Astronomy.

Sun’s Place being found, in

Earth’. xii_ •„ , i ■ .i ’

o a luutiu, iii fcw 14^ 22 03 ,

.cij - “ Place will be in the, opposite Part of the

'Hi S Vi ' z ' in ct. 14° 22' 03" at T. If therefore from

\ A e Dbtract the Comet’s Heliocentric Place at H,th e j have the Arch HT ~ 63° 49'43" = D S T,Arw n & e °s Commutation.

f 49 43

And as the Earth’s mean,a rt , ,~v is 7 S. 4^ 58' 23”, the Logarithm of the*ls 0 {( s distance S T will be 9,993947. But S D is

Or ; therefore we can find the Angle DTS

J ' " J UJC.ICIU1C we. K.G .li HIV

^ ° n gation of the Comet from the Si

Is °f the Sides ST-f SD = 1,74000= 0.240549

eir Difference ST—SD = ~ "

tileT a „ r. , a D “ T

1 a ng. of \ theAng.-

so

T

an g. of i their Diff.

2

D—T

-0,23240:158° 00':

thus

0-2-.9-366236

10.204211

2 12"’ 03’= 9.329S98

^ e nce 58' + 1 2’ 03 — 70° 03the ^ 130 03' — 45 0 57' = S T D, or

:TDS, and

-j — _ Longitude of

hc e ° niet from the Sun ; which added to the Sun’sh, j I gives the Geocentric Longitude of the Comet at0 r^ n ’ Qo° And to find the Geocentric Latitude,

^ n Sle D T Q, W e have this Analogy :

h t ttle Si neo f Commutation TSV-fiL LO-9.953650So Sine of Elongation STD =45 57 '= 9 ’ 8 5^ 8sa «g. ofHelio.Lat. DSQ=24 0 i2'= 9 .652650-j' —--

° the Tang. of Geo. Lat. DTQ=i9'46-9-5$5568

Thus you have the whole Process of Calculation,i p re 'ates to the Phænomena of a Comet moving, in'sted f ola near the Vertex, and is the fame with that,A n{ j “ r the Planets' (from ’the 25th Article inclusive).9 hd t h ? u gh it is certain (from what will be shewn byy) that this Comet does not deicribe a L*avabola^Ldtz ^ ^Uipsis, yet the computed Longitude and Lati-^ re the fame which the Comet was observed toAw a ^ l hat very Tin,e j whence the Accuracy of this.a ha r . | sufficiently appears : But as it is thus limited toiio t ^ a 'ola, and only one. small Part.of that, and can-the ^. ex tended to determine the 7 \xis of the Orbit, or‘ute of its Revolution, I shall here supply thisP 3 great