File:Elements of theoretical and descriptive astronomy, for the use of colleges and academies (1901) (14597632409).jpg

Identifier: elementsoftheore00whit_0 (find matches)
Title: Elements of theoretical and descriptive astronomy, for the use of colleges and academies
Year: 1901 (1900s)
Authors: White, Charles J
Subjects: Astronomy.
Publisher: New York: J. Wiley & sons
Contributing Library: University of Florida, George A. Smathers Libraries
Digitizing Sponsor: University of Florida, George A. Smathers Libraries with support from LYRASIS and the Sloan Foundation

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and S, and the least valueof S. The result is 1° 3 37: and no eclipse will occur when themoons latitude exceeds this limit. The least value of the expres-sion is 51 49: and when the moons latitude at opposition is lessthan this, an eclipse cannot fail to occur. There are some con-siderations, however, which have not been taken into account,which may increase each of these limits by about 16. When the moons latitude at opposition is within these limits,an eclipse is possible, but not necessarily certain. In order todetermine whether in such case it will or will not occur, theactual values which P, P, S and will have at that time mustbe substituted in the expression, and the result compared withthe corresponding latitude of the moon. 156. Since a lunar eclipse is caused by the moons enteringthe earths shadow, it will be seen at the same instant of time byevery observer who has the moon above his horizon: and thecharacter of the eclipse, whether total or pn-**^, will be every PLATE III.
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TOTAL ECLIPSE OF THE SUN, OF JULY 18, 1860, showing the Corona and the Red Flames; as observed by OrFeilitzsch, at Castellon de la Plana. SOLAR ECLIPSE. 139 tfhere the same. As the moons motion towards the ea&t is morerapid than that of the earth (and consequently of the shadow),the eclipse will begin at the eastern limb of the moon. A totaleclipse of the moon may last for nearly two hours. Even whentotally eclipsed, however, the moon does not, in general, disappearfrom view, but shines with a dull reddish light. This phenomenonis caused by the earths atmosphere, which refracts the rays oflight from the sun which enter it near the points G and H, Fig.57, and turns them into the cone. The rays which pass stillnearer to these points are probably absorbed by the atmosphere,thus giving rise to the observed increase of the shadow mentionedin Art. 153. SOLAR ECLIPSE, 157. In Fig. 59, let 8 represent the sun, E the earth, and Mthe moon, at the time of a solar eclipse. HAK will be a secti

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