long,
narrow and bright, and
Cassiopeiae,
ri
10 mag.
to
Nebula in Cetus was discovered by Caroline Herschel,
138,
1783 Qh
120, Star Cluster in Cassiopeia, discovered by Caroline Ilerschel. somewhat coarsely over a space of from 15' to 20'
stars are scattered
a yellowish
is
star,
preceded by
Sept. 23,
a star of 9 magnitude.
4 mag., with a purple coloured
The Ilerschel, 17 Aug., 1779. 1882 was 5.2"; the position angle 165.7°; the time of revolution round its primary as calculated by Duner is 176 companion of 7.5 mag., discovered by distance of the companion in
years
the parallax, according to Clausen,
:
from the earth of eleven Ql.
43m
is
0.371", indicating a distance
billion miles.
65, Piscium, a double star, discovered
by Herschel in 1783.
are of 6 mag., and their relative position does not seem to vary.
Qh
48m
+
18°
32'
being 6 mag., the companion 7 mag.
^O-"
+
60°
be
0.6".
minute
stars nearer to
the primary, but they can only be seen with a
telescope of the highest power. O**
50™
+
Miidler, in 1843, found the distance
Dembowski, in 1885, could only perceive a single star of elongated form. Burnham, in 1880, calculated the companion's distance to be 0.4". The velocity of revolution of the companion is very high. 7 Cassiopeiae. This star, 3 mag., has a companion of 9.5 mag., at distance 432", position angle 327°. There are nearly a dozen very
to
0''
stars
Recognised as a double star at Pulkowa, the primary
Piscium.
66,
Both
Distance 4.3".
37°
{See note p. 8.)
Andromedae, a double star such by John Herschel. The /x
as
of 4
mag. and 11 mag.,
first
distance of the companion
recognised is
49";
its
position angle 110.5"; only visible with a very powerful telescope. O"-
0-2"
+
U
81° 14' in
Cephei, a variable star of the Algol type, discovered by Ccraski
1880.
The
star is generally 7 mag.,
periods of 2.5 days.
With
11.5 and 13 mag. respectively, 44'
0^
59"
+
20° 50'
may
be seen.
Primary 6 mag., companion 9 mag. distance 16" angle 253°. The position of the companion does not seem to vary. Piscium, a double star, consisting of two white coloured stars of
26, Ceti, a double star. position v]/'
5 mag.
;
but diminishes to 9.5 mag. in
a powerful telescope, two faint companions, of
distance 30".
pocket telescope.
No
They can be
;
easily "divided " with the help of a
change has been observed in their relative positions
during the last 130 years.
—
14 Eight Ascension
Declination 1880.
1880.
Jh
+
0"
4°
16'
77, Piscium, a beautiful double star
6.8 mag.
+
30°
;
No
distance 32.8".
primary 6 mag., companion
;
change has been observed in their position.
47'
Piscium, recognised as a double star at Pulkowa. Primary 5 mag., ff companion 10 mag. distance 2.5". 23° 57' Piscium, 6 mag., with a remarkably faint companion at 7.6" <p ;
+
distance; position
angle 22°.
Piazzi
been as faint then as
+
6°
56'
calls
a
it
double
but
star,
would not have enabled him
quite evident that his telescope
to see it
it
is
had
it
at the present day.
it is
^ Piscium, a beautiful double star, easy to observe, the primary and companion being 5 mag. and 6 mag. respectively. The distance and position angle have not undergone any essential alteration since Struve measured them in 1821, the former being 24", the latter 64°. [Shown
1889, to be a triple star.] 1"
+
11"
S
71° 50'
Cassiopeiae, a variable star of long period, discovered by Argelander
at
At maximum it is 6.7 mag., though minimum it is under 13 mag., or it becomes
is
607.5 days.
in 1861.
1"
+
12-
58°
9'
—
1°
8'
1"
15-"
+
88°
40'
Sept.,
The
stars
42, Ceti, a double star, 6
range from 7 to 10 mag.
There
1787.
and 7 mag.
a Ursae Minoris, the Pole Star.
Hcrschcl, 17 Aug., 1779.
According
result
+
67° 30'
is
4-
very untrustworthy.
to di\dde this latter into
;
18.5",
gives a yellowish light.
It
which was discovered by
to Peters' calculation, its parallax is
40
billions of miles,
but this
{Sec note p. 8.)
Cassiopeiae, a triple star.
and a companion 8.5 mag.,
Discovered
Distance only 1.3".
2 mag.
0.08", indicating a distance from the earth of
17-°
mag. period
a double star in the cluster of
is
has a companion of 9 mag., distance
V
The
[Bright lines spectrum.]
by Ilerschel, 18 8 and 9 mag.
14m
often less than 8
quite invisible.
256, Star Cluster in Cassiopeiae, a large cluster, rich in stars and nearly round in shape.
Ih
it is
saw only the primary 4.4 mag. Struve, in 1831, was the first of 8.9 and 9.5 mag. respectively,
Ilerschel
at distance 30".
two separate
stars
distance 3".
V
+
lO"
8°
55'
307, Nebula in Pisces, a bright and fairly large nebula, with increase of brilliancy towards the centre
1"
+
24"
2°
R
16'
minimum
than l"
+
25-"
60°
2'
jh
25-"
—
27"
+
it loses,
.
it is
as low as
and the period
8 mag., and a double 7° 29'
30°
1851.
in
342,
large
an
it.
and
star,
it is
from 7^ to 8| mag.,
12J mag. it gains more quickly 345 days. ;
in brilliancy
is
This
is
among
not a very large cluster, but others a red-coloured star of
primary 6 mag., companion 10 mag., distance 13.6". faint and rather small, much brighter towards
Discovered by Ilerschel, 10 Sept., 1785.
faint,
in
Triangulum.
Discovered
first
but easy to observe in consequence of
saw the most
seven-foot telescope Herschel
With
near to
Nebula in Cetus,
352, Nebula
4'
stars
At maximum
contains several stars of G to 9 mag.,
the centre. l"
Hind
341, Star Cluster in Cassiopeia. it
4
Piscium, a variable star of yellowish colour with a long period,
discovered by at
;
it
its
by Messier; very extent.
With
a
dimly, and best with a low power.
a ten-foot reflector, brilliant part was resolved into separate and when a still stronger instrument was employed, almost the whole nebula was resolved into stars, which seemed to Herschel nothing more than stars,
— Right Ascension
15
Declination 1880.
1880.
the smallest imaginable points.
Rosse observed in
— 30°
shown by 1'
361,
nebula
P
30°
+
15° 10'
is
372,
it
nodes of
This nebula
light,
and
Discovered by Herschel 9 Dec., 1798.
in Cetus.
This
fairly brilliant, with a brighter nucleus,
and is 6' long by li' broad. Discovered by Mechaia in Sept. 1780, and
Nebula in Pisces. him as a starless nebula
of fairly large dimensions, but very
Messier confirmed
to observe.
difficult
Herschel, on the other hand, describes of being
Lord
arrangement
spiral
his telescope in several similar objects.
Nebula
described by dull
nearly 30' in extent.
is
and the well-known
clearly
gradually at
this view.
Sir
as a globular star cluster,
it
resolved into separate stars, whoso brilliancy
and then suddenly
first,
John
capable increases
Lord Eosse, with the
at the centre.
help of his great telescope, detected a spiral arrangement of the stars.
Yogel
saw-
it
October,
in
with
1867,
the
8-inch
Leipsic, as a faint, globular star cluster, 3' in diameter, the little
1"
3.5°
+ 50^ 59' a
more densely collected towards the centre. 385, Nebula in Perseus, the preceding of two
distance of 2' from one another.
and described consist of
V
mistake.
38°
+
60= 38'
it
as a small, faint, starless nebula.
small stars,
The nebula
intermingled with nebula
it first,
at
5 Sept., 1780,
Messier believed ;
at
stars being a
which stand
nebulaa,
Mechain saw
refractor
it
to
however, was a
this,
is fairly brilliant.
302, Star Cluster in Cassiopeia, a beautiful object, 15' in diameter, rich in stars, ranging from brilliant to faint
minute points a double star, primary 9 mag., companion 10 mag., distance 8", is to be seen in the cluster also a red coloured star 8 mag. in the southern portion. ;
;
Ih
44m
Ih
4(jm
— IP 17' + 35° 34'
X
Ceti, 5 mag., at distance 3' stands a star of
422, Nebula in Perseus.
In
7 mag.
4 Sept., 1784, discovered four separate starry nebula}, three standing in a line, the fourth at right angles to them that at the angle is much the largest. D'Arvest observed this Herschel,
;
these nebula} a
others
second time.
near them,
According to Lord Rosse, there are three Dreyer thinks these to be identical with those
but
observed by Herschel. 1"
47°
+ 18° 42'
primary 4.2 mag., companion 4.4 and described by him as remarkable in the highest degree. It can be divided by the help of a small telescope distance 8", position angle 179°. There is besides, at distance 4', position angle 84°, a faint star, first seen by J. Herschel and South in 1823.
7 Arietis, a beautiful double
mag., observed by
Burnham extremely Jh
50m
+ 37°
5'
Hooke
discovered that difficult.
this
Between
457, Star Cluster in
star,
in 1644,
it
star
is
Andromeda,
l*-
51° 53°
+ 23= + 20° 28'
1'
star,
but
its
division
is
faint star.
numerous
a keen eye without the aid of Herschel first observed it 21 Sept., 1786.
a telescope as a nebulous star.
X Arietis, a double
double,
30' in diameter, containing
brilliant, coarsely scattered stars, visible
P
also
and 7 he saw another very to
primary 5 mag., companion 8 mag., distance
38", can be divided by a good pocket telescope.
2
196, Arietis, a quadruple star, primary 6 mag., companions 9, 10 respectively. The brightest companion is at distance
and 12 mag.
3' 4", position I''
56°
+
2° 11'
angle 0.8°.
2 Piscium, a beautiful double star, primary (which
2.8 mag., companion (which
movement
of the
companion
is is
is
green in colour)
blue in colour) 3.0 mag., distance 3".
very slow.
The
—
16 Bight Ascension
Declination 1880.
1880.
1"
56"
+
32'^
42'
E
This
Trianguli.
6.5 mag.,
star,
an exceedingly faint com-
lias
panion, distance 4", position angle 116.8'^
It requires a very
powerful
instrument to distinguish this companion. 1"
57"
+
41° 45'
7 Adromedae, a gold-coloured
The
Distance 10".
6 mag.
star,
are easily recognised as a double star.
that the companion
and 8.5 mag.
distance
still less
is
very intense, and they
is
In 1842, however, Struve discovered
a double star, consisting of two separate stars
is itself
of 6.7 mag.
3 mag., with a blue companion,
colour of both stars
At
respectively, distance only 0.5".
and a refractor of great power
(0.3"),
present this
is
required to
divide the companion.
3"
2^
+
25° 22'
14, Arietis, a triple star 36.4°,
ar
position
;
the primary 5.6 mag., has at distance 93",
a companion 8.9 mag., and a second at
106"; position angle, 278.5°
Ilerschel
distance
had measured the distance of the
nearer companion in 1783.
Km
Oh
+ 29°
44'
6,
Trianguli, a double
(which
panion
primary (which
5 mag., com-
yellow)
is
6 mag., distance 3.8".
blue)
is
star,
Discovered by Herschel
in 1781.
2^
9"
+ 24° 30'
B Arietis,
a variable orange-coloured star, discovered at
Bonn
in 1857,
and since then frequently observed. The period is 186.2 days. At maximum at minimum 12 mag. and under. When the star is 7.6 to 8.5 mag. ;
approaching
its
maximum
the increase in brilliancy
is
weeks
often for
together very slow. 2''
11"
+
56° 36'
512, 521,
Two
large Star Clusters in Perseus, being one of the most
magnificent objects of
its
kind in the heavens.
The
larger of the two
x
is
30'
in diameter, and consists of a large number of stars ranging in magnitude from Vogel and Lament have measured this cluster with the 6.5 to 13 and 14.
The southern cluster h is smaller, being 15' in diameter and The stars appear condensed towards the centre. Photographs
micrometer. less rich.
have been taken of both Lohse at Potsdam. 2h
13in
3°
81'
by the brothers Henry,
at Paris,
(Mira), a variable star with long period, and the
Ceti variability
clusters
was
12 August,
detected.
D. Fabricius observed
it
early on the
1596, as somewhat brighter than a Arietis.
had disappeared.
Ho saw
Holwarda observed
in
it
it
and Dr.
first whose morning of
In October
again in February and March, 1609;
1638, and recognised
it
then
periodical variability.
its
According to Argelander's calculations the period is 3311 days, but it is very irregular, and the diff'ercncc of period is sometimes as much as 25 days. Its
as
magnitude
at
maximum
also varies greatly,
2 and often not more than
5.
At minimum
being sometimes as it is
much
9 mag., being the same
magnitude as that of a cunipanion at distance 2', position angle 85°. The star is of a deep red colour, and gives an interesting spectrum. [The third line of hydrogen has been detected at Greenwich in the spectrum.] 9h
1
.^m
_|_
410 47»
5i7,
Nebula in Andromeda,
with a dark cleft in the middle.
1783. is
According
to
fairly
John Herschel
seen obliquely by us.
brilliant,
15' long
by
3'
broad,
Discovered by Miss Herschel in August, it is
a vast,
fiat,
nebular ring, which
17 Right Ascension
Declination 1880.
1880.
2"
19"
+ 66^
2''
20"
—
2"
21'"
2''
30"'
2''
30"'
2''
33"
2''
34'"
+
26° 33'
2^
35-"
+
42° 17'
2h
37m
—
0°
2h
37™
+
2° 44'
2"
40""
—
8°
2*"
42-"
+
55° 24'
+
17°
2'
58'
52'
0°
31'
4'
2"
43"'
+
16°
2h
4gm
+
26° 45'
— Ascension
Dcclinatiun i
1880.
1880.
2''
18
52">
+
20° 52'
Arietis (S 333), a double star, primary, 4.5 mag., companion 6 1.5". As conjectured by Struve, the primary probably
f
mag., distance
varies from 4.5
oil
.'"win
+
38° 23'
mag.
the brightness at 2''
58°
+
The
1854, by J. Schmidt.
in
and the companion
maximum
also
seemed
to
him
this theory.
This orange-coloured star was
Persei.
?
to 6.5 mag.,
Engelmann supports
variable.
period
is
first
recognised as variable
seemingly quite irregular, and
varies considerably.
by companion
52, Arietis (S 346), triple, but cannot be clearly divided except
24° 47'
The primary,
a very powerful telescope. at distance
0.7"; the
5.5 mag., has one
outer companion, which
is
very faint (11 mag.),
is at distance 5".
3^
0"
+
40° 30'
/3
Persei (Algol), one of the most interesting variable
variation
was discovered
but Goodricke, in
According
is
was
the
as
recognise
to
first
true
its
nature.
the star remains invariable for 2| days, and hours to 3.7 mag., and during the next 4h hours
to his account,
then decrease? ia it
as far back
1782,
The
stars.
1767 or 1769, by Montanari,
4^-
mag. The period is 2 days 20h. 48m. 53!4s. This not constant, there being a difference of a few seconds in the course of
increases to 2.2
the year. gh
7r
1°
39'
3h
7>
+
which
94, Ceti, 5.5 mag., has a very faint companion at distance 5.7", it
needs an extremely powerful telescope to distinguish.
46° 47'
658, Star Cluster in Perseus.
A
beautiful cluster 8' in diameter,
W.
Discovered by
very rich in stars of 10 mag. and under.
Herschel,
27 Dec, 178G. 3h
7n,l_29o
28'
12, Eridani, a star of 3.5 mag., with a
companion 7.5 mag., distance
2.4", position angle, 316°.
+
65°
13'
52, Camelopardalis.
