200

As T R 0 N O M ¥.

a Comet in every Part of its Orbit? ^how from thence it moves with a retar . v

Yeloc 1 "

(i pis'

as follows. The Line NC, as being the r icar? - s pel'tance of the Centres of the Shadows and Di^?A ^ st

pendicular to the Path E H, and is >-' tn "

NT - 62s 10" 4 - 16" 52" -st 16' 23",

“ eq, “ 1 ."- -4"!

VIZ-

. -I- 1 -- "O ’ Ijh

the Moon’s Horizontal Parallax, and of the Sen* :ters of the Sun and Moon, all of them whenAlso the Angle N C, when least, is 5 0 2 °'‘ r .J til 6fore in the Right-angled Triangle N C, to 11Side K C, we have the following Analogy.

As the Sine of the Angle N 8 C r 5“ 30' — 8-9

^qqC^

Is to Radius 00°- 00 = l0, °co0 0 ^

So is the Logarithm of the SideNC —95',5 =

To the Logarithm of the Side 9 € — 996',4=

23. The Ecliptic Limit, therefore, is 99^

36’, beyond which Distance from the Node Kbe no Eclipse ; and within that Distance if the

be New, the Shadow will fall on some Part of t*V e j 0 vf Sas at B ; where all those Places over which the Spass will fee the Sun eclipsed, in part only by th e _ aI APenumbral Shadow, but totally by the dark ShauO'^’^erthe Sun will be centrally eclipsed to all those Pl‘ lCwhich the Centre of the Shadows paffeth. v/iy

24. If the Moon be new in the Node itself, st 6the Centre of the Shadows pass over the Centr? e j)tDisk, as represented at Q . In this Cafe if the a P‘guJi>Diameter of the Moon be greater than that of t* 1 p a r tsthe Face of the Sun will be wholly obscured to ®

over which the Centre pastes ; but if not, the ^jjlonly be centrally eclipsed?^ but his Circumferences?appear a bright Annulus , or luminous Ring?,

Width will be equal to the Difference of the D )aof the Luminaries. , „ j it

25. As the Distc of the Earth is here pi'ojstrepresents the Cafe of an Eclipse on an Equinoflsi y steso that A K is the Ecliptic, Æ Q_the Equator, 2 * ^js