s ° ʹ
Sun’s mean distance from the Node at F. Moon in _May 1761_ 11 26 47
Add the Equation of the Node, for the Sun’s Anomaly 10^s
18° 15ʹ[85] + 6
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Sun’s mean distance from the Node corrected 11 26 53
Add the Equation of the Sun’s mean Place + 1 15
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Sun’s true distance from the Ascending Node 11 28 8
To which add 6 Signs, See § 363 6
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The sum is the Moon’s true distance from the same Node 5 28 8
[Sidenote: Pl. XII.]
Or the _Argument_ of her _Latitude_; which in Table XIV, gives the
Moon’s true Latitude, _viz._ 9ʹ 56ʺ North Descending.
385. Having by the foregoing precepts § 355 found the true time of
Opposition of the Sun and Moon in a lunar Eclipse, with the Moon’s
Anomaly enter Table XV and take out her horizontal Parallax, also her
true horary Motion and Semi-diameter: and likewise those of the Sun by
his Anomaly, as already taught § 364 & _seq._ Then add the Sun’s
horizontal Parallax, which is always 10 Seconds, to the Moon’s
horizontal Parallax, and from their sum subtract the Sun’s
Semi-diameter; the remainder will be the Semi-diameter of that part of
the Earth’s shadow which the Moon goes through.
386. From the Sum of the Semi-diameters of the Moon and Earth’s Shadow,
subtract the Moon’s Latitude; the remainder is the parts deficient.
Then, as the Semi-diameter of the Moon is to 6 Digits, so are the parts
deficient to the Digits eclipsed.
387. If the parts deficient be more than the Moon’s Diameter, the
Eclipse will be total with continuance; if less, it will not be total;
if equal, it will be total, but without continuance.