;>h
Qm
_|_
40O
2
2'
distance, 3.5", 16'"
— 15°
49'
692,
star of 6.5 mag.,
very
with a companion 7 mag.,
diificult object.
Double Star in Perseus.
369,
yellowish- white colour;
3''
A
A
at a distance of only 0.5".
The primary, 7 mag.,
the companion, 8 mag.,
is
is
blueish-white.
of a
The
seems to bo increasing, but very gradually.
Nebula in Eridanus, rather
faint, large, irregularly
round in shape,
A
gradually increasing in brilliancy towards the centre.
star,
7 mag.,
precedes the nebula.
+
2
59° 31'
385, Camelopardalis.
The primary, 5 mag.,
is
yellow in
the companion, 9 mag., distance 2.4", position angle, 161°, 3''
21""
+
55°
2'
3h
21"'
— 21°
46'
colour,
white.
is
2 390, Camelopardalis. Primary 5 mag., greenish-white in colour, with a faint companion 9.5 mag., distance 15", position angle, 160°. 709, Nebula in Eridanus, discovered by
W.
Herschel
elongated, but small, with a nucleus, followed southwards
;
fairly bright,
by a small and
very faint nebula. Sh
22"'
+
35°
H Persei, a variable
15' as
8
mag.,
and
at
Period, 208.5 days.
under
for
star. At maximum it sometimes reaches as much minimum becomes frequently less than 13 mag.
According to Schoenfeld
two months' time
it
remains at 12 mag. and
— Bight
Declination
AsceDsion
1880.
1«80.
S*"
23° +36°
717, Star Cluster in Perseus, large (15' in diameter), contains about
53'
60 3h
24"
19
+58°
Discovered by Ilerschel, 28 Dec, 1799.
stars coarsely scattered.
2
21'
396, Camelopa,rdalis, a star 6.5 mag., with a faint companion,
8
mag., distance 20.3". 3h
27m +24°
3"
31°
4'
Tauri (2 412), 6 mag., with a companion 10 mag., distance 22". The star is thus described by W. Herschcl, South, and John Ilerschel. But Struve, with the Dorpat Refractor, divided the primary into two stars 7,
of almost equal brilliancy, at a distance of only 0.6" from one another.
+
0°
2
12'
422, Eridani, a double star, primary 6.5 mag.,
The primary
distance 6.5". 3h
34m
+
4°
2
45'
position
The primary
angle, 301°.
3^
3S° +33°
The The second at
55°.
angle, is
companion 8 mag.,
yellow, the companion blueish.
Triple 6.5, 9 and 9.5 mag.
430, Tauri.
distance 26",
is
companion
first
is
at
distance 38", position
yellowish.
Persei (2 431) a star 5 mag., with a faint companion 9.5 mag.
35'
distance 20". 3"
38™ +23°
768, Nebula in the Pleiades, discovered by Tempel, 19
20'
An extremely
faint nebula, situated near the
star
Oct., 1859.
The brothers
Merope.
Henry have discovered, by the aid of photography, another very faint nebula which seems to proceed from the star Maia, but this can only be scon with a most powerful telescope. (Of. Sheet xiii.)* 3"
40° +23°
V in the Pleiades,
44'
quadruple and a very beautiful object even as
The primary
seen with a small telescope.
6.5 mag. at distance 118", position angle,
116",
position
angle,
344°.
Lastly there
distance 115" from the companion of ri
3h 40°
+52°
is
also
known by
the
name
775, Star Cluster in
18'
3h
42° +10° 3h 42m +23°
46'
is
30,
41'
2
from
6.5
of Alcyone.
is
has
one companion
a second 7 mag., distance a small
mag.,
star,
position
(See Sheet
9
mag.,
1
to
at
303°;
angle,
xiii.)
Perseus, small, consisting of about 30
ranging in magnitude from 1
whole
3.5 mag.
289°,
13, besides one star of 10
stars.
The
mag,
2' to 3' in diameter.
Tauri (2 452), primary 5 mag., companion 9 mag., distance
453, (Atlas) in the Pleiades, a
star,
4 mag.
9".
In 1827 and 1830
Struve fancied that he could distinguish a companion to
this
star
of
8 mag., distance 0,8". It was, however, never seen afterwards by Struve or any other observer. Even Burnham always found the star to be single and perfectly round, 3h
471
+ 31°
32'
Quintuple. The primary 2.7 mag. has, at distance companion 9.5 mag., at distance 90" another of 10 mag., and a third 10 mag., at distance 122". There is besides a faint star of 12 mag., ^ Persei (2 464).
13", a
distance 33", position angle, 286°. 3h
43m
3°
32,
19'
Eridani
(
2
470), primary 5 mag., yellowish, with a companion
6 mag., distance 6.7", of a blueish colour.
Discovered by
W.
Herschel in
1781.
The fuller traces of nebulosity wliicli, in 1885, afipcaicil lound Maia and Merope, now shown on more sensitive plates (Dec. Itis7j as well-defined nebula; of complex structure. Mr. Barnard, of the Lick Observatory, has discovered (Nov. 14, 1R90) a new [*
are
and somewhat round cometary nebula
elo.se
South and following Merope.
—En.]
—
20 Hight Ascension
Declination
1880.
1880.
S"
50"'
+39°
40'
Persei (S 471), primary 3.5 mag., companion 8 mag., distance 9".
s
The companion
is
probably variable,
colour too,
its
said to change from
is
blue to red. S"-
50™
+80°
99/
+ 12°
9'
S 460, Cephei, a very close double 6 mag., distance only 0.7".
10''
;
than 57"'
+G0°
Period 4 days
magnitude it
at
3.4, at
minimum
by an S-inch refractor
+62°
2
9'
more quickly
Rosse saw a star of 14 mag., sur-
in the centre
it is
To observe
of this nebula.
nebula in detail a most powerful telescope
57"'
It loses
4.2.
gains in brilliancy.
801, Nebula in Camelopardalis.
31'
It belongs to the
the changes in brilliancy, however, only occupy
;
maximum
rounded by a nebular ring
3"
primary, 5.5 mag'., companion
X Tauri, found to be variable by Baxendell in 1848.
Algol type.
3"
star,
is
required
:
this
even when examined
very faint.
485, Camelopardalis.
Two
stars of
about G mag. at 18" distance.
A
(S 484) consisting of three stars of 9 mag., precedes this double
triple star star. 4i>
1'"
+49°
809, Star Cluster in Perseus, very beautiful and rich in stars,
12'
diameter, rather crowded and irregularly round in shape. is
surrounded by a ring of faint
stars,
7'
in
This cluster
which cannot be well seen except
with a very powerful instrument. .
4''
1"'
+14°
50'
2
4h
2-"
+30°
28'
813, Nebulous Star in Taurus, a star of 8 mag., surrounded by a
495, Tauri.
Primary 6.5 mag., companion 9 mag., distance 4".
faint nebula 3' in diameter.
4"
G"
+48^
G'
f/.
Persei.
Discovered
be a double star by "W. Herschel, 2 Aug.,
to
The primary is 4 mag. and white in colour, the companion 8.5 mag. is at a distance 92". At Pulkowa another very faint companion was discovered, distance (according to Burnham) 14", position angle, 349°. 1782.
4''
6"
+50°
54'
820, Star Cluster in Perseus, rich in stars, nearly 15' in rather crowded with a in curves
4"
8"
^h
f)m
+
8°
58'
+15°
G'
;
number
30' to the south
of fairly brilliant stars, apparently
it is
Primary 5 mag., companion 8 mag., distance only 0.8". There is, in addition, a second very faint companion (12 mag.) at distance This last was discovered by Burnham. 32.2", position angle, 223°. 4,
Tauri.
Up
to
1872, J. Schmidt found that he could always
with the naked eye as of G mag.
decreased to 7 mag., and then again became visible
has any variation been observed in 9"
—10°
33'
4h
gm
—13°
9'
arranged
followed by a reddish-coloured star of 9 mag.
47, Tauri.
this star out
4''
diameter,
its
make
In September, 1872, it to the naked eye, nor
brilhancy since 1874.
A
Eridani (2 516), primary 5 mag., and yellowish in colour, with a First discovered to be a double very faint companion 9 mag., distance 6.3". star by W. Herschel, 31 Jan., 1785. 82G,
cording
Nebula in Eridanus, a
to Lassell there is a star of
discovered this view.
it
in 1785, look
The nebula
is
it
to
planitary disk,
of fair brilliancy.
12 mag. in the centre.
be a star cluster, and
a very small one.
its
Herschel,
Ac-
who
spectrum supports
21 Eight Ascension
Declination 1880.
1880.
4h
IQm
4''
12"
4h
,
—
7° 50'
+
49° 56'
—
— Right Ascension
Declination 1880.
1880.
4h
30m
22
+
53° 15'
Camelopardalis (2 566). 6 mag., yellowish, with a blueish composition distance (according to Eiigelmann, 1883), 1 .9" panion, 7.4 mag. 2,
;
;
angle. 291.9°.
4h
32in
+
15° 41'
Two
Tauri.
7
stars of 4.6
and 5.5 mag.
;
429"
distance,
can be
;
divided by the naked eye. 4h
35m
+
— 41m
+
Discovered by Chr. Mayer.
at distance 63".
9°
1'
Eridani (2 590). The primary distance 9". 55,
Found 411
4.5 mag., with an easily distinguished companion, 7 mag.,
T Tauri.
22° 44'
to
bo double by
W.
A star is
of 6.2 mag., with a companion,
7 mag.,
yellowish, the companion white in colour.
Herschel in 1783.
905, Star Cluster in Orion, consisting of 18 stars of from 8 to 11 mag.
10° 43'
Somewhat
Vogel has measured their relative positions with the
scattered.
micrometer. 4h
45m
V Tauri. A variable
4- 17° 20'
The
star
is
48"
+
53° 33'
reaches 8.3 mag.
it
;
minimum
at
it
Period, 108.6 days.
diminishes to 13 mag. 4"
recognised as such by Auwers, 1870.
star, first
At maximum
reddish.
A star of 5 mag., with a very faint 7, Camelopardalis (2 610). companion (11.3 mag.), at distance 25". Dembowski, in 1864, discovered that the primary was itself a double star, having a companion of 8 mag. at distance 1.2".
4h
50m
—
5° 22'
4h
51m
+
37° 43'
4h
gOm
+
7° 57'
Eridani, 6 mag., with companion 8 mag., distance 64".
b
A
star 5.5 mag., giving a greenish light, with 4, Aurigae (^ 616). First recognised as a double star by a companion 7 mag., distance 6".
W.
Herschel, 30 Oct., 1779.
E is less
4h
52m
+
A
Orionis.
than
variable
At maximum
Ilind in 1818.
star, it
of a deep red colour,
Period, 379 days.
1 3.
minimum
it
According to Schoenfeld the increase
in brilliancy
from 10 mag. upwards occupies 70 days
maximum
10 mag., 105 days.
to
by
discovered
reaches almost 9 mag., at
;
the decrease from
940, Star Cluster in Camelopardalis, fairly large and conspicuous.
53° 41'
The
stars are of various magnitudes,
and are
closer together towards the
centre.
4h
53m
+
43° 39'
£
is
Recognised as variable by Schmidt and Heis.
Aurigae.
3 mag., but has been seen at times as a star of 4.5 mag.
The
The
star
variations
of brilliancy are, hoAvevcr, very irregular, and are often for a long time
imperceptible. 4U-
54m
— 14°
Jt Leporis.
59'
star "
The
by Hind.
period
the star 4h
54m
+
3° 26'
is
is
A
variable star of a bright red colour, called a " crimson
Schmidt, in 1855, was the
first
to recognise
it
about 438 days, but -seems to be very irregular.
6 to
7, at
minimum
2 627, Orionis,
8.5 mag.
6,5 mag., with a
It
as variable.
At maximum
has a remarkable spectrum.
companion of nearly 7 mag.,
at
distance 21". This latterhas not undergone any perceptible change since 1831.
4h
5h
59m
o-"
+ +
1°
1'
37° 12'
A
96 P., Orionis. as of 7
tint is
probably
al.'^o
remarkable red-colouved
mag, but by Pirmingham,
and Besscl
field
estimated by Lalande
mag. The red
slight!)" variable.
996, Star Cluster in Auriga. a rich
star,
in 1871, as of 6
of stars.
Herschel
This first
is
saw
really not a cluster, but rather it
17 Jan., 1787.
brilliant stars contained in it are of 7,5 mag,, the faintest 11.5
The most
mag.
— Eight Ascension 1880.
5h
5"'
J.
Declination 1880.
3° 31'
23
— Right Asccasion
Declination 1880.
1880.
5h
lo-"
—
24
+
20°
S
0'
674, Tauri, a star of 6.5 mag., with a companion 9 mag., distance
10.5", position angle, 147.3°.
+
39° 59'
ham found
Burn-
5 mag., with a companion 9 mag., distance 121".
X Aurigae.
yet another
very
faint star at distance 40",
position angle,
198°.
+
39° 13'
Cluster in Auriga, a beautiful group of stars slightly
1067, Star
A
denser towards the centre.
7 mag. outshines all the
star of
others.
Discovered by Herschel, 18 Oct., 1786.
+
2
46° 51'
681, Aurigae, a double
star,
primary 6.5 mag., companion 9 mag.,
distance 23.2", position angle, 180.8°. 5'^
12"
—
6°
58'
This
T Orionis.
ham
AB It was
C
mag., 6^
17™
-f
3° 26'
star,
4 mag., has three very
gives the following measurements
in
Distance 36.2"
AC
„
Bb
„
Burnham who
faint
Burn-
companions.
:
249.1°.
Position angle,
60.0°.
30.1"
„
4.0"
„
50.0°.
B
discovered that
a double star
is
:
B
is
10.5
11 mag.
Orionis (2 696), a greenish-white star 5,5 mag., with a companion
(white) 7 mag.,
position angle,
31.7",
distance
No
28.1°.
change of
position has, as yet, been observed.
+
Ill, Tauri, a star of 5.5 mag., with a companion 8 mag., distance 75",
17° 16'
position angle,
5"
17"
— 24°
distance 3.5",
is at
distance 59", 17ni
+
Herschel had already made the measurements.
The primary
Triple star in Lepus.
54'
which 5h
271°.
is
is
is
G mag., the nearer companion,
9 mag., the farther companion, which
at
8.5 mag.
1101, Star Cluster in Auriga, fairly large, and rich in
33° 17'
is
stars, slightly
denser towards the centre. S'-
18"
—
T Orionis, 3.5 mag., with a companion, 5 mag., at distance
2° 31'
Dawes, in 1818, discovered that the primary was having a companion of 5.5 mag. at distance
1".
itself
a double
110". star,
It requires a very
strong instrument to "divide " this star. 6°
14'
7 Orionis, a star of 2 mag., supposed by J. Herschel to be slightly variable. Gould, too, finds slight variations, but only of about I mag.
— 24°
38'
1112, Star Cluster in Lepus, a splendid globular cluster discovered
+ .f.h
19"
by Mcchain, and which Messier described as a starless nebula with a Herschel was the first to resolve the nebula into stars. brilliant centre.
+
35° 13' 4' in
12.
+
2° 59'
1114, Star Cluster in Auriga, a somewhat crowded circular cluster, diameter, consisting of small stars ranging in magnitude from 9 to
Discovered by 4/
-
W.
Herschel, 17 Jan., 1787.
Orionis, a star of 5.5 mag., with
a very faint
companion of 11
mag., distance 2.9", position angle, 322°. :,''
21"
+
35° 47'
11 19, Star Cluster in Auriga, a beautiful object, about 10' in diameter.
Discovered by Messier.
The
stars are of
quadratic.
The
ful telescope.
A
unequal
cluster
is
brilliant star
brilliancy.
not at
all
Its
may
be observed in the centre.
form, according to Messier,
nebulous
if
is
examined with a power-
25 Right Ascension
Declination 1880.
