Solar eclipse of May 9, 1910

A total solar eclipse occurred on May 9, 1910. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. A total solar eclipse occurs when the Moon's apparent diameter is larger than the Sun's, blocking all direct sunlight, turning day into darkness. Totality occurs in a narrow path across Earth's surface, with the partial solar eclipse visible over a surrounding region thousands of kilometres wide. Totality was visible from part of Wilkes Land in Antarctica and Tasmania in Australia.

Solar eclipse of May 9, 1910
SE1910May09T.png
Map
Type of eclipse
NatureTotal
Gamma-0.9437
Magnitude1.06
Maximum eclipse
Duration255 sec (4 m 15 s)
Coordinates48°12′S 125°12′E / 48.2°S 125.2°E / -48.2; 125.2
Max. width of band594 km (369 mi)
Times (UTC)
Greatest eclipse5:42:13
References
Saros117 (63 of 71)
Catalog # (SE5000)9304

Related eclipsesEdit

Solar eclipses of 1910–1913Edit

This eclipse is a member of a semester series. An eclipse in a semester series of solar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternating nodes of the Moon's orbit.[1]

Solar eclipse series sets from 1910–1913
Ascending node   Descending node
117 May 9, 1910
 
Total
122 November 2, 1910
 
Partial
127 April 28, 1911
 
Total
132 October 22, 1911
 
Annular
137 April 17, 1912
 
Hybrid
142 October 10, 1912
 
Total
147 April 6, 1913
 
Partial
152 September 30, 1913
 
Partial


Metonic seriesEdit

The metonic series repeats eclipses every 19 years (6939.69 days), lasting about 5 cycles. Eclipses occur in nearly the same calendar date. In addition, the octon subseries repeats 1/5 of that or every 3.8 years (1387.94 days).

ReferencesEdit

  1. ^ van Gent, R.H. "Solar- and Lunar-Eclipse Predictions from Antiquity to the Present". A Catalogue of Eclipse Cycles. Utrecht University. Retrieved 6 October 2018.