Full text: Elemente der physischen Astronomie (Dritter Theil)

. 358 
Es war aber 
, _ r(^) * = ,_ 
h 2 J V dv * u 2 
[ ——-—-Cos2(v—mv)— .eCos[2rv-mv)—(cv_ w)]+| 
2(1—m) v l—m—c v J 
3 m 
3 
also ist 
/ ^ ju 2 \ 
ndt = — dv ( Cos 2 ( v —mv) — aA°Cos2 (v —mv) I und 
\/ f (i—m) * ' 2 J 
A° . 3 m* 
nt — Sin2(v—mv)— — ——j Sin 2 (v—mv), 
1—m 
woraus folgt 
ndt 
C c = 
Eben so hat man 
'3 m' 
A° 
ö(i—m) : 
3 m* 
1—m 8(1 —m)* 
So m' 1 \ 
= * i—m-c 6 C0S ^ (. v ~ mv )~ (cv-w)] J 
— 2 dv. A' e Cos [2 ( v —mv) — (cv—w)] 
f , 3 m 
X * + 
l 
2 1—m—c 
2 
* eCos[2(v—mv) — (cv 
-w)]j 
nt 
/ 3 m 2 \ 
ss edv. Cos[2(v—mv)—(cv—w)] . ^ ,;_;; ])L _ C — 2 Ay, also 
/ 3m* sA' 
\(2—2m — 
^ e Sin [2 (v—mv) — (cv—w)] , 
c) * 2 — 2 m —c 
woraus folgt 
q? _ 3 m 2 — 2 A' (2 — 2 m — c) 
(2 — 2 m — c) 2 
Endlich ist für den Winkel c'mv— w / 
nd t •= — 2 A 5 e / dv . Cos (c'mv—w') , also 
¡A 5 e / 
c'm 
Sin (c'mv—w') / und daher 
C* = — 
2A 5 
c'm
	        
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