1880.
6^ 22"°
5^
23""
—
+
25°
3'
— 20°
51'
118, Tauri (2 716), a double star, primary G mag., companion 7 mag. Discovered by Herschel in 1782, but since liis time the position of the companion has undergone little or no change. Distance 5", position angle, 200 \ This star, 3 mag., has, as discovered by Burnham,.sever;il /3 Leporis. very faint companions (10 11 mag.), whose position he thus calculated in
i879
—
:—
A B distance 2.7" position angle, U»So. A C A D distance 211.5"; position angle, 5yo. ;
75°.
In 1834, 5^ 2.3»
—
J.
distance 200.3"
;
position angle,
Herschel saw a faint star at about 70" distance, position
angle, 146°.
r
ir
31, Orionis (2 725), a double star, primary 5.8 mag., companion 11 mag., distance 12.7", position angle, 88.4°. The primary is reddish in colour and apparently variable at least Gould at Cordova estimated its magnitude at various times as 4.7 mag., to 6 mag. 32, Orionis (2 728), 5.2mag., with a companion 6.7 mng., distance (in 1878) only 0..5". In W. Herschel's time the distance was more tlian 1". 1137, Nebula in Auriga, a large, brilliant, circular nebula, witli a slightly increased brilliancy at the centre, where there is a triple star. The whole is 5' in diameter. Discovered by Herschel 4 Feb., 1793. According to Brodie the nebula is very faint. n' 33, Orionis (2 729), 6 mag., with a companion of 7 mag., at distance 1.9". Not easy to observe with an ordinary telescope. 2 730, Tauri, a double star, G.5 and 7 Distance 9.8". Position ;
5h
24-°
511
24"
5" 25-°
b^
25"
5''
25°-
5^
26"°
gh
27".
+ + + + +
5° 51'
3i^
9'
3° 12'
16° 59'
angle, 142°.
30° 21'
0°23'
+
A
21° 56'
[Nova Aurigae. This new star was discovered on January 24th, 1S92, by Dr. T. D. Anderson, of Edinburgh. It was found afterwards t" have imprinted its image on the photographic plate of Prof. Pickering, U.S.A., on the nights of December 10th and 20th, 1891. When discovered it was a star of the 5th magnitude; by April 2()th it had become a star of the 15th magnitude. Its spectrum was seen to be very like the JS^ora of 1866, and it has in many respects a spectrum similar to that of Vega. Vogel lias discovered in the spectrum, beside the hydrogen lines, the lines of the Solar Chromosphere, which had been recognised also in the Nova in Cygnus of 1876. Vogel also thinks, from an examination of the spectrum, that we have to do with three celestial bodies, one having a dark line spectrum, and the other two bright lines. The relative rates of movement of these bodies on the line of vision have also been calculated by Vogel. The increased temperature and consequent brilliancy may be owing to the near approach to each other of these bodies. Ed.] S Orionis, a double star, 2.5 and 6.8 mag. Distance 52.7". Burnham lately noticed yet another companion of between 13 and 14 mag., and remarks that this is one of the faintest that he has ever seen near a brilliant star. The primary is variable, but only to extent of half a magnitude, and the period 1157,
is
irregular.
Nebula
in Taurus. Seen as far back as 1731, by Messier, but imperfectly, and described by him as a starless nebula, something like a dull flame. W. Hersohel thought it capable of being resolved, and
Lord Posse, with bis great teleobject. he compared its obtain an exact view of the nebula appearance to that of a crab (crab-nebula) he saw several very minute stars in it, and gave a drawing of the whole. Dreyer, however, asserts that all the former representations of this nebula fail to give a satisfactory description of its appearance as seen through a telescope of the highest power. a Leporis, yellowish, 3.5 mag., with a companion 10 mag., at distance alluded to
scope,
it
was the
as a magnificent first to
;
;
5"
27"
— 17° 55'
5"
28"
+
35", position angle, 156°.
34°
4'
A
1166, Star Cluster in Auriga. Near the star <p. cluster 9' in diameter, a very fine view of which may be obtained with a 3^-inch The stars are from 7 to 11 mag., the double star 2 737 (S and refractor. 9 mag., distance 10.6".) being among them.
E
— Right Ascension
Declination 1880.
1880.
5" 29=
—
26
+
9° 51'
X Orionis (2 738), a yellowish-white star, 3.5 mag., with a reddish 4". This latter had already been seen by
companion 6 mag., distance
Struve found another very faint star
Hei'schel.
position angle, 184°,
(12 mng.), distance 27",
and another of 10.5 mag., distance 149", position
angle, 278.
5^ 29"'
6°
2
5'
ti^
29"
5° 28'
star, 5.6 and 6.5 mag., distance 36". companion has not changed since 1833.
The
747, Orionis, a double
position of the
in Orion, the most conspicuous and interesting kind in the Northern Heavens, and an inexhaustible field of No descripall who have a powerful telescope at their disposal.
The great Nebula
1179, object of
its
research to
The
tion can give an adequate picture of this nebula.
given by
De
earlier accounts
Only the Tempel can be considered at all
Vico, Herschel, and others are not satisfactory.
sketches given by Rosse, Bond, and
In Sheet xiv. will be found a reproduction of Bond's masterThis map was obtained with the help of a 14-in. refractor, a piece. first-class instrument, though far inferior to Eosse's 6-foot reflecting telescope adequate.
Nevertheless, this latter failed to discover
in point of illuminating power.
any additional feature of importance. Bond's drawing covers an area of Taking the quadruple star, S Orionis (2 748), which forms the celebrated Trapezium, as a starting point, this area extends 2' 15"
31° square.
on both sides in liight Ascension, and 1° 30' in Declination to the north and south respectively. The chief nebula round S seems to be connected with the nebula? round
c
and
i
;
a
of 1,101 stars, all
list
is
undecided.
of which, however, are in positions where his refractor
Bond has
shows
itself
in
several frequently proceed from a
many stars
;
also
a kind of spiral structure in certain portions of the Orion
This
nebula.
Bond has given
G. P.
showed nebular matter connected with the great nebula. pointed out
Rosse and Bond
at least, the observations of
point to this conclusion, while Herschel
attempts have been
made
narrow
common
to resolve the
Huyghens, and
streaks,
of
of
which
Since Herschel's time,
nebula in Orion into separate
Trapezium, which
especially has the part south of the
called after the astronomer
crooked
centre.
is
generally
which the most brilliant portion
seems to be drawn out into a rhomboidal or lozenge shape, been carefully examined wath the most powerful telescopes with a view to disintegration.
For a long time
it
was reported that Lord Rosse's great
telescope
had
succeeded in resolving this portion of the nebula into a star cluster, hut this Rosso and his collaborateur, Hunter, succeeded only in was not the case. discovering faint luminous points in individual places where no stars had
been seen previously.
Finally, spectrum analysis has proved that the nebula
composed principally of masses of luminous gas. The central portion may be said to be marked off by the four brilliant stars which compose the celeis
brated Trapezium, which, standing on a dark background, are surrounded by
masses of luminous nebula. labours by
The
elder Herschel,
measuring the distances of the
observed more than four stars there. Sir
ill
Struve saw a
fifth
his astronomical
Trapezium, never (12 mag.) in 1826
;
1832 discovered a sixth of 13 mag. and 1839 saw three others, but these have never since been again
John Herschel and South
De Yico
who began
stars in the
in
;
•M
Right Ascension
Declination 1880.
1880.
Lament
observed even in the most powerful telescopes.
also discovered
two
stars which could be considered as belonging to
the Trapezium, and Lasscll, at
Malta, 2 Jan., 1862, another very faint
that altogether the
star, so
tot;il
num-
ber of stars belonging to the Trapezium, which have been observed within a
These, however, have never
space of 4 minutes square, amounts to 11 or 12.
been
same time
visible at the
unquestionably one of the ablest, particular vi'sible in
if
He
in
able, observer
more than
is
this
six stars are
the Trapezium, and considers the observations which
tbeory to be untrustworthy.
oppose this
likewise refuses to credit the supposed
This
variability of the fifth or sixth star.
[From
not the most
absolutely declines to admit that
field,
who
Moreover, Burnham,
to one observer.
he thinks
last
to be
12 mag.
of
the splendid photographs taken 1888-89 by Mr. Roberts,
it is
clear
that the mass of the nebula is concave towards an axis "passing through the Ranyard, Trapezium in a north-easterly and south-westerly direction."
Knowledge,
&"
30"
—
xii.
These photographs
147.
p.
4°
27'
An
1184, Star Cluster in Orion.
—
extended group of
Among them
7 mag., besides some fainter ones. &" SO-"
show an implication of
also
outlying I'cgions in the great spiral sweep of this nebula.] stars, of
6 and
is a double star (2 750),
6 and 9 mag., distance 4.3". 6°
0'
A
(S 752). triple star, primary 3.5 mag., companions, W. Herschel saw only the companion of 7 mag. at distance The farther and fainter companion (distance 50"), was observed by
Orionis
1
7 and 9.5 mag. 11.3".
South in 1824.
[This triple
is
said to be enveloped in a nebula.
"System
of
the Stars," p. 262.] S''
30"
S'^
1185,
21'
Nebula
in Orion, fairly brilliant and
the centre, where there object,
i""
30">
+21°
and described
it
is
towards
brighter
a star of 8 mag.
as a star with a nebulous envelope.
A
1191, Variable Nebula in Taurus.
9'
large,
Messeir had observed this
star of
11 mag. was observed
by Chacornac in 1852, but without any trace of nebula. Next year he saw the star again, this time surrounded by nebula; on 27 Jan., in this place
1862
1856, the nebula had become very brilliant, but in
The
disappeared, and has not since been observed.
had
it
star (11
entirely
mag.) has not
been observed to vary. S^
30-°
1°
1193, Nebula round
17'
he
writes in his diary that
e
Orionis.
is
On
Jan. 2,
nearly certain that
by an irregularly blurred, milky mass of nebula. it
turned out, a just one
nebula round the
star.
;
several
even with
+25°
3',
The
stars are all
very numerous.
+30°
26'
s
26, Aurigae.
Herschel
surrounded
This observation was, as
efforts, it
it in 1850 and 1852 was impossible to distinguish ;
Orionis has besides a faint companion, of 9
position angle, 57°.
1199, Star Cluster in Taurus.
45'
is
Rosse's great telescope showed
this instrument,
mag., distance
W.
1786,
Orionis
other observers have noticed the faint
but in 1874 and 1878, in spite of many it,
e
A
large
cluster,
15'
in diameter.
of nearly equal magnitude, and evenly distributed, but not
Discovered by Herschel, 7 Dec, 1785.
A double star,
by "W. Herschel in 1782.
6 and 8 mag., distance 12".
Burnham found
distance, 26", position angle, 113°.
also
a small
Discovered
star,
11 mag.,
—
-28
—
Declination 1880.
33"
18j:0.
•2"'
40'
Orionis.
«•
A multiple star,
and two very faint one companion B
C
another
mag.),
(7.5
mag.},
(6.0
really a group consisting of
The primary
stars.
762j
(5:
12",
distance 61",
distance
very faint companion (11 mag.),
angle, 236^.
The second quadruple star The three most brilliant
322^.
Between these two groups
is
x,
distance
of
angle,
48°;
42';
and
angle,
distance
at a
stars
two quadruple
4 mag., and has
position
position
finally a third
angle,
is
this
a very powerful instrument shows
12",
position
3|',
position
are
mag.
8.5
two very
faint
[There seems to be no relative motion among the members of the
stars.
group.] b^
34"'
-17"-
45, Leporis, a Multiple Star.
55'
tuple, but
were
first
tudes:
Described by J.
Herschel
as quin-
has other companions as well, though they are very faint, and
discovered by
A 6.8, B 9.3,
Burnham that
it
C
Burnham. 8,
D
8.5,
E
The 8.5,
latter gives
F 13, G
the following magni-
directed his attention to this system of stars
A and B
were each of them double
ments, calculated by
stars.
Burnham and Dembowski,
of the various stars belonging to the system. angle.
d
b he saw
10, a 8.3,
The
9.7.
at
When a glance
following measure-
give the relative positions
d=distance, p
=
position
— Right Ascension
Declination 1880.
1880.
+ 65°
— 22° —
5h
40m
5"
41'°
gh
40m
+
6°
511
44m
+
32°
5"
0°
43'
29'
29
— Right ABcension
Declination 1880.
1880.
gh
3m
Q^
G"
IP
+
8'
5° 29'
6^
+
12°
50'
6"
+
36°
12'
6^
gh
IQm
&"
IS™
gh
19m
Qh
21-
30
—
Eight Ascension
1880.
+
11° 22'
2 mag.
26""
—
Declination
1880.
&"
31
+
4° 57'
921, Monocerotis, a star of 6.5 mag., witli a companion of nearly 8 Distance 16", position angle, 4°.
1424, Star Cluster in Monoceros, visible on a clear night, with the as a nebulous star. With a telescope is seen to be a somewhat dense cluster of stars, one of which (12 Monocerotis) is of 6 mag.
naked eye 6"
26"'
+
10° 15'
6
28"
+
7° 40'
gh
3;^m
+
16° 30'
A
1452, Nebula in Monoceros. very interesting object, fairly bright, comet-shaped, or rather fan-shaped, extending from a star of 10 to 11 mag. The whole is probably H' long. 14, Monocerotis (2 938), yellowish-white, 6.5 mag., with a very companion (12 mag.) Distance 10", position angle 209.9°.
7 Geminorium, a star of 2.5 mag. with 2 siderable distance.
AB
AC
Burnham
faint
faint
companions at a con-
gives the following measurements.
Distance 141.7" 294.7" „
Position
angle,
„
335.5° 133.0°
6"
32"
+
10° 59'
1435, Star Cluster in Monoceros, large, containing about 40 stars of 9.5 to 12 mag., which are irregularly distributed.
6"
34"
+
10°
S (15) Monocerotis (2 950), the chief star of a coarsely scattered star cluster (G.C. 1440) 6 mag., with two companions, one 9 mag., distance 3",
0'
the other 11.5 mag., distance 16". The primary is surrounded by a thin veil of nebula, and, as discovered by Winnecke, varies about half a magnitude. The duration of light variability is only 3 days, lO*" 38™. The colour of this star is described by Struve as green, it is now yellowish. 6"
36"
+
59° 34'
W.
12, Lyncis (2 948), triple, 5.2, 6.1 and 7.4 mag. Discovered by Herschel in 1780. The nearest companion is at a distance 1.4"; the
further at distance 8.7". 6"
37
+
25° 15'
This white star of 3.5. mag., £ Geminorum. 8.5 mag., at distance 111", position angle, 94°,
6"
38°
+
43° 42'
6 mag., of a clear white colour, with a blueish-white 56, Aurigae. companion 8 mag., at distance 48", position angle, 21.1°.
e"
38"
+
55° 52'
2 958, Lyncis. 6 mag., consisting of two white stars of almost equal magnitude, at distance 5".
6"
40"
— 16°
33'
has a companion of
The most brilliant fixed star in the a Canis Majoris (Sirius). heavens viewed with a powerful telescope, it is of dazzling splendour, and may be compared to a sun. [Hydrogen lines are very strong in the ;
The ancients described Sirius as red, at present it is perfectly spectrum.] white it has probably changed its colour since the days of Ptolemy. [But see " Observatory," No. 120, p. 104.] Bessel (in 1844) was the first to declare that Sirius must have a companion, as its proper motion showed irregularities which could be only explained by this hypothesis. In January, 1802, the companion demanded by Bessel's theory was discovered by the younger Clark with an 18-iuch refractor it was afterwards actually seen with smaller instruments, and Auwers estimated the time of its revolution The companion is 8.5 mag., and in 1800-70 was at distance at 49 years. 10", but this has gradually decreased [in 1889 only 5"], and the companion cannot now be distinguished except by a telescope of great power. [The The companion is probaby not less periastron passage is timed for 1896. than half the mass of Sirius, and it is instanced as the case of a star already approaching solidity and obscurity.] ;
;
— Right Ascension
Declination 1880.
