&Iv

A

Sis RONOM t

_

S-tP A -(- P S == S Q_= Distance of the Comet

A . 7* g'ves the Ordinate A Q, and thence we have■ W ^ -

*he ^ , e Sim, which therefore is given. Therefore ina !x sl S^ e S A Q_, right-angled at A, we have SQ,%g] e '> to find the Angle QS A ; and then P S Q_the.j' om the Perihelion is known. When this isL’ a ’ a the other Particulars are the fame as in the

I ^° r ^P alcu ^ s -

. * "Efe are the Principles or Elements of Calcu-^Ple* ^ich we shall now proceed to illustrate by Ex-a Hd obs^ at *-he Praxis may not remain so difficultc fioi Ce Curs as it has hitherto been ; and we snail make^he last Comet for this Purpose, whose mean‘Pitied ^ 0r ^‘ urna l Area is in the first Place to be deter-

S of 11 0r fier‘ to this, we have the constant mean Mo-lQfl 'I)'sl.^’ 0rnet nroving in a Parabola, whose Perihe-1 tance P8—p.—I —Lemidiameter of the Earth’s

109 D. 14 H. 46""

: 0.91228, whose

On.

> ‘^> &;V < 100

^ntUs 9 ' 960138 ^ therefore always at hand for

^ L 0 ^fi e Perihelion Distance P 3 —r—0,22206, and^t 0 f J t ar ‘ t hrn 9,346472, as in the Table, for the Co-

I ?4v* But we have its mean Anomaly s = NX

n Article 15.); therefore to find n by Logarithms

'he p r

*Pk ° Ce fi ‘s as follows : ' >

. It 7,

’’Hicjj S ar ithm of Perihelion-Distance r — 9.346

Multiply by

* tie p

, r °du<£f ; s t h e Logarithm otVl(ie ^7 2, the Quotient is Log. of

tr 1 ’

3 _

Osteal Complement is the Log. of ~ -

^ioh add the Logarithm of ^ —

V ?• of mean Anomaly

III, P

209

: 8.03941619.019708

: ©,980292: 9.960128

8,7:8^0,94042021. Having