100
Gaseous Stars
[ch. Ill
The last column of the table gives values of the central temperature T c ,
or rather of the quantity T c r, where r is measured in terms of the radius of
the sun; these are calculated directly from equation ( 88 ‘ 6 ).
Table XI. Solutions fon stars of different masses.
K
n
£(o = i)
\
-(A)*
T '{mf
1-308
3-250
358
00
0
0
1-307
3-254
360
230
0-20
11 X 10°
1-307
3-256
361
150
0-25
14x10°
1-306
3-272
363
42
0-50
28 x 10«
1-301
3-325
375
12-2
1-00
55 x 10°
1-300
3-333
375
11-0
1-06
58 x 10°
1-286
3-500
400
3-50
2-49
126x10°
1-267
3-750
446
1-62
5-44
264 x 10°
1-250
4-000
500
1-00
10-12
490 x10°
1-222
4-500
614
0-50
29-13
1900x10°
1-204
4-900
758
0-32
65-25
15200x10°
1-200
5-000
799
0-29
78-78
00
1-141
7-000
—
o-oo
oo
00
As examples of the use of this table and Table X, Table XII gives
calculated values of the central density and temperatures of actual stars,
calculated on the supposition of a uniform effective molecular weight fx = 2 5.
Table XII. Solutions for actual stars.
(Solutions with j — l = 0 calculated for eff. mol. weight /x = 2 5.)
Star
Mass
(0=1)
\
n
P
Pc
r (O = 1)
T e
B.D. 6° 1309
[78]
0-29
5-00
0-14
[oo]
[oo]
H.I). 1337 A
36-3
0-45
4-59
0-004
40
23-8
200 X10°
Y Puppis A
19-2
0-67
4-27
006
120
7-6
160 X10°
u Herculis A
7-6
1-20
3-90
0-14
70
4-6
100 x10°
Sirius A
2-45
3-53
3-50
0-93
140
1-58
80x10°
Sun
1-00
12-2
3-33
1-42
140
1-00
55 x 10°
60 Kruger A
0-25
150
3-26
9-6
860
0-33
42 x 10°
„ B
0-20
230
3-25
60
5300
0-17
65 x 10°
Betelgeux
[40]
0-42
4-65
2x10-°
[0-041
300
10 x 10°
Capella A
4-18
2-08
3-65
0-004
1
11
19x10°
a Cent. B
0-97
12-9
3-32
0-76
70
1-2
45 x 10°
92. In § 90 we saw that when the mass M of a star is given, and the
effective molecular weight ¡x of the matter of which it is composed, it is
possible to calculate the value of \ c , the ratio of gas-pressure to pressure of
radiation at its centre. It is also possible to calculate n. Thus all stars for
which M and ¡x are specified have the same values of \ c and n. They are