1880.
6"
41"
—
32
+
41° 12'
1451, Star Cluster in Auriga, fairly
Discovered by W". Herschel, 3 Feb., 1788.
double star near the middle. (Jh
42m
with a
rich, coarsely scattered,
1453, Star Cluster in Monoceros.
Coarsely scattered,
not rich,
contains stars of 8 to 11 mag. gh
42in
— 20°
37'
1454, Star Cluster in Canis Major.
and recognised
as
a
A
magnificent object, described
The
by Messier.
star cluster
smallest astronomical
telescope will suffice to distinguish separate stars in
Seen with the
it.
lowest power of a refractor, the whole field of vision seems full of stars of
A
various magnitudes. Qh
42m
_(_
590 34-
14,
splendid sight
A
Lyncis (2 9G3).
mag., and of a golden colour Struvc.
red, according to is
e^
46"
+
0° 36'
Near the
Burnham
+
13° 20'
A
C;
Geminorum
38,
The
(1878).
48m
+
18°
8'
rjjm
— 13°
The primary and of
distance
seems
diminish.
to
a
is
6
purple
the latter
A
very
is
20' in diameter, rich in small
a triple star 8 and 9 mag., for which
A B;
(2
distance 20.9";
distance 8.6", position angle, 281.9°.
982). blueish.
Primary
mag.,
5.4
Distance 6.3",
and
yellowish,
position angle,
164°
colours of both stars are relatively intense.
A
triangular cluster consisting of 1467, Star Cluster in Gemini. The whole, in the average telescope, looks like small stars densely crowded.
Discovered by AY. Ilerschei, 30 Dec, 1783.
a nebula. Qh
star,
(1880) gives the following measurements:
companion 7.7 mag., and
gh
the
centre there
position angle, 80°;
48"
double
required to divide the companion from the primary.
is
1465, Star Cluster in Monoceros. stars.
6"
;
difficult
the companion 7.1 mag.
Distance 0.8", position angle, 64.1°;
slowly increasing, while
powerful instrument
very
Canis Majoris (2 997), a yellowish star 4.7 mag., with a blueish
53' ij,
companion 8 mag., distance 2.5" (1878), slowly decreasing, position angle, 342°, apparently unchanged since 1831. 6'^
52"
+
10° 25'
1474, Star Cluster in Monoceros, consisting of a large number of coarsely scattered stars of 10 to 11 mag.
Qh
54m
— 13°
32'
1479, diameter.
Star Cluster in Canis Major, somewhat scattered, 20' in The stars are from 8 to 11 mag. Discovered by Herschel,
8 Feb., 1785. G*"
56"
+
2
52° 56'
1009, Lyncis, a double star 6.7 and 6.8 mag., both of a brilliant Distance 3", position angle, 156° this latter has probably
white colour.
;
decreased since Struvc took the measurement in 1830. C"
57"
+
20° 45'
^ as
Geminorum,
variable by J.
a star of a deep yellow colour,
mag., and lasts 10 days
more rapid than the
The
first
position
at
3''
43".
increase.
distance
angle, 84°.
The
Schmidt in 1844.
94",
3.7 mag., recognised
variation of brightness
= 0.8
somewhat The ^has two companions 7 and 10.5 mag. decrease in
position
angle,
brilliancy
352°,
is
the latter 87",
— Right Ascension
Declination 1880.
1880.
gh
57m
6''
oS'"
—
8° 10'
16° 27'
+
22° 53'
7h
0°
+
27° 23'
7h
2""
+
10° 14'
7"
7h
711
— 26°
12'
+
13°
59'
ll"
+
16° 45'
i2">
+
73° 19'
12°'
7h
7h
14m
13°
0'
33
—
— Right Ascension
Declination 1880.
1880.
+
7"
14°
1'
— 11°
19'
34
— Right Ascension
Declination 1880.
1880.
7h
3gm
—
35
—14°
32'
1564, Star Cluster in NaYis, extends over 30', and small telescope, discovered by Messier.
mag.
In
this cluster
W.
The
Herschel found a
stars faint,
is visible
range from 7.5
with a to
11
planetary nebula 2'
in
diameter, which Rosse declares to be annular. rjh
37m
—17°
55'
7h
37m
+28°
A
1567, Nebula in Navis. the edges.
30'
;3
planetary nebula, somewhat blurred at
It looks like a nebulous star in ordinary telescopes.
Geminorum
companions,
all
A
(Pollux).
brilliant star
of which are very faint.
W.
of 1.5
mag., with several
Herschel saw one of them in
1784, South another in 1825, and Struve a third in 1836. the
first
that the nearest companion distance telescope.
is
so
small that
Burnham
AB
rjb
37n
+24°
41'
7h
39n
+33°
44'
7h
39m —23°
35'
7h
42-°
-11°
54'
7h
42"
+24°
2'
7h
4gm
+22°
19'
52"
+
2°
33'
54"
—10°
27'
is it
gives
system, 1879-80,
Distance
Burnham was
view of the whole system, and he discovered
to obtain a complete
itself
double, 10 and 12.5
mag., but the
can be divided only with a very powerful the following measurements
of the whole
— Eight Ascension
—
36
Declination 1B80.
1880.
-j-h
5611
+
9^
46'
gU
in
—
8°
54'
1617, Nebula in Canis Minor, fairly faint, small (30"), elongated, with sudden increase of brilliancy at the centre.
2 1183, Monocerotis,
a yellowish white star of 5.5
mag. with a com-
panion 8 mag., distance 31".
3m
gh
—
2°
29, Monocerotis (2 1190), a yellowish star 5 mag. with two faint commag., distance 31.6" and 67", position angle, 105°.
38'
panions 9.5 and 9
and 245°. -12°
1630, Star Cluster in Navis, 20' in diameter, coarsely scattered, rich Discovered by W. Herschel, 31 in small stars, among them a double star.
34'
Jan., 1785.
+
18°
1'
^
Cancri (2 1196), a
triple star, consisting of
a double star 5.5 and 6
mag., distance only 1", and a farther companion 5.5 mag., distance 5.4". VV. Herschel saw the inner companion in 1781, but later on, neither honor
South could distinguish it. Struve was the first to find it again in 1826. [It seems now, from observations made by M. Seeliger and others, that these three bright stars are attendants on a dark body of greater mass than any one of them.] 8" 8'^
6°
—12°
34'
8"
—
26'
5°
1632, Navis, a nebulous
star, 6.7
mag. Fairly large and crowded with
1637, Star Cluster in Monoceros. stars of 9 mag., also a pretty double star.
gh
10"
+12°
Ji Cancri, discovered to be variable
yellowish red, at
maximum
6.5, at
by Schward in 1829.
minimum 12 mag.
The
The period
star is is
354
days and seems to be gradually lengthening. gu
15m
+17°
V
40' is
Cancri, found to be variable by
under 7 mag., at minimum
less
Auwers
At maximum
in 1870.
The
than 12 mag.
period
is
it
nearly
270 days. 8^
20-°
+27°
20'
(p-
Cancri (2 1223), 6 mag. with a companion 6.5 mag., distance 5",
divided long ago by Chr. Mayer.
Cancri (2 1224) 6 mag. with a companion 7 mag., distance 5.9".
8"^
20" +24°
56'
V
8"
25" +18°
30'
S
Cancri, a yellowish star 5.5 mag., with a faint companion, distance 61".
8''
29"
2
1245, Hydrae, a star 6.5 mag., with a somewhat fainter companion,
+
7°
2'
^
distance
No
10.3", position angle 25°.
change in position has been
noticed during the last 60 years. 8^
33"
+20°
22'
1681, Star Cluster in Cancer, visible to the naked eye, the so-called "PrcBsepe."
With
a telescope this cluster, which
can be easily resolved. gh
37m
-|-19°
28'
S
minimum 8^^
lasts
8^
39" +•29°
1
very rich in stars,
Cancri, found to be variable by Hind in 1848.
yellowish variable belongs to the Algol type.
12'
is
^
;
9.8 mag.
Period 9 days
11''
38".
This somewhat
At maximum it The decrease in
is
8.2,
at
brilliancy
the increase 13^.
Cancri (2 1268) 4.5 mag. with a companion 6.5 mag., distance 30.7", Discovered to be double by Herschel, 8 Feb., 1782.
position angle, 307.3^.
gh
4Qm +78°
40'
1691, Nebula in Camelopardalis, fairly bright, and tolerably large,
with an increase of brilliancy towards the centre, at
first
gradual, then sudden.
— Eight Ascension
Declination
1880.
1880.
8" 40-"
+
6°
51'
3h
45m
+51°
46'
8h
45m +12°
15'
gh
45™ +33°
53'
gh
45m
—
6°
41'
gh
47m
+
3°
31'
8"
9^
8"
37
—
— Bight Ascension 1880.
gh
iim
9"
11"
gh
12™
9h
14m
gh
14m
gh
21m
9^
22°'
9"^
38
—
39 Right Ascension
Declination 1880.
1880.
9h48m
+
5°
30'
9,
Sextantls.
A
icddisli
star,
7 mag., with a companion 8 mag.,
distance 53", position angle, 292°. 9'"
59"'
2008, Nebula in Sextans, discovered by Herschel, fairly brilliant with an increase of light towards the centre which resembles a star of 9.5 mag. Very faint when viewed with a small telescope.
A
+
12° 33'
a Leonis (Eegulus). At brilliant star with a beautiful spectrum. distance 3' is a star 8.5 mag., which has the same proper motion as a.. There is an extremely foint companion at distance 3.3", position angle, 88.5°.
10''
7-"
+
74°
0'
2024, Nebula in Draco, fairly brilliant, large, round, with of brilliancy towards the centre, at first gradual then abrupt.
IC
8"'
+
4°
1'
2038, Nebula in Sextans, fairly brilliant, small, round, with a sudden increase of brightness towards the centre. It is followed in the field of vision by another fainter nebula not noticed by "W. Herschel.
10M3'"
+
20° 27' red
an increase
7 Leonis (- 1424). A golden-yellowish star, 2 mag., with a greenishcompanion of 3.5 mag., distance 3.4". According to Struve, the
most beautiful star in the northern heavens. Singularly enough, W. Herschel gives both stars as white. [It has been calculated that if this star be of equal density with the sun, then it is three hundred times more brilliant than the latter. If we suppose its light equal to that of the sun, then its density must be seven times rarer than air at standard pressure. A. M. Gierke, 8yHicm of the Stars, p. 203.] 10" 19-"
18°
2'
A
planetary nebula nearly 1' in diameter, 2102, Nebula in Hydra. W. Herschel saw no traces of a starry nature in it. To Secchi, on the other hand, it appeared quite differently within a circular nebula he distinguished two star clusters, which are bound together by a fairly brilliant.
;
shining ring composed of two semicircles of stars. There is also a star in Tempel thinks tbe nebula very wontbe nebulous space at the centre. He considers it to be a small, oval, brilliant disc of light surrounded derful. by sharply defined, densely collected stars. In the southern central and northern portions shine out a few stars of greater brilliancy. "These," says Tempel, "like living, pulsating points, form a striking contrast to the dark background, which is totally free from nebula."
lot 21'°
+
29°
7'
2104, Nebula in Leo Minor, fairly brilliant, elliptical in shape, with a kind of brilliant nucleus in the centre.
10''29"'
+
9°
16'
G mag., with a companion 9 mag., at distance 49, Leonis (- 1450). 2.4", the position of which does not seem to alter.
10" SI-"
+
54°
8'
10" 36"
+
69° 24'
2168, Nebula in Ursa containing 2 stars of 10 mag. i?
12 mag. 10" 37"
10" 37"
Ursae Majoris.
At maximum
+
25° 33'
+
12° 20'
+
A
somttinies
planetary,
with
blurred
edges,
variable star, recognised by Pogson in 1853. (J, though often only 8 mag., at minimum
Period, 303 days.
2178, Nebula in Leo Minoris, fairly bright, with an increase of There is a star surrounded by the nebula. Rosse sees spiral coils round a luminous centre.
brilliancy towards the centre.
2184, Nebula in Leo, discovered by Mechain, and described as a very nebula it really is fairly brilliant, large and round, brighter at the centre, with a nucleus resembling a star of 10 mag.
faint starless
10" 37"
it is
Major,
5°
23'
;
35, Sextantis (S 1466). distance 67", position angle, 240°
6.5
mag., with a companion 7 mag.,
— Right Ascunsion
Declination 1880.
1880.
IQh 40-°
+
12°
27'
10" 42°'
+
13°
16'
10" 45""
—
8°
10'
10" 47"
+
57° 37'
10" 49"
+
25° 24'
10" 52"
4- 59°
10" 53"
+
lO*"
54"
+
lO*"
54"
+
62° 50'
10" 55"
+
57°
10" 57"
+
28° 37'
10" 59"
+
11"
4"
+
56° 19'
11"
8"
+
55° 40'
11"
9"
11" 12"
33'
29° 37' 4°
0°
16'
2'
37'
40
—
— Bight Ascension 1880.
ll" 12'°
11'" 14"'
11" 18-"
41
— Eight Ascension
—
42
Declination 1880.
1880.
+
11" 58-"
22°
8'
2,
159G), 6 mag., with a companion
Comae Berenices (S
mag.,
7.5
distance 3.7".
loh
1"
j
_|_
430 44'
2723, Nebula in Canes Yenatici,
4"
4- 19° 13'
jOh
5m
+
2
40° 33'
1606,
7m
+
ir>° 34'
Berenices, of moderate
very
size,
bril-
the stars are more densely collected towards the centre.
A
Canum Yenaticorum.
7 mag., distance lOh
Coma
2752, Star Cluster in liant, globular,
with a very
Discovered by IIer.?chcl 14 Jan., 1788.
brilliant neucleus. 12''
fairly bright, elongated,
star of 6 mag.,
with a companion
1.4".
2786, Nebula in
Coma
with
Berenices, a large pale nebula 15' long,
Tempel found
Discovered by Mechain 5 Mar., 1781.
a star-like centre.
another small round nebula to the southward. 12h lO"
+
41° 20'
2,
Canum Yenaticorum
with a
mag.,
(2 1622), a reddish star 5.5
The
blueish companion 8 mag., distance 11.4", position angle, 260°.
colours
are fairly decided.
12" lO-
+
13° 48'
2806,
Nebula
9' to 10' long, brighter in
in Yirgo.
covered by Herschel 8 April 1784.
It
Dis-
the centre.
Tempel saw
spindle shaped, and
is
two accompanying nebula. The one preceding it to the south is 5' long, oval in shape, and has 3 brilliant nodes it is situated towards the centre of the principal nebula star 10 is
round,
2
3° 17'
12" 12"
— 11 mag. 1' in
:
— 35^ —
;
To the south there
6h'.
The companion nebula on the
north,
a small
follows
which
follows
it,
diameter, and very faint.
1627, Yirginis, 6 mag., with a comjianion 6.5 mag., d z=20", p
=
196°.
12" 13"
+
15°
4'
2838, Nebula in
Coma
Berenices.
Discovered by Mechain
1781, and described as a starless nebula. refractor at Leipslc,
and found
it
to
Vogel observed
be
large,
magnifying power 192, a spiral arrangement was 12" IS""
+
2841, Nebula in Ursa Major,
47° 59'
Discovered by
shows that 12" 13"
—
18° 35'
+
5°
8'
this
nebula
brilliant,
starlight points.
With
visible.
with a nucleus,
fairly
large.
