Solar Eclipse
A Solar Eclipse occurs when an observer on Earth passes through the shadow cast by the Moon which fully or partially blocks the Sun. This happens when the Sun, Moon and observer are nearly aligned on a straight line when the Moon is close to the ecliptic. In a total solar eclipse, the disk of the Sun is fully obscured by the Moon. In partial and annular eclipses, only part of the Sun is obscured.
Sun Moon Size Coincidence
It is acknowledged that it is an 'extraordinary coincidence' that the maximum size of the Moon matches the size of the Sun. From p.67 of A Question and Answer Guide to Astronomy by Astrophysicists Carol Christian (bio) and Jean-René Roy (bio):
“ Is it just coincidence that the apparent diameters of the Moon and the Sun are the same?
Yes, it is a coincidence that the two diameters are the same but it was not always so. The diameter of the Sun is about 400 times that of the Moon, but the Sun is also 400 times further away from us than the Moon. The configuration leads to the same apparent diameters for both objects when seen from Earth (05°). This extraordinary coincidence grants us the opportunity to have total eclipses of our star, a majestic cosmic phenomenon that used to terrify ancient peoples. ”
Solar Eclipse Path Comparison
Of interest is that on the globe the paths of the Solar Eclipse look rather odd:
On the Flat Earth map the paths appear to be symmetrical arcs:
From A Text-Book of Astronomy by George C. Comstock (p.113) (Archive)
“ Fig. 36.—Central eclipses for the first two decades of the twentieth century. Oppolzer.
Future eclipses.—An eclipse map of a different kind is shown in Fig. 36, which represents the shadow paths of [pg. 114] all the central eclipses of the sun, visible during the period 1900-1918 A. D., in those parts of the earth north of the south temperate zone. Each continuous black line shows the path of the shadow in a total eclipse, from its beginning, at sunrise, at the western end of the line to its end, sunset, at the eastern end, the little circle near the middle of the line showing the place at which the eclipse was total at noon. The broken lines represent similar data for the annular eclipses. This map is one of a series prepared by the Austrian astronomer, Oppolzer, showing the path of every such eclipse from the year 1200 B. C. [pg. 115] to 2160 A. D., a period of more than three thousand years. ”
Further Reference
Also see this interesting comparison:
