Solar eclipse of December 3, 1918 | |
---|---|
Type of eclipse | |
Nature | Annular |
Gamma | -0.2387 |
Magnitude | 0.9383 |
Maximum eclipse | |
Duration | 426 sec (7 m 6 s) |
Coordinates | 36°06′S53°42′W / 36.1°S 53.7°W |
Max. width of band | 236 km (147 mi) |
Times (UTC) | |
Greatest eclipse | 15:22:02 |
References | |
Saros | 131 (45 of 70) |
Catalog # (SE5000) | 9325 |
An annular solar eclipse occurred on December 3, 1918. 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 Chile including the capital city Santiago, Argentina including capital Buenos Aires, southern Uruguay including capital Montevideo, northeastern tip of South West Africa (today's Namibia) and southwestern Portuguese Angola (today's Angola). Aconcagua, the highest mountain outside Asia, also lies in the path of annularity.
A solar eclipse occurs when a portion of the Earth is engulfed in a shadow cast by the Moon which fully or partially blocks ("occults") sunlight. This occurs when the Sun, Moon and Earth are aligned. Such alignment coincides with a new moon (syzygy) indicating the Moon is closest to the ecliptic plane. In a total eclipse, the disk of the Sun is fully obscured by the Moon. In partial and annular eclipses, only part of the Sun is obscured.
Earth's Moon is an astronomical body that orbits the planet and acts as its only permanent natural satellite. It is the fifth-largest satellite in the Solar System, and the largest among planetary satellites relative to the size of the planet that it orbits. The Moon is, after Jupiter's satellite Io, the second-densest satellite in the Solar System among those whose densities are known.
Earth is the third planet from the Sun and the only astronomical object known to harbor life. According to radiometric dating and other sources of evidence, Earth formed over 4.5 billion years ago. Earth's gravity interacts with other objects in space, especially the Sun and the Moon, Earth's only natural satellite. Earth orbits around the Sun in 365.26 days, a period known as an Earth year. During this time, Earth rotates about its axis about 366.26 times.
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]
A lunar node is either of the two orbital nodes of the Moon, that is, the two points at which the orbit of the Moon intersects the ecliptic. The ascending node is where the Moon moves into the northern ecliptic hemisphere, while the descending node is where the Moon enters the southern ecliptic hemisphere.
Solar eclipse series sets from 1916–1920 | ||||
---|---|---|---|---|
Ascending node | Descending node | |||
111 | December 24, 1916 Partial | 116 | June 19, 1917 Partial | |
121 | December 14, 1917 Annular | 126 | June 8, 1918 Total | |
131 | December 3, 1918 Annular | 136 | May 29, 1919 Total | |
141 | November 22, 1919 Annular | 146 | May 18, 1920 Partial | |
151 | November 10, 1920 Partial |
It is a part of Saros cycle 131, repeating every 18 years, 11 days, containing 70 events. The series started with partial solar eclipse on August 1, 1125. It contains total eclipses from March 27, 1522 through May 30, 1612 and hybrid eclipses from June 10, 1630 through July 24, 1702, and annular eclipses from August 4, 1720 through June 18, 2243. The series ends at member 70 as a partial eclipse on September 2, 2369. The longest duration of totality was only 58 seconds on May 30, 1612. All eclipses in this series occurs at the Moon’s ascending node.
Saros cycle series 131 for solar eclipses occurs at the Moon's ascending node, repeating every 18 years, 11 days, containing 70 events. All eclipses in this series occurs at the Moon's ascending node.
Series members 33–70 occur between 1702 and 2369 | ||
---|---|---|
33 | 34 | 35 |
July 24, 1702 | August 4, 1720 | August 15, 1738 |
36 | 37 | 38 |
August 25, 1756 | September 6, 1774 | September 16, 1792 |
39 | 40 | 41 |
September 28, 1810 | October 9, 1828 | October 20, 1846 |
42 | 43 | 44 |
October 30, 1864 | November 10, 1882 | November 22, 1900 |
45 | 46 | 47 |
December 3, 1918 | December 13, 1936 | December 25, 1954 |
48 | 49 | 50 |
January 4, 1973 | January 15, 1991 | January 26, 2009 |
51 | 52 | 53 |
February 6, 2027 | February 16, 2045 | February 28, 2063 |
54 | 55 | 56 |
March 10, 2081 | March 21, 2099 | April 2, 2117 |
57 | 58 | 59 |
April 13, 2135 | April 23, 2153 | May 5, 2171 |
60 | 61 | 62 |
May 15, 2189 | May 27, 2207 | June 6, 2225 |
63 | 64 | 65 |
June 18, 2243 | June 28, 2261 | July 9, 2279 |
66 | 67 | 68 |
July 20, 2297 | August 1, 2315 | August 11, 2333 |
69 | 70 | |
August 22, 2351 | September 2, 2369 |
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Fred Espenak is a retired emeritus American astrophysicist. He worked at the Goddard Space Flight Center. He is best known for his work on eclipse predictions.
The National Aeronautics and Space Administration is an independent agency of the United States Federal Government responsible for the civilian space program, as well as aeronautics and aerospace research.
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