Solar eclipse of January 3, 1927

Summary

An annular solar eclipse occurred on January 3, 1927. 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. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide. Annularity was visible from New Zealand on January 4 (Tuesday), and Chile, Argentina, Uruguay and southern Brazil on January 3 (Monday).

Solar eclipse of January 3, 1927
Map
Type of eclipse
NatureAnnular
Gamma−0.4956
Magnitude0.9995
Maximum eclipse
Duration3 s (0 min 3 s)
Coordinates52°48′S 124°48′W / 52.8°S 124.8°W / -52.8; -124.8
Max. width of band2 km (1.2 mi)
Times (UTC)
Greatest eclipse20:22:53
References
Saros140 (24 of 71)
Catalog # (SE5000)9343

Observations edit

 
View of the eclipse from Buenos Aires

Related eclipses edit

Solar eclipses 1924–1928 edit

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 1924 to 1928
Ascending node   Descending node
115 July 31, 1924
 
Partial
120 January 24, 1925
 
Total
125 July 20, 1925
 
Annular
130 January 14, 1926
 
Total
135 July 9, 1926
 
Annular
140 January 3, 1927
 
Annular
145 June 29, 1927
 
Total
150 December 24, 1927
 
Partial
155 June 17, 1928
 
Partial

Inex series edit

This eclipse is a part of the long period inex cycle, repeating at alternating nodes, every 358 synodic months (≈ 10,571.95 days, or 29 years minus 20 days). Their appearance and longitude are irregular due to a lack of synchronization with the anomalistic month (period of perigee). However, groupings of 3 inex cycles (≈ 87 years minus 2 months) comes close (≈ 1,151.02 anomalistic months), so eclipses are similar in these groupings.

Saros 140 edit

It is a part of Saros cycle 140, repeating every 18 years, 11 days, containing 71 events. The series started with partial solar eclipse on April 16, 1512. It contains total eclipses from July 21, 1656, through November 9, 1836, hybrid eclipses from November 20, 1854, through December 23, 1908, and annular eclipses from January 3, 1927, through December 7, 2485. The series ends at member 71 as a partial eclipse on June 1, 2774. The longest duration of totality was 4 minutes, 10 seconds on August 12, 1692.

Tritos series edit

This eclipse is a part of a tritos cycle, repeating at alternating nodes every 135 synodic months (≈ 3986.63 days, or 11 years minus 1 month). Their appearance and longitude are irregular due to a lack of synchronization with the anomalistic month (period of perigee), but groupings of 3 tritos cycles (≈ 33 years minus 3 months) come close (≈ 434.044 anomalistic months), so eclipses are similar in these groupings.

Notes edit

  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.

References edit

  • Earth visibility chart and eclipse statistics Eclipse Predictions by Fred Espenak, NASA/GSFC
    • Google interactive map
    • Besselian elements