G. Hinrichs on Planetology. 
so that (43) becomes is Be 
1 
- fat re] we Op ng” 8. ee eee (44) ie 
giving for » constant, 
é=C.: “Vere eo. ke 
or, since by Kepler’s third law, c?=axy, 
= Snr 271, 
above. ei 
Instead of solving the problem directly, we may indirectlyt 
to find how » must vary that (86) may become (88), i. @ 0 
a constant term to (46). In other words, C instead of being 
stant must be considered a function oft, i. e. (44) must be 
1fde 
lat|= pli); 9 <. 6 eae (47) 
so that the resistance now becomes, see (42), 
‘ yee ao, O89 
elas ee: Sal) 
instead of (41), where cos 7 = soi and ds is the element of 
orbit. The function g(t) can now, by the method of the ¥ 
tion of the arbitrary constants, be so determined that (46) 
coincides with (38). Since r is a function of ¢, we may ™ ) 
Har git » So 6 eee ee 
hence (47) becomes Dans dk 
of rc=s (0). a te.) ae ee Se 
Taking the complete differential of (45), i.e. also conside 
C variable, substituting in (50) and reducing by (45), we ¢ 
for the determination of C 
ig Sf aa ee 
This gives, by making K an arbitrary constant, 
Oh Gere fe ae 
which, substituted in (46), gives, . 
ox ok 4.fe"'f).diy 8 
This should be identical with (88), i.e. (remembering 
here is counted from the most distant, in (88) from the 
