hi 
; 
fe 
E 
f 
i 
J. H. Lane on the Theoretical Temperature of the Sun. 61 
it has in common air, and £=1#2, which is the maximum 
sible value it can have in the hight of Clausius’ theory of the 
constitution of the gases. The calculation of the curve of 
9 
%o 
small values of «x, integration by series enables us readily to 
deduce from oe hn (6) and (7) the following apipieicindate 
numerical equations 
, or of (2) , begins at the sun’s center where z=0. For the 
For k=14, 
M= Jes — yer ah ee? —sh Thee + ke. (8) 
1\°4 
i—(-) = fe? — pet od ret®—ro fs ge®-+ &e. (9) 
0 
For k=13, 
w= Je? — aye? +t pt" — selegt®+ ke. (10) 
ai )i=yet— hot +rzp0t'— srtpav®+ &e. (11) 
0 
kl 
For larger values of 2, until =) becomes _ sufficiently 
small as there is no need of great precision in these bed 
tions, I have merely developed the values of # and 
corresponding to =1'1, x=12, z=1°3, &, by means of dif- 
ferences taken from the differential co-efficients at the middle of 
each increment of x, and for the same reason have thought it 
sufficient to begin with z=1, in equations (8) and (9) or (10) 
k-1 
and (11). After arriving at a sufficiently small value of (s ) 
the calculation is finished by aid of the following — 
= also derived by integration fron (6) and (7). 
ee es 
k-1 k-~-1 if 
pl a ola (-2) (14+X) M2) 
7" @—e) (k-1)? JE es 2g 
Qo. u(x —a “9 — a 
= ogi ob (x1) 2 a og —2) 
2 
(k—1)(2k2—3k42) Fie vei 
In these abe x’and “’ are the values of x and u corres- 
ponding too= =0, or the upper limit of the supposed solar 
atmosphere, and 