A continuous spectrum
of rcsolvability.
a very distinct star cluster.
is
Ji CorYi, recognised as variable it
12" 16">
No trace
Ilersclicl.
with the 8-inch
and apparently
brilliant,
where there are two bright
resolvable at the centre,
it
15 Mar.,
generally reaches 7 mag.
;
at
2878, Nebula in Yirgo.
by Karlinski
minimum
it is
At maximum
in 1867.
11.5 mag.
Period 319 days.
A
Discovered by Messier 1779.
very faint
nebula ia which Herfcliel recognised two nuclei. 12" IG"
+
2G° 31'
12
Comae
Berenices, 5 mag., with a companion 8 mag.
Distance
66", position angle 169°.
jgh 17m
4- 16° 29'
2890, Nebula in
Coma
1781, fairly largo, round and
12" 19"
+
13° 34'
2930, Nebula in
suddenly increases in
Berenices.
Discovered by Mechain 15 Mar.,
faint.
Yirgo, a brightness
fairly brilliant,
towards the
circular centre.
nebula,
which
Discovered by
Messier.
12" 19"
+
18° 52'
Coma
Berenices.
described as faint and starless.
Herschel
2946, Nebula in follows 2' southward.
Discovered by Mechain, calls it brilliant.
A
star 9
and
mag.,
43 Eight Ascension 1880.
12" 20"
12" 21"
— Right Ascension 188Q.
SI"
+
60°
12" 32°'
+
12° 29'
12" 32"
+
7° 39'
12" 33-"
— 26°
12''
12" 34-°
12" 36-"
12" 38" 12" 38-°
12"
'69""
9'
5'
44
-^
— Right
45
Declination
A sceneion
1880.
1880.
+
12" 45-"
6°
U Yirginis,
12' is
recognised as variable by Harding in 1831.
reddish, and at
maximum
8 mag., at minimum 13 mag.
The
star
Period nearly
207 days.
+
12" 47-"
11°
53'
3278, Nebula in Yirgo. Two faint nebula3 at 8' to 10' distance from one another. Discovered by W. Herschel on 15 March, 1784. The preceding nebula
+
12" 47"
21°
54'
35,
is
Comae
long and thin and has an elongated nucleus.
Berenices, (2 1687), 5 mag. and yellowish, with a blueish
companion 8 mag., distance
1.3",
and a second companion 9 mag., distance
28.5".
— 11°
12" 49"
56'
3293, 3294, Nebulae in Yirgo, double,
Tempel has made
nebuliB in the vicinity.
+
12" 50-°
38° 58'
a
with other small, faint
faint,
map
of this group of nebula).
2 1692, Canum Yenaticorum. The brightest star in the constellation and known by the name of " Cor Caroli." The star is a little over 3 mag., and has a companion 6 mag.
at distance 20", in
whose position no change
has yet been observed.
+
12" 51"
54° 44'
p
+ 14°
12" 53"
2
=
1695, Ursae Majoris, 6.5 mag. with a companion 8 mag., d
49'
3342, Nebula in
Coma
+ 11°
36'
13"
+ 18°
4°"
3.2",
=
is
of fair size with
a small star in this nebula.
= 120°.
241" p
10'
There
Yirginis, a star of 4 mag., with a very faint companion (12 mag.),
£
d
A brilliant nebula
Berenices.
a core-like density at the centre. 12" SG-"
:
287°.
42,
distance
double
Comae Berenices (2 1728). Two stars so small that they may be considered one
is
stars.
Struve,
who
of 5
mag., but whose
of the most difficult of
discovered their duplex character in 1827, could
generally only distinguish an elongated star, actual division being only occasionally possible. star
Burnham, however,
;
angle, 192°. still
+ 39°
4-°
in 1879,
in 1863,
too,
saw only an elongated
measured the distance as 0.67", position
Since 1882 the division has been easier than heretofore, but
[These stars
requires an instrument of the first-class.
oscillate to
and
about 26 years, oculting each other twice in a revolution.]
fro in
13"
Dembowski
8'
15, 17,
5.5 mag.
Canum Yenaticorum,
The
distance
is
two
4' 30", still
stars
of nearly equal brilliancy,
they cannot be divided without a
telescope.
13"
—
4°'
4°
54' fi
7.1'',
13"
5" I
+
37°
42' 1.5'
Yirginis, triple, 4.5, 9 and 10 mag.
p
= 344°, the farther and
7-"
+
18° 48'
d
The nearer companion
is
d
=
— 71", p = 297°.
3437, Nebula in Canes Yenatici, a fairly brilliant nebula, 6' long by Increases a"bruptly in broad, discovered by Herschel 1 May, 1785.
brilliancy towards the centre,
13"
fainter,
3453, Star Cluster in
where
Coma
it
has what looks like a nucleus.
Berenices.
Discovered by Messier in
In reality it is a star cluster in 1777, and described as a starless nebula. very beautiwhich, according to Eosse, 4 or 5 condensations are visible.
A
ful object.
— Eight Ascension
—
46
Declination 1880.
1880.
13" 10"
+ 42°
13" IS-
— 10^
40'
3474, Nebula in Canes Yenatici.
Discovered by Meehain in 1779, and described as a faint and starless nebula. According to Herschel, it is 10' long by 4', with a bright nucleus. Iluggins finds that it gives a continuous spectrum, which proves it to be a star cluster at an immeasurable distance. [a Yirginis (Spica).
3'
Professor Vogel announced on April 24, 1890,
that this consists of two close stars (companion obscure) of equal mass,
round their
revolving-
spectrum IS" IG" *See Nature
+
55° 33'
^
common
of Class IV.
is
centre of gravity in
—Ed.]
4-0184 days.
The
Ursae Majoris, 2 mag., and greenish-white, with a companion 4.5 One of the most beautiful double stars in the heavens.
mag., distance 14".
Feb.27, 1890 p. 403,
At
11' 47" distance from ^
is
or Alkor, and, in addition, a star 8 mag.,
r;
distance 8.5', together with several fainter ones,
13" 20"
W Yirginis,
2° 45'
maximum 22° 40'
At maximum 2.'5°'
+
47° 49'
it
it is
seems
variable
as
is
very uniform.
recognised as variable by Maraldi in 1704.
star,
minimum 10 mag.
4 to 5.5 mag., at
3572, Nebula in Canes Yenatici. faint,
starless nebula,
Discovered by Messier in 1773, but double, each portion being
W.
bright in the centre, and 4^' in diameter.
a
circular
brilliant,
surrounded by a
nebula,
accompanied by a second nebula. were also wrong. nebula,
It
refractor.
These
true
also
as
and
and drawing
structure
wound round
have
spiral coils
it
nebular halo
J. Herschel's description
Hosse's telescope showed the
centre {Vide Plate xvi).
tinguished and
Herschel describes faint,
a spiral mass which seems to be
i.e.,
Period 437 days,
have been longer.
to
and described as a
by Schoenfeld in 1866. At to 10.4 mag. Period 17.3
minimum 10
of brilliancy
Hydrae, a deep red
-K
formerly 13"
recognised
9 mag., and at
The change
days.
13" 23"
is
it
of the
a brilliant
been clearly
dis-
mapped out by Vogel, with the help of the Leipsic 8-inch would thus seem that we have here a mass of a really
nebulous character coiling in vast convolutions round an enormous centre, yet
spectrum analysis contradicts
The nebula has
this theory.
lines,
a con-
and without any bright
tinuous spectrum similar to that of the stars,
which are never absent from the spectra of true incandescent nebulaj.
[Mr. Roberts' photograph, taken 1889, in four hours' exposure, gives clearer 13" 27"
—
arrangement of
details of the
6° 35'
S
brilliancy
is
somewhat
times only 8 mag., at
13h32m
_i7o
13" 32"
+
16'
this nebula.]
Hind At maximum
Yirginis, recognised as variable by irregular.
minimum under 12 mag.
3614, Nebula in Yirgo, faint
;
in
1852
the star
;
is
the change of
5 mag., some-
Period 374 days.
according to
Lassell, a spiral with
two arms. 36° 55'
25,
Canum Yenaticorum
A
(S 1768).
star of 5 mag., with a
com-
panion 7.5 mag., distance (when discovered by Struvc in 1829), 1.05."
It
has decreased since then, and Eugelmann, in 1883, calculated it as 0.8". Apparently the distance is The companion's position angle was 151°.
now 13" 32"
+
9° 30'
increasing again.
3615, Nebula in Yirgo, nebulous nodes in the centre. several fainter ones to the north. in its vicinity.
10' in length, with
brilliant,
9'
There
one star to the south of
is
to
Tempel discovered some very
it,
two and
faint nebula)
— Right Asoenaion
Declination 1880.
1880.
IS" 35"
+ 20°
37"
+ 4° + 28°
13''
13'' 37-"
34'
9'
59'
See Nature^ 2G
Dec,
1889, p. 183.
13" 37'"
+ 3G°
16'
13" 42"'
+ 18°
3'
13" 43'"
+49°
55'
13"
56'"+
2°
7'
14"
8'"
+
19°
38'
14"
9"
+ 52°
22'
14" 10"'
+ 19°
49'
14" 12"
+ 51°
55'
14" 19"
+ 54°
21'
14" 22"'
47
—
— Eight Ascension
Declination 18«0,
1880.
14" 35"
—
48
+ 14°
15'
The primary
^ Bootis (2 1865).
nearer 4 mag., of the
can distinguish
first class
1883 was
companions,
3.5 mag., has two
at present so close to the
is
the
primary that only instruments
According to Pcrrotin, the distance in
it.
0.6", the position angle,
297
The
'.
farther
companion
at
is
distance 90", position angle 27°.
14h 40n.
+ 27°
35'
Bootis (S 1877), one of the most beautiful of the double
E
primary
The
stars.
2.5 mag., and yellow, the companion 6 mag.,
is
The
tance 2.9".
and blue. and their contrast has a pretty
colours are very decided,
Dis-
effect. 141.
44m
14h 46°.
15°
+
33'
Librae, 2.5 mag., with a companion 5 mag., distance 230".
a.
? Bootis
19° 36'
The
mag.
(S 1888), 4.5 mag., and yellowish, with a red companion 6.5
distance of this latter
3.9", while in 18'29
it
The
also rapidly changing.
I4h 4()m
+
39, Bootis (S
49° 12'
The primary
U"
50™
— 20°
is
1890), a double star 6 and 6.5
d
was
it
position angle is
mag.,
distance
3.6".
=
The primary
in Libra, a remarkable multiple star.
The
rest are all very faint.
(1878), gives the following measurements
AB
The
period of revolution seems to be 130 years.
6 mag., one companion [B], 7.5 mag.
ham
In 1882
rapidly decreasing.
white, the companion reddish.
Anonyma
52'
is
was, according to Struve 7.2".
15.1" p
= 290°
ACd=120.6"p =
322°
A D d=
171.0°
52.5" p
=
:
=
69.4" p
=
52.5°.
A F d=
105.5" p
=
166..5°.
AE
d
is
Burn-
The primary and the more brilliant companion compose a system with very decided proper motion. The other stars do not really, but only appear to, belong to 14" 55"
8°
Librae, variable and belongs to the Algol type.
S
2' its
it.
At maximum
only occupy 12 hours.
14" SG"
+
54°
0"'
+
48°
is
5, at
of brilliancy
minimum
4029, Nebula in Draco, irregular, faint but large.
23'
W. 15"
the star
Schmidt recognised
The changes
Period 2 days 7" 21.3".
variability in 1859.
6 mag.
Discovered
hy
Herschel, 5 May, 1788.
8'
44, Bootis (2 1909), a yellowish star 5 mag., with a blueish
6 mag., distance 5".
Both primary and companion seem
to
companion
be variable to a
[Said to be a mutually occulting pair, with a period of 261
slight degree.
years.]
— 19°
20'
;
Librae, a star 4.5 mag., with a companion 9 mag., d=57", p=110°.
Burnham found
the companion itself to be double, consisting
of two
stars
of 10 mag., distance 1.9".
15"
?"
+
S
19° 44'
1919, Bootis, 6.5 mag., and somewhat yellowish, with a white com-
panion 7 mag., distance 25". 15" lO"
15" 11"
+
+
?8°
33°
1
43'
p = 4C'
192G, Bootis, 0.5 mag., with a faint companion 9
259°.
A difficult
double
mag., d=1.4",
star.
Bootis, 3 mag., and white.
At
distance 105",
mag., whose position has not changed for 50 years.
is
a companion 7.5
— Right
49.
—
Declination
Aso^n.sion
1880.
1880.
+
15" 12"'
2° 31'
Observed by Messier in 1764, and
4083, Star Cluster in Serpens.
described as a beautiful, circular nebula 3' in diameter. clear weather
it
Kirch, in 1702, was the
first
to discover this nebula.
"In
Messier says,
can be seen very well with an ordinary telescope of
1' focus."
Messier could find
no trace of stars. Nevertheless, an average telescope shows that it is a cluster of stars and no nebula. Ilerschel, with his 40-foot reflector, could distinguish over 200 stars, though towards the centre they were so densely in
it
placed that
+
15" IS"
2°
13
5,
was impossible
Serpentis (2 1930).
= 10.6",
d
it
to resolve them.
Rosse says the cluster
is
diameter, the stars ranging from 12 to 15 mag.
7' to 8' in
p=:40.8^, the
companion 10 mag.,
5 mag., with a faint position
which does not seem
of
to
alter.
Struve, in 1836, believed the primary to be itself double, but this view has
not been since corroborated.
+
15" IS"
10° 49' p
+
15" 13"°
=
2
6.5 mag., with a companion 7.5 mag., d=13.5'', change of position has been noticed in last 50 years.
1931, Serpentis.
No
173°.
2 1932, Coronae.
27° 17'
6 mag.
both white.
;
The primary Distance,
is
5.5 mag.,
and has a companion
according to Engelmann,
1883, 1.2",
position angle 308°.
+
15" 13"
32°
U
5'
A
Coronae.
Winnecke
in
1863.
variable star
At
Period 3 days 10" 51.2". increase 5.2".
15" 14"
— 19°
S
57'
8
+
mag., at
S
14° 45'
of
the Algol type,
The decrease
brilliancy at
maximum
minimum under 12 mag.
recognised
minimum
mag., at
7.6
in brilliancy occupies
The changes
at
S
31° 48'
1860.
+
15" 18"
30° 43'
4.5'',
the
maximum
only
Discovered by Borreily in 1872.
A
Serpentis.
reddish star, noted by Laiande in 1794 as of 8 mag.,
was not recognised till 1828. At maximum under 12 mag. Period 361 days.
+
by
mag.
of brilliancy are very
but which could no longer be found by Harding in 1807.
15" 17"
8.8
varies somewhat.
Librae, variable, slightly reddish in colour,
irregular.
15" 16"
The
maximum
it is
7
Its variability
— 8 mag., at minimum
Coronae, of a reddish-yellow, recognised as variable by Hcncke ia Maximum 8, minimum 12 mag. Period 361 days.
Coronae (2 1937). A yellow star of 5.2 mag., with a golden it is extremely close to the primary, the coloured companion 5.7 mag distance (Engelmann, 1884) being only 0.6". 7)
;
+
15" 20"
37° 48'
IX.
7
Bootis.
A
yellow-greenish star 4 mag., with a companion
mag., distance 108", position angle 172-.
This latter
is
(pi,-)
itself double,
but, at present, can be divided only with a very powerful telescope.
15" 29" ^
+
10°
d 15" 32"
—
Serpentis (s 1954), yellowish, 3.5 mag., with a companion 4 mag.,
57'
8° 24
=
3.5",
2
p
= 190°.
1962, Librae, two stars 6 mag., distance 12".
— Eight Ascension
Declination 1880.
1880.
15^ 34"
+
36° 38'
IS*- 35""
37°
16^ 36-"
+ +
15" 37-"
+
26° 41'
IS''
38"
2'
80° 50'
50
— Eight Ascension
Declination 1880.
