126 
SOLUTION OF THE EQUATIONS 
fulfilled and it was possible to go beyond the original starting-point to 
r = 0-5.10 11 ; the small mass then remaining would fill the interior with 
mean density -0038 which is (as nearly as we can judge) in the proper 
relation to the actual density -0065 at the point reached. There were 
76 steps in this final calculation and the results at every fourth step are 
given in Table 11. The adopted value of /z was 2-2. 
Table 11. 
Solution for a Point-source. 
r 
M r 
P 
T 
Vr 
Po 
•5 
•0020 
•652 
6-93 
5-889 
1-697 
•9 
•0234 
•989 
6-68 
5-065 
2-477 
1-3 
•0941 
1-273 
6-43 
4-344 
3-070 
1-7 
•2536 
1-501 
6-16 
3-675 
3-473 
2-1 
•5435 
1-659 
5-88 
3-043 
3-660 
2-5 
•997 
1-726 
5-57 
2-452 
3-609 
2-9 
1-628 
1-697 
5-24 
1-916 
3-336 
3-3 
2-422 
1-578 
4-88 
1-448 
2-892 
3-7 
3-337 
1-391 
4-51 
1-058 
2-356 
4-1 
4-313 
1-166 
4-14 
•7489 
1-811 
4-5 
5-286 
•934 
3-77 
•5144 
1-321 
4-9 
6-198 
•719 
3-41 
•3441 
•9202 
5-3 
7-012 
•535 
3-07 
•2250 
•6162 
5-7 
7-707 
•388 
2-74 
•1443 
•3990 
6-1 
8-278 
•274 
2-44 
•0909 
•2511 
6-5 
8-734 
•1895 
2-17 
•05641 
•1543 
6-9 
9-088 
•1288 
1-92 
•03448 
•09268 
7-3 
9-356 
•0861 
1-69 
•02071 
•05456 
7-7 
9-554 
•0567 
1-48 
•01215 
•03146 
8-1 
9-699 
•0372 
1-28 
•00675 
•01780 
Unit 10 11 
1 0 33 
10- 2 
10 6 
10 12 
10 12 
We see from the trend of the column M r that not much mass remains 
to be added after the last line of the table. The small amount to come, 
computed by the methods of § 67, is found to be Ailf = 0-26.10 33 gm. The 
additional radius, which is not required with any great accuracy, is also 
approximately calculated to be A R = 3-25.10 11 cm. 
92. Our result then is that a star for which 
M = 9-96.10 33 gm. = 5-02 x O, 
R = 11-35.10 11 cm. 
emits radiation at a rate given by 
log 10 KL = 62-6590. 
For comparison we calculate by our previous methods the radiation L'