1880.
16"
l"
—
51
+
2
13° 39'
2007, Herculis, a double
star,
6.5 mag. and 7.5 mag.
;
distance
32".
16"
3"
+
17^ 22'
Herculis (S 2010), a yellowish star with a somewhat reddish com-
X
panion, G mag., distance 30".
16"
5°
— 19°
9'
Scorpionis, an easily observed double
V
40.5"
Cincinnati in 1846, found that the companion of 2 stars of 6.5
mag.
at distance 1.8".
Lastly
S"
+
13°
double, and consists
Buruham
1874 divided
in
only 0.8".
is
Primary 6.5 mag., companion 6.7 mag.,
49 Serpentis (S 2021).
51'
Mitchell, however, at
itself
is
the primary also into two stars, but the distance
16"
4 and 7 mag., distance
star,
thus observed by both Herschcl and South.
;
distance 3.7".
16" 10"
+
34° 10'
T
Coronae (2 2032), 5 mag., yellowish with a blueish companion, 6 mag., 88", besides a 54", p There is also a star 10 mag., d
=
distance 3.7". faint star,
4.9',
p
=
=
48.9°.
4173, Star Cluster in Scorpio, discovered by Messier in 1781, and
22° 41'
16" 10">
d
=
described as a circular nebula, 2' in diameter, with brilliant centre, like the
nucleus of a comet.
Later on Herschel, with the aid of his great telescope,
the stars in which are saw a star of 6.5 mag. in exceedingly dense. On 21 May, 1860, Auwers the cluster which had not been visible there before, and this observation
found that the object was in reality a star
was confirmed a few days
later
cluster,
The
by Pogson.
star
was already decreas-
and by the middle of June, 1860, was no longer visible. Near it are two variable stars R and S. The former, discovered by Chacornac in 1853, is ing,
maximum, being only 9 mag., and at minimum is almost under 13 mag. The change of brilliancy occupies 223 days. The latter {S) varies
faint at
between 9 and 13 mag.
Period only 177 days.
Neither star
is
of any
particular colour.
16" 12"
+
29° 29'
V
Coronae.
A star
of 5.5 mag., with a
companion of 9 mag., and three
other very faint companions.
Burnham
AB AC BD A 16" 14°'
25° 18';
a
a
gives (1879) the following measurements
d
p
86.3"
22.4"
A
6 mag.
123.6"
52.3°
C
9
13.2"
222.7°
D
13
56.1"
29.-5°
Scorpionis.
3.5 mag.,
B
10 mag.
12
=
20.4",
dense cluster of very small
stars,
with a companion 8.5 mag.
;
d
273\ 16" 16"
26°
14'
4183,
Nebula in Scorpio.
A
and 1| degrees to the west ot it. Observed Messier saw the cluster in 1764, and list
almost on the parallel of Antares,
by Lacaille, and included in his remarks that it is 2i minutes In diameter, and looks like a patch of nebula W. Herschel (In 1783) resolved the whole in a telescope of low power. ;
into stars with a 10-foot reflector.
— Right Ascension
Declination 1880.
1880.
+ 16'' 18"'
19° 26'
— 23°
7 Herculis, 3.5 mag., with a companion 8 mag., distance 38".
10'
Ophiuchi, a star of 5 mag., whicli
§
+
U Herculis,
19° 10' it
recognised as variable by
sometimes reaches 6.5 mag., at
degree
apparently to a slight
is
=
companion 7.5 mag., d
variable, with a le,^ 20""
52
3.7",
p = 358°.
Hencke
minimum
it
in 1860.
At maximum
under 11 mag.
is
Period
nearly 408 days. Ki'' 22"'
— 26°
10'
a Scorpionis (Ant ares), a brilliant star 1 mag., with a companion 7.5
mag., d at
=
3",
p
=
The companion was
274°.
Borne and Cincinnati
in
1849.
discovered simultaneously
when
Biirg at Vienna, 13 April, 1819,
Antares was eclipsed by the moon, and when Antares should have come disk, saw a star of 6.5 mag., which, 5 seconds seemed suddenly to attain the same brilliancy as Antares. He at once came to the conclusion that Antares was a double star. [Its
from behind the moon's later,
spectrum belongs 16'' 22-"
+
61° 58'
to
99, Draconls
Group
II.]
(2 2054), 5.5 mag., with a companion 7 mag.,
distance
only 1". 2gh 22""
+
61° 47'
7)
d
Draconls, a star of 2.8 mag., yellow, with a faint companion 10 mag.,
= 4.8", p =:
Burnham has
144°.
seen several other very minute stars
in the vicinity.
+
42°
9'
30,
(/
Herculis, recognised as variable by Baxendell in
At maximum
changes of brilliancy are very irregular.
minimum 16'' 25'"
+
2° 15'
The
1857.
the star
and at
is 5,
6 mag.
A
X Ophiuchi (2 2055). yellowish star of 4 mag., with a blueish companion 5.5 mag. The distance, which is increasing, was in 1884 V6", :
position angle, 43^. IG"- 26"'
— 12°
47'
An
4211, Star Cluster in Ophiuchus. Discovered by
stars.
W.
Ilerschel on 12
very beautiful, rich, and dense cluster,
5'
stars are collected with gradually increasing
Five 16'' 33"'
+
53° 10'
brilliant stars are to be seen
IG, 17,
extensive
of
cluster
round the
Draconis (2 2078), appears,
density towards
the centre.
cluster.
to the
naked eye,
a star of
like
The one
4.5 mag., in reality 2 brilliant stars of 5 mag., at distance 90".
which follows 16" 35"
+
4°
26'
))i
+ 49°
10'
+ 31°
49'
two
stars of
mag.
In
6 mag., at distance 69".
42, Herculis (2 2082), a star of 5 mag., with a
mag., d
16" 37"
double, having a companion G mag., at distance 3.7".
Herculis appears, to the naked eye, like a star of 6
reality it is
IGi-SS"
is
small
May, 1793, and described as a to 6' in diameter, in which the
faint
companion 11
= 22.4", p = 92°.
^ Herculis (2 2084), a brilliant white star of 2.G mag., with a
panion 6.5 mag.,
d=
1.4",
p=
114° (1880),
W.
the companion in July, 1782, but, later on, could no longer see
next observed in 1826 with the Dorpat refractor. of revolution seems to be only
36
years.
com-
Herschel discovered it.
It
was
The companion's period
—
53 Right Ascension
Declination 1880.
1880.
IQh 37m
+ 36^
41'
A magnificent cluster
4230, Star Cluster in Hercules. clear night, with the
who
discovered
that
it
it
naked
eye, as a light cloud,
as
on a
visible
remarked by Halley, in 1764, and says,
Messier observed this object
in 1714.
can be seen with a 1-foot telescope as a starless nebula,
circular, brighter at the centre.
Its
diameter
brilliant,
estimated by Messier to be
is
and the same astronomer remarks that the nebula is situated near two 8 mag., of which one is above, the other beneath it. A 4-inch refractor will resolve the nebula into stars, and Secchi, with his 9-inch 6',
stars of
found the stars
refractor,
Their number
is
to
[The great
among them.
Observatory has thoroughly resolved
24°
4234, Nebula in Hercules.
1'
diameter.
Lick
36-in. refractor of the
the central glow of nebulosity
into
Ed.]
separate points.
+
in
probably 5,000 to 6,000, and Rosse has noticed a remark-
able spiral grouping
lei-so-"
8'
be distributed over a space
A blueish,
diameter, and ill-defined at the edges.
Its
planetary nebula, circular,
8'
iu
spectrum shows the nebula
to
be
composed of incandescent gas, being characterised by the three bright lines, Elsewhere the spectrum is dull and of which the first is the most brilliant. continuous. Webb describes the appearance of this nebula by saying that it
16" 41'°
—
1°
43'
looks like a star which has not been properly focussed in the telescope.
4238, Star Cluster in Ophiuchus. Discovered by Messier in 1769, and described as a faint, circular, starless nebula, 3' in diameter, near which there
In 1783, Herschel's
a star of 9 mag.
is
into stars
showing a cluster of
7' to 8' in
nebula
reflector resolved the
diameter, at the centre of which
the stars are very densely collected. 16i'41»'
+
2°
17'
19,
p 16" 41-"
+
35°
=
2
52'
p IQb 44m _^ 470 44'
Ophiuchi (2 2096), 6 mag., with a companion 9 mag., d
=
2101, Herculis, a star of 6 mag.,with a companion 9 mag., d
4244, Nebula in Hercules, a large, round but
stars of 6
+
36°
8'
leMe^'n-
15°
9'
22.2",
=
4.2",
57°.
discovered by
16" 44"
=
93°.
2
W.
Herschel 12 May, 1787.
planetary nebula,
faint,
It forms
a triangle with two
mag.
2104, Herculis, a pretty, double
star, 6.5
S Herculis, of a clear red colour and variable, discovered at Bonn At maximum it is 6 mag., sometimes only 7 mag., at minimum
1856.
decreases to 11.5 and 12 mag.
16h5im„
33
6".
and 8.5 mag., distance
54'
4256, Star Cluster in Ophiuchus.
Discovered by Messier, 29 May,
faint, circular, starless nebula,
cerned without
with a 3-foot telescope.
first to
it
Period 303 days.
1763, and described as a difftculty
in
resolve this nebula into a densely
crowded
which cannot be
W.
dis-
Herschel was the
star cluster.
These
stars
are partially visible in a 4-in. refractor.
16" 53-"
— 12°
ova Ophiuchi,
42'
1848.
On 28
April of
this
year.
4.5 mag., of a yellowish-red colour in this place where
been
visible.
began
The
to decrease
star
and
maintained this brilliancy
is
now under 12 mag.
till
it
Hind saw a star had never before 10
May
;
it
then
51 Right Ascension
Declination 1880.
1880.
16" 54"
29° 56'
A beautiful
4261, Star Cluster in Scorpio. Messier, 7 June, 1771, and described by
bim
nebula, discovered by
as like a comet.
The nebula
was resolved into stars by W. beyond the reach of ordinary refractors.
It is
Herschel, with bis 20-foot telescope.
4264, Star Cluster in Ophiuchus, discovered by Messier, 5 June, 1764, catalogued by him as a starless nebula, situated oq the parallel of
16" 56"
Antares,
3' in
diameter, and of which a good view can be obtained with 31-
foot telescope.
16" 58"
— 24°
36'
2
1'
— 22°
to be a globular star cluster.
it
4268, Star Cluster in Ophiuchus, discovered by "W. Herschel, 2' to in diameter, brilliant and more condensed towards the centre, easily
According
resolved.
16" 59"
W. Herschel, in 1784, proved
32'
W.
to
Ophiuchus, discovered by W. Herschel, globular, fairly brilliant, round, somewhat condensed
4269, Star Cluster
21 May, 1784.
It
Herschel, the stars are of a faint red colour.
is
in
towards the centre, and easily resolved. 17h
lmi_150
M
5g/
At
Ophiuchi, reddish, and recogaised as variable by Pogson in 1853. maximum it is not more than 7.5 mag., at minimum it is under 12.
Period 302 days. 17"
3""
17"
3"
+
54°
38'
— 26°
25'
Draconis (S 2130), 4.5 mag., with a companion 5 mag., distance
IM
2.7".
8°
— 26°
25'
globular cluster, fairly bril-
and round, with a sudden increase
centre, can be resolved into
17"
A
4270, Star Cluster in Ophiuchus. liant, large
It
stars.
is
mag., and of a golden
36, Ophiuchi, 5
in brightness towards the
followed by a faint nebula. yellow, with a
companion
6 mag., distance 4.7", position angle 211° (1870). 17"
9™
+
14° 32'
cc
Herculis (S 2140), a variable star of a yellowish-red colour, 3 mag., The changes in brilliancy are
recognised as such by Herschel in 1795.
At minimum
not very great, but very irregular. a companion G mag., distance
17" 10"
+
24° 59'
it is
over 4 mag.
It
has
4.7".
S Herculis (2 3127), 3 mag., of a greenish-white, with a blueish com[Spectrum of Group beautiful object. panion 8 mag., distance 19.5".
A
IV. type.] 17" 10"
+
1°
U
21'
1881.
The
Ophiuchi, a remarkable variable It is generally of 6.1 mag.,
period
is
17" 11"
17" 12"
— 24° — 18°
at
discovered by Sawyer in
minimum
In
known
this respect it is the
at present.
The
most interesting of
the
type.
39, Ophiuchi, 6 mag., with a
9'
companion 7.5 mag., distance 11".
4287, Star Cluster in Ophiuchus, discerned by
25'
resolved
+
all
star naturally belongs to the Algol
scribed as a faint, circular nebula 3' in diameter.
17" 13"
decreases to 6.8 mag.
only 20" 8", and the change of brilliancy occupies the short
space of 4 hours. variable stars
and
star,
it
into stars, with a 20-foot reflector.
4294, Star Cluster in Hercules.
43° 16'
Messier, and de-
In 1784, Herschel
Described by Messier as a starless
nebula, with a brilliant centre, easily discerned with a small telescope.
A
refractor of
moderate power will resolve the nebula into stars which
are distributed over an area 8' in diameter.
solved even in Hosse's telescope.
The
centre could not be re-
55 Right Ascension
Declination 1880.
1880.
17" 13°
17" 14°' 17" 17-°
17" 20™
+
33°
— 12° — 17°
14'
43' 42'
—
— Eight Ascension
Declination 1880.
1880.
17" 40"
— 27°
X
47'
Sagittarii, recognised
2
17" 42"" -K17° 46'
+
+
72° 12'
17" 47""
+
23°
The
(1878.)
Herculis (2 2220), 8.5 mag. and yellowish, with a companion 9.5 244°. mag., d 31", p In 1856 Clark discovered that the companion
=
W
Schmidt, in 1866.
(U.
=
itself is double, consisting of
17"
J.
2215, Herculis, 6.5 mag., with a companion 8 mag., distance only
0.7", angle 301°.
27° 48'
by
as variable
between 4 and 6 mag., within a period of 7 days.
star varies
17" 42-"
56
2 stars of 11 mag., which were then at dis-
tance 1.8".
This distance has since steadily decreased, and
about 0.5".
A
very
is
now only
difficult object.
Draconis (S 2241), a star of 4.5 mag., with a companion 5 mag., distance 31". Recognised as double by Flamsteed. 4/
4343, Nebula in Hercules, small, round, rather brighter towards the
6'
centre, with a small nucleus.
19°
17" 50"
0'
A
4346, Star Cluster in Ophiuchus. Messier, 20 June, 1764.
The
nearly 80 stars of 9 to 12 mag. the whole
field
beautiful cluster discovered
and
Its diameter is 15', stars
by
in this space there are
seem
to be scattered over
of vision, the lowest magnifying power must, therefore, be
used.
17" 64'°
+
51° 30'
7 Draconis, 2.5 mag., with a very faint companion 11 mag., d =z 125",
p=116°. d 17" y.S™ 4-
2° 56'
— 23°
2'
saw, besides, an exceedingly faint star, 13.5 mag.,
152°.
67, Ophiuchi.
8 mag. 17" 56™
Burnham
= 21", p =
This star 4 mag. has, at distance 55", a red companion
Tlie contrast of colour in these stars is pretty.
A
4355, Nebula in Sagittarius.
group containing several nebulte.
Erroneously described by Messier as a star cluster.
In 1874, Herschol
saw 3
Herschol found this
nebula?, with a double star in their midst.
star to be triple.
J.
Either the star or the nebulas seems to rapidly change
its position.
17" SB"
— 30°
2'
4359, Star Cluster in densed towards the centre.
17" 57'"
+
21° 35'
— 24°
stars are exceedingly small.
95, Herculis (2 2264), 5 mag.,
5.5 mag., distance 6".
17" 57"
Sagittarius, globular, fairly brilliant, con-
The
23'
somewhat
greenish, with a
4361, Star Cluster in Sagittar
s,
a very beautiful object discovered
by Messier in 1764, and described by him as a star consists of several to
17" 57™
—
8° 10'
— 22°
31'
ncbuloj, with a triple star
cluster.
It really
and numerous others near
it.
T Ophiuchi (2 2262), 5 mag., with a blueish companion 9 mag., d=i: 100", p
17" 58"
companion
[Concerted changes of colour are recorded of these.]
=
127°.
The primary,
double star.
Schiaparelli in
of revolution
is
as discovered
1882 found d
—
by
W.
1.9",
Herschel,
p=252°.
is
itself
a
The period
nearly 200 years.
4367, Star Cluster in Sagittarius, discovered by Messier in 1764,
and a beautiful
object.
The
stars are of
they are mingled with nebula;.
8 mag. and under.
Messier says
— Right Ascension
Declination 1880.
1880.
17" 57-°
—
67
— 29°
W Sagittarii,
35'
maximum
it is
5,
recognised as variable at
by
J.
The
raiuimum 6.5 mag.
At
Schmidt in 1866.
period seems to be from
7 to 8 days.
17" 59"
+
66° 38'
4373, Nebula in Draco.
He
describes
it
Discovered by Hcrschel, 15
A
diameter, one angle very ill-defined.
Huggins found the 3rd
of bright lines.
other hand, declares refractor has 17'' 59'^
+
2° 33'
it
The nebula can
this
spectrum
It gives a beautiful
Vogel, on the
line the faintest.
[The Lick
to be quite as brilliant as the second.
shewn that
in
long and careful examination
reveals a brilliant, well-defined centre, round in shape.
be seen very well with a Hl-inch refractor.
Feb., 1786. disk 35"
as a planetary nebula of groat brilliancy,
nebula has a helical form.]
Ophiuchi (2 2272), 4 mag., and yellow, with a red companion, 6 mag. Since Herschel's time, this companion Period has completed more than a full revolution round the primary. The parallax is of revolution, 95 years [Mr. Gore niiikes it 88 years]. 70,
distance (Schiaparelli, 1882), 2.3".
0.16", the distance
from the earth
— 1,300,000
radii of the earth's orbit.
The mean distance of the companion from its primary is 4.300 million kilometers, or nearly 30 radii of the earth's orbit [said recently to range from 14 to 42 radii], and the whole mass of the system is equal to about three times that of our sun
18"
O"
+
18"
0-"
— 23°
18"
3""
18"
4"'
+ +
S
48° 29'
26°
2277, Herculis, 6 mag., with a companion 8 mag., at distance 27".
4376, Star Cluster in Sagittarius, large and fairly rich.
14'
100, Herculis (2 2280), two stars 6 mag,, distance 14".
5'
3° 58'
73,
Ophiuchi (S 2281), a
difficult
only
+
31°
a variable star, discovered at
liancy ranges from 7 to 12 mag.
18"
5-°
+
1
16° 27'
it.
la 1876
it
was
1".
T Herculis,
0'
The
double star 6 and 7.5 mag.
distance seems to Lave decreased since Struve observed
It
is
Bonn
in
of a deep red colour.
1857.
Its bril-
Period 165 days.
2289, Herculis, a star of 6 mag., with a companion 7 mag.
Dis-
tance, only 1.2".
18"
6'"
ISh
gm
21° 36'
^
4388, Star Cluster in Sagittarius, a fairly large and scattered cluster of stars, ranging from 9.5 to 11 mag. 4390, Nebula in Ophiuchus, fairly
6° 49'
brilliant, planetary.
Its
contains the three early recognised bright lines, of which the
most
brilliant,
the last (falling on
i^),
the faintest.
5'
/x
the
[Spectrum consists of
the thiee chief nebula lines, and a faint continuous spectrum.
21°
spectrum
first is
Huggins.]
Sagitarii, a quintuple star, primary 3.5 mag., and yellowish, has a
=
=
119°; another 10 mag., d =: 50" 25", p companion 10 mag., d companions seen by Burnham, are merely faint two 115°. The other p
=
points of light.
18"
9°
+
40, 41, Draconis (S 2308).
79° 59' like
a star of 5 mag.
They
Seen with the naked eye, these look
are really two stars 5.2 and 6 mag., dis-
tance 20".
18" 11-°
— 18°
28'
A rich star cluster, discovered 4397, Star Cluster in Sagittarius. 1|^ in diameter. Visible to the Nearly by Messier, 20 June, 176 i. naked eye as an offshoot of the Milky Way.
58 Right Ascension 1880.
18" 12"
Declination 1880.
13° 50'
— 17°
12'
18" Il-
— 16°
15'
ls" 17"
— 24°
56'
18'-
13"
18" 18"
—
— Right Ascension
Declination 1880.
1880.
IS"-
29°
50
— 24°
0'
4424, Star Cluster in Sagittarius, 1665.
common
cular and easily seen with a
18" 30°
—
33°
+
it,
catalogued
telescope of 3|'
stars.
the nebula into a star cluster.
Towards the middle the
diameter 8° 19'
This splendid
^
exhibited
indicate that
The
type.
and
of
mag., has near
1
star,
merely
it is
= 48", p = 156°,
of 9.5 mag., d
it
One
optical.
several
of them,
star for calculating
another of 9 mag.,
Winuecke and Burnham have also measured a very [In Nov., 1890, Mr. A. Fowler (13 mag.), d = 52", p = 292^ to the E..A. Society photographs of the spectrum of Vega which
150", p
faint star
is
rich,
Hcrschel, 16 June, 1784.
which was used by Struve and Briiunow as a comparison the parallax of Vega,
=
denser;
are
stars
Sobieski, large, fairly
W.
faint stars, but their connection with
d
cir-
sur-
is
Ilerschel's 10-foot telescope resolved
Scutum
Discovered by
Lyrae (Vega).
a
It
8'.
4426, Star Cluster in
38° 40'
Iblc,
as
it
focus.
rounded by 5 irregularly placed
moderate density. IS*-
by Abraham
discovered
Messier could not distinguish any star in
40°.
it is
a spectroscopic double of the
i3
Auriga: and
The
principal lines are due to Hydrogen.
§
Ursae Majoris
separation of the
K
within a few hours, indicated a circular orbit, and a period of revolution
line,
of about 24.68 hours.
K
This duplication of the
line
has not (1891) been
confirmed by photographs taken by Pickering, Vogel and the Messrs. Henri.] 18" 35° 18" 39°
18" 40°
— — —
4° 52'
4429, Star Cluster in are
little
4482, Star Cluster
9° 31' 2' in
1°
5,
5'
p
+ 39°
=
33'
Sobieski, large and rich, but the stars points.
Scutum
in
Sobieski.
Discovered by
Messier,
diameter.
Aquilae, (S 2379), 6 mag., with a blueish companion 7.4 mag.,
There
distance 18.2".
18" 40°
Scutum
more than minute luminous
is
also a second
companion 11
=
d
mag.,
27.3",
145°. £
A
and 5 Lyrae.
very interesting pair of double
observed
stars, first
by Flamsteed, though with keen sight and under specially favourable cumstances
£
and S^Lyrae can be seen
according to Auwers, 1682, itself
is
as clearly separated.
The
208".
fact that
e
[From
seems to be slowly decreasing.
their
distance,
The
distance
8.045".
same year
common
is
Herschel
1863,
and 5 Lyrae.
of the two components from sis. according to Dembovvski, distance of both stars from 5 Lyrae was in the
cir-
each of these stars
double was verified by Christian Mayer, and in 1823 John
discovered three other very faint stars between
The
The
2.48",
and
proper motion,
these seem to constitute a physical system of vast dimension?.]
18" 41°
+
37° 29'
18" 41°
—
5° 50'
^ Lyrae, a star of 4 mag., with a
recognised by Flamsteed.
E
Scuti Sobieski.
change' of brilliancy 4.5 mag., though
8 mag. T.
18" 41°
+
20° 26'
The
+
60° 56'
is
it is
period
is
Recognised as variable by Pigott in 1795.
very irregular
;
often under o.o irregular.
maximum the star is mag., at miuimum it is 6, at
[The spectra seem, according
The
sometimes soincUrncs to the
Rev.
E. E>pin, also to vary considerably.] 110, Herculis, 4 mag., with a companion 11 mag., d
Burnham saw a S 2408, Draconis, still
18" 43°
companion 5.5 mag.; distance 44",
Struve, in 1882, d
fainter
companion, d
= 61", p = 92°.
= 45", p = 95°.
6 mag., with a companion 9 mag.
= 1.9",
p
=
259°.
According
to
—
GO Right Ascension
Declination I
1860.
1680.
J
6°
18" 4.5"
2.5'
Discovered by Kirch in Star Cluster in Scutum Sobieski. and described later by Messier as a cluster of small stars, only visible
4437, ll)81,
The
with a good instrument.
can be clearly seen with a 3i-inch
stars
Lamoiit and Helmert have taken the measurements of the
refractor.
whole cluster by Trigonometry. IB" 4G"
+ 33°
P Lyrae, a variable star with three companions, a pretty spectacle when
13'
The primary is The period
seen with the telescope.
mag., at
minimum
mag.
4.5
days 21" 51™, with a double
maximum
yellowish white, at
maximum and minimum.
3.5
12 [The spectrum of
of the change of brilliancy
The
this star consisting of bright lines is periodic in brightness.
is
variation
most marked, as Gothard shews, in the case of Da.] Of the companions, 149° a second, 8 mag., has the most brilliant is 7.4 mag., d 45.6, p 19°. 318° 86", p a third, 8.5 mag., d Finally, d G6", p is
=
=
=
=
Burnham has ]
8"
40"
+ 10°
—
8°
51'
;
seen a fourth very faint star
=
(11 mag.) d
4440, Star Cluster in Aquila, a beautiful object,
12'
= 46", p =
248°.
consisting of
stars
Vogel has measured 62 of them with the micrometer.
9 to 12 mag.
18" 4?"
;
=
4441, Nebula in Scutum Sobieski, brilliant, large and nearly circular, more condensed towards the centre. According to Herschel it is resolvable into stars.
30°
Asm 18" 48' li
4442, Nebula
37'
in
According
described as a faint nebula with a brilliant centre.
+ 32°
to
Herschel
a globular star cluster consisting of very minute stars.
it is
18" 49"
and
discovered by Messier in 1778,
Sagittarius,
4447, Nebula
53'
Lyra,
in
the
Discovered by Darquier,
nebula.
He
Lyrae.
describes
it
beautiful at
and
easily-observed
Toulouse, 1779, between
as very delicate, with well-defined
/3
Ring and y
boundaries, of
about the same size as Jupiter, and looking like a planet that
is
about to
become extinct. Messier describes it as a luminous cluster, apparently composed of small stars. It is, indeed, remarkable that this nebula, which appears like a disk, with a bright border, has a brilliancy wherein one fancies one can see twinkling star-points.
they have succeeded in resolving
it'into
Rosse and Bond maintain that
separate stars, but
its
spectrum
is
one
which indicate that it is really composed of incandescent gas. A minute star, of 10 mag., follows the nebula closely. [The 36-in. Refractor of the Lick Observatory shows three stars in the central space, See Nature, August 9, where Lord Rosse's drawing gives a blank field. 1888. The photographs taken at the Algiers Observatory in 1890 shew of bright lines
that the nebulosity spreads towards the centre, and that the
there
is
surrounded by three very feeble
the evidence as to elliptical.
18" 50"
+
4°
3'
6
+ 33°
49'
form {Nature, March
5,
+ 43°
47'
star
1891), pronounces the nebula
Ed.] with
a
somewhat
faint
at distance 21".
The primary, 6 mag., has a companion 6.5 Multiple Star in Lyra. 351 45", p Struve repeatedly observed this double star, mag., d but Burnham in 1879 was the first to discover that the primary is itself 126°. 1.7", p double, there being near it a small star of 10 mag., d
=
=
'.
=
18" 52">
central
Miss Gierke, summing up
Serpentis, a yellowish-white star 4 mag.,
companion 18" 50"
its
stars.
R
=
Lyrae, a variable star discovered by Baxendell in 1856, of a reddish The change of brilliancy is but slight, the star varying between colour. 4.3 and 4.6 within a period of 46 days.
— Right Ascension 1880.
18''
54™
18" 59'"
61
— Right Ascension
Declination 1880.
1880.
19" 37"'
+
39° 55'
19" 39""
+
19" 41"'
-f-
50° 15'
The
44° 50'
Cygni (S 2579), a greenish
5
seen by
W.
Ilerschel, 1783.
be distinguished,
till
50° 14'
drawing of 33° 27'
19" 43"
+
11° 31'
+
27°
12 mag.
star,
3 mag., with a companion 8 mag., the companion could no longer
Later,
was
According to Engelmann,
1.8", position angle, 321°.
it
out
looks like a star
W.
Herschel,
Sept., 1773.
Secchi has
of focus.
made a
this nebula.
17, Cygni (2 2580), a reddish star 5.6 mag., with ablueish companion 8 mag., distance 26".
Aquilae (S 2583), 6 mag., with a companion 7 mag., distance, which
TT
is
19" 43"
to
4514, Nebula in Cygnus, discovered by
In small telescopes
+
large and rich cluster, discovered
Struve saw it again in 1826.
the distance in 1883
19 42"
10
stars are of
16, Cygni, 2 stars of 6 mag., distance 37".
first
+
A
4511, Star Cluster in Cygnus.
by Harding in 1827.
19" 42"
—
62
at present gradually increasing, 1.6".
1'
At
Vulpeculae.
11,
this
spot there appeared in 1670
mag., which disappeared in the autumn of the same year
appeared as a star of 4 mag., but again vanished
and
now completely
is
invisible.
a star of 3
1671 it rewas again seen in 1672,
;
in
;
In 1852 Hind discovered a small star
which in 1861 had diminished to 12 mag., and which he It seemed to him somewhat held to be identical with the star of 1670. blurred as compared with other stars in its vicinity, and this impression of 10.5 mag.,
was shared by Talmage and Baxendell. 19" 44"
+
18° 51'
^ Sagittae
refractor,
d=8.7", p
+
8° 33'
a Aquilae, Altair.
(Vogel
;
= 312°.
found the "[jrimary to be
Burnham's measurements 19" 45'"
a greenish- white star, 5.6 mag., with a com-
(2 2585),
9 mag.,
panion
Class la).
are d
A
There
Clark, in 1875, with
itself
= 0.3",
double.
p=:
very
a 12-inch
difficult object.
158°.
brilliant star 1 mag., is
A
with a beautiful spectrum
a companion 10 mag., d
There are several fainter stars nearer to the primary.
—
152", p
—
322°.
Burnham saw
over
a dozen with bis great refractor. 19"
46"
+
32° 37'
X,
Cygni, a variable star of long period, with irregular variations in Its variability was discovered by Kirch in 1686. At maximum
brightness.
the star reaches 4 mag., at is
19" 46'"
+
minimum
it
diminishes to 13 mag.
The
period
about 400 days.
0° 42'
7)
it is
At maximum Aquilae, recognised as variable by Pigott in 1784. minimum 4.7 mag. The period of 7 days 4'' 14.2" is at present
3.5, at
slowly increasing. 19" 40'"
+
59°
7'
4517,
Star Cluster in Draco, a
fairly large bu'; not
very dense cluster,
containing stars of 7 mag. 19" 48"'
+
18° 29'
4520, Star Cluster in Sagitta, described by Messier as a faint nebula. beauit into a dense cluster of stars, 3' in diameter.
Herschel resolved
A
tiful object.
19" 49™
+
69° 58'
6
Draconis (2 2603), 5 mag., with a companion 7.6 mag., distance 2.8".
— Bight Ascension
Declination 1880.
1880.
19" 49"
+
6°
19" id-^
—
8° 32'
19" 53"
+
52°
19" 54°
+
22° 23'
19" SS""
19" or-"
19" 59""
20"
20"
0"
7'
7'
63
—
0-4
Right AsceDBioa
Declination 1880.
1880.
20'' 11"°
— 12°
20" 13"
+
20" IS-"
— 19°
20''137
+
20" 14-"
— 15°
20" 17-°
+
20" 19"
20" 28"
55'
37° 40'
30'
77° 21'
10'
19° 43'
—
65 Right AKcension
Declination 1880.
1880.
20'' 29'°
+
60° 16'
20'' 29'"
+
27° 54'
20'' 32-"
+
14°
11'
20'' 33-"
+
0°
4'
20" 34"'
+
15° 29'
20" SC"
+
31°
20" 40'°
20" 41'"
20" 41'"
20" 41-"
20" 42'°
20" 43"
20" 44"
20" 45"°
—
— Right Ascension 1880.
20" 47""
20' SO" 20''
SS"
20" se-
Declination 1880.
—12°
59'
CO
—
— Right Ascension
Declination 1880.
1880.
21"
5°
+
9°
7 Equulei, 5 mag., yellow, with a companion 6 mag., distance 366".
39'
The primary
2P
7"
+
45° 11'
21h
gm
+
67°
Burnham
T Cephei,
54'
the star
+
also
saw
a very faint star,
at d:=:2.1",
d=41", p=10°.
4645, Star Cluster in Cygnus, an extensive but not very rich cluster
A star of 7 mag.
of stars of 10 mag.
8-
double, having a small star 10 mag.
is itself
pzz: 274.5°.
21"
—
67
2
59° 29'
recognised as variable by
is 5.5, at
minimum
Wilson (1873)
it
on
its
edge.
Ceraski in 1879.
At maximum
Period 390 days.
9 mag.
The primary
2780, Cephei.
are white.
follows
the companion 7 mag., and both
is 6,
calculates,
d^
1.0",
No
p ^224.3°.
change
of position has been observed since the time of Struve.
2ih
gm
+
9°
31'
S
Equulei (S 2777), 5 mag. and yellowish, with a companion 10 In 1852 Otto Struve found that the primary
mag.
a companion 10.5 mag. near to
Burnham
it.
ABd= ACd=
0.35", p
=
29°.
22.7",
=
37.9°.
p
is itself
double, having
(1880) calculates
:
The primary can only be divided with a most powerful instrument. [The motion of the two is the quickest known. Burnham has shown that the period of 11 J years
2P
10"
+
is
too short.]
T Cygni, 4 mag., a difficult double star, discovered by Clark in 1874.
37° 32'
According
to
Burnham, the companion
another very faint companion, d
21" 13-"
+
d 21" 16-"
+ 58°
=
15, p
2
7'
16",
=
p
= 1", p =
150°.
Hall saw
260°.
Cygni, a star of 4.5 mag., with two faint companions of 10 mag.,
V
34° 23'
=
at d
is
=
219
',
=
and d
21.-5",
p
=
178°.
2790, Cephei, 6 mag. and red, with a companion 10.5 mag., d=4.5",
p =46.-5°.
21" 17"
+
19° 17'
Pegasi, a yellow star 4"5 mag., with a companion 8.9 mag., d==37",
1
p = 301°. 21" 17"
+
G°
18'
Equulei, 5 mag., with a companion 10.5 mag., d
/3
and, in first
addition, a second companion 11 mag., d
companion
Uurnham
+
=
d
32", p
=
=
86", p
67", p
=
= 309°
276°.
The
mag., distance 6.5". 260°.
This latter
is
very powerful telescope only.
4670, Star Cluster in Pegasus, recognised as a nebula by Maraldi
11° 39'
Herschel resolved
as far
back as 1745.
With
a 5-inch refractor
be resolved. to
21" 27"
a double star of 10 and 11
also found a very faint star,
visible in a
21" 24"
is itself
=
12 mag.
At
it
be
3'
—
of moderate brilliancy
eastern edge.
into a globular cluster of stars.
the edges are scattered a large
Diameter
number
of stars of from 11
4'.
4678, Nebula in Aquarius.
1° 21'
it
has this appearance, though the centre cannot
and
In the average telescope this appears circular,
with a small
faint star
at
to
the
Discoverel in 1746 by Maraldi, was resolved into stars by
Herschel.
ojh 27"
+
70°
2'
ii
Cephei (S 2806), a greenish-white
8mag., d=13.6", p
= 250\
star of 3 mag.,
with a companion
Right Ascc-nsion
Declination 1880.
1880.
21" 28°'
+
47° 54'
Star Cluster
4G81,
Cygnus, a
in
and beautiful
largo
cluster,
discovered by Messier in 17G4, visible in a small telescope.
21" 32""
+
6°
Pegasi, a star of G mag., with a companion 7.5 mag., d
3,
5'
=
349°. No change of position has been noticed since p observed by "W. Herschel.
21" 34™
— 23°
it
= 39",
was
first
4687, Star Cluster in Capricornus, described by Messier as a strip
43'
of starless nebula visible only with difficulty.
It can be resolved into stars
Herschel saw the stars with a 10-foot reflecting
with a 5-inch refractor. telescope.
21" 35"
+
56°
2
54'
B
6 mag.,
AB
follows:
p 21" 37"
+
78°
5'
=
+
42°
8,
D
Wilson and Seabroke's
9.
= 122.3°, d = = 50".
p
174.2°, d
11.7"
p= 339.9°,
C
as variable
and
at
A is
calculations (1873) are as
d
= 19.8"; A D
by Hencke in 1855.
minimum
At
diminishes to 12
it
Period about 485 days.
Nova Cygni,
18'
A
;
S Cephei, a red star recognised maximum it never exceeds 7.5 mag., mag.
21" 37"
C
8,
The primary
Triple, with a distant companion.
2816, Cephei.
3 mag.
It
was
and in was it
place,
year
discovered 24 Nov., 1876, by Schmidt as a yellow star of
was taking was only 10.5 mag. in the following mag., and inwible except in the most
at once apparent
Sept., 1877, the
— 14
13
only
that a decrease of brilliancy
star
;
The spectrum
powerful telescopes.
at
the
time of greatest
brilliancy
contained eight bright lines indicating the presence of hydrogen, natrium
and magnesium. Finally these were reduced to a single bright line accompanied by only the traces of a continuous spectrum, and bearing a close resemblance to the
spectrum of a planetary nebula.
At
the Dunecht
Observatory a sketch was made, by means of a 15-inch refractor, of the surroundings of
21" 38"
+
9°
first
seen by
W.
measurements
within a radius of
The primary
Pegasi.
£
20'
Nova
the companion 8 mag.
=
138.5", p
= 323°.
This latter was
South (1825) gives the following
Herschel, 20 Nov., 1782.
d
:
is 2.3,
7.5'.
According to Schmidt and Seidel
the primary seems to be variable in a slight degree.
21" 39"
+
28° 12'
/w-
Cygni, (S 2822), a star of 4.5 mag., with a beautiful blue companion
= 208.7", p = = 264°.
5 mag., distance 3.8", besides a companion of 7 mag., d
Burnham saw 21" 39"
+
25°
G'
another star of 11.5 mag., d
X Pegasi, (2 2824), a star of
=
=
308°. p double, but the companion
mag., d
11",
=
35.5," p
57°.
4 mag., with a very faint companion 11 discovered that the primary is itself
Burnham is
only at distance 0.27".
The two
stars differ
about half a magnitude in brilliancy. 21" 40"
+
58° 14'
//(.
Cephei, cf a deep red colour, and varies between 4 and 5 mag.
not yet ascertained.
The
star has
;
period
two companions, but they are both very
faint.
21" 43"
+
G5°
12'
4709, Star Cluster in Cepheus, fairly large, rich in
massed together.
In largo telescopes a very beautiful object.
stars,
densely
— Declination 1880.
21" 48-"
21" 55"
22"
O-"
22"
1"
22"
5""
22"
69
—
— Right Ascension
—
70
Declination 1880.
1880.
+
22'' 31-°
33° 48'
4816, Nebula in Pegasus,
bright and large, with a sudden
fairly
increase of brilliancy towards the centre.
+
22'' 37"'
29° 86'
Pegasi, 3 mag., with a companion 10.5 mag., observed by Herschel
r,
=
and South, d
— 14°
22" 41°'
41'
[Spectrum continuous.]
90", p
= 339°. companion 9 mag.,
of 6 mag., with a
69, Aquarii (2 2943), a star
d=28", p = 115°.
+
22" 41'"
11° 34'
d 22" 43°"
— 14°
18'
22" SI""
— 20°
59'
=
= 12",
=
128", p
mag., with a companion 10.5
5
Pegasi,
?
Herschel), d
Buinham
p=:113°.
mag. and
S
a star of a
Aquarii,
red, with a
+
22" 58""
27° 26'
companion 5.5 mag., distance 180".
deep reddish-yellow colour, recognised as
At maximum
variable by Argelander in 1853.
12 mag.
mag. (observed by J. saw a star of 11 mag.,
21.8°.
T Aquarii, 4
mum
also
it is
only 8 mag., at mini-
Period 280 days.
The primary is variable, at maximum it is 2.2, at minimum The changes of brilliancy are somewhat irregular, and are accompanied (or caused) by a change in the reddish tint of the star. The companion, which was observed by J. Herschel, is faint and in 1878 the ^ Pegasi.
2.7
mag.
;
measurements were d = 99", p = 208°. 23"
4"'
'+74°
44'
Cephei, observed by J. Herschel as a double
TT
triple
by the refractor at Pulkowa
central star
is
The
5 mag.
panion, which was
first
9°
44'
seen in the great refractor at
According
deep yellow colour. 49.6".
— 14°
23" 14"' i
+
6'
16'
/S
is
+
60°
56'
star,
recognised as such even by
Struve the primary is
is
4.5 mag., and of a
mag. and
8.5
The primary (deep The position
Ceptiei (S 8001).
it is
23" lO"
The The nearer comPulkowa is, accord-
blue.
Distance
94, Aquarii (2998), recognised as a double star by W. Herschel, 20 Aug., 1781. The primary is G mag. and yellowish-white, the companion The companion's change of position is slight, but the 7 mag. and blue. mutual motions of the stars show a physical relation between them.
67° 27'
8°
to
The companion
(deep blue) 7.8
change pretty rapidly.
+
be
,
panion
23" U"-
to
1..5".
Aquarii, an easily- observed double
J/
Chr. Mayer.
23" 13"
the primary being
but found
itself double.
farther companion 11 mag.
ing to Struvo, 8.9 mag., distance
23" 10"'
;
star,
star,
5.5 mag., the com-
of a yellowish-red colour.
occasionally 7 mag., but faint, at
regard to
is
of the companion seems to
Distance 27", position angle 192°.
Pegasi, a variable
known with
yellow)
mag.
its
minimum
it is
At maximum
only 12 mag.
Nothing
period.
4957, Star Cluster in Cepheus. Discovered by Messier 7 Sept., 1774, and described as follows: "A cluster of very small stars mingled with nebula.
Can only be seen with an achromatic
telescope."
The
cluster
is
preceded by two stars of 7 and 8 mag., and followed by one brilliaut It contains one star of an orange colour. star.
— Eight Ascension
Declination 1880.
1880.
23" 21"
—
71
+
41° 52'
4964, Nebula in Andromeda, a small,
W.
15" in diameter, discovered by nised in
brilliant,
planetary nebula
Herschel, 6 Oct., 1784.
Lassell recog-
a nucleus with two oval rings, Rosse a spiral arrangement.
it
The
spectrum (according to Huggins) contains four bright lines indicating a
[One of these
gaseous nature.
near
lines,
W.
L. 470, occurs only in this
and the Orion Nebula.] 23" oS-
— 15°
Aquarii, a star of a somewhat deep red colour, recognised as variable
li
by Harding in 1811. It varies from 6 somewhat under 390 days. 23" 40"
— 19°
23" 46""
+
21'
=
p
15° 39'
56°
A
5031, Star Cluster in Cassiopeia.
3'
brilliant,
+
=
50° 43'
cluster of coarsely scattered stars
and upwards.
1783, between
23" 52"'
Period apparently
138'^
5023, Star Cluster in Pegasus. of 10 mag.
+
11 mag.
107, Aquarii, 5.6 mag., with a blueish-white companion 7 mag., d 5.2",
23" 51"
to
§
and
<y
and the whole object
li Cassiopeiae,
stars
are numerous but
not
a beautiful sight in a powerful telescope.
is
recognised as variable by Pogson in 1853, of a deep
At maximum
red colour.
Discovered by Caroline Herschel in
The
Cassiopeia.
it is
5.5, at
The
minimum 12 mag.
period
is
about 426 days and seems to be decreasing. 23" 53"
+
55°
cr
Cassiopeiae (2 3049). Discovered to be double by W. Herschel, 31 The primary is 5.4 mag. and greenish, the companion 7.5
Aug., 1780.
and deep blue position of the
23" 53-"
+
33°
4'
23" 56™
+ 26°
27'
2
30°, also
the
Editorial Note.-
so-called "
A
— In
Law
Newton's
recent
=
326°.
= =
stars,
=
it,
distance only
0.7", position
This companion cannot be discerned save in an instrument
" The Extension of the it is
Law
of Gravitation to Stellar Systems," by
shown that there
Groombridge, 1830, and
/x
perihelion, and yet with no
a theoretical difficulty
which
is
increased by the
Cassiopeia, stars
moving through
visible attracting
body near them.
of Gravitation to double stars, a difficulty like
is
determination of the parallax of Arcturus (only -f 0.018
at right angles to line of sight,
373 miles per second
The
p
3",
faint
accepted, brings this star within that category, for it
sight).
=
star of 6 mag.,
an exceedingly
(Gould's Astron. Journal, 177),
runaways "
Hall's
d
first class.
space with the speed of a comet at Prof.
The
both are very intense.
to alter,
an extraordinarily faint star near
angle 287°.
in applying
colours in
15". with a companion 9 mag., d 277°. 62", companion 13 mag., d p p Finally, Burnham (1878) found that the primary is itself double, there
of
Asaph Hall
The
3050, Andromedae, two stars 6 mag., distance 2.9".
85 Pegasi.
=
being
Prof.
in colour.
companion does not seem
+
0.022),
if
Las a great proper motion (amounting to
and 55 miles per second in the
line of
following Table gives some of the stars of which the parallax, and motion across,
have been ascertained
:
72
Star's Name.
Magnitude. ParolLix
Centauri 61 Cygni Lalande 21,185 Groombridge 34 Lalande 21,285 Arg. (Eltzi'ii 17,415
5 7 8 8'5 9-5
Siriiis
1
a.
.
.
.
.
.
4
Groombridge 1830
7
6
Ursre Majoi-is .
.
=
Distance in years
Annual Motion
of light.
across.
4-35 7-00 6-50 11-00 12-40 13-60 8-00 21-7
.
3
0-150 0-034 0-089 0-046
1
•127
36-6 70-9 25-44
.
2
-05
63-
.
....
a Bootis Pole Star
0-75 0-467 0'501 0-290 0-262 0-247 0-390
1
.... 70 Opliiuchi a Lyrfc .... .
—
1
Printed by Peeet, Gaedneb
&
96-
—
Miles per second.
3-674 5-160 4-750 2-801 4-403 1-270 1-310 1-13 0-36 7-05 1-11
14-4 35-
27-8 28-3 49-2 159 8
22 31
2-258
232 70 373
0045
2
Co., Farringdon Road, London,
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Dedinalion-* 90째
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Ileliographical reproduction from a photograph by the
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Star atlas
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containing
maps
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all
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Hermann
the
K553 J.
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PRESENTED BY
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