Solar eclipse of October 22, 1911 | |
---|---|
Type of eclipse | |
Nature | Annular |
Gamma | 0.3224 |
Magnitude | 0.965 |
Maximum eclipse | |
Duration | 227 sec (3 m 47 s) |
Coordinates | 6°18′N121°24′E / 6.3°N 121.4°E |
Max. width of band | 133 km (83 mi) |
Times (UTC) | |
Greatest eclipse | 4:13:02 |
References | |
Saros | 132 (40 of 71) |
Catalog # (SE5000) | 9307 |
An annular solar eclipse occurred on October 22, 1911. 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 the Russian Empire (the parts now belonging to Kazakhstan, Uzbekistan and Kyrgyzstan), China, French Indochina (the part now belonging to Vietnam), Philippines, Dutch East Indies (today's Indonesia), Territory of Papua (now belonging to Papua New Guinea) including the capital city Port Moresby, and British Western Pacific Territories (the parts now belonging to Solomon Islands and Tuvalu, including the city of Honiara and Tulagi).
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 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 |
This eclipse is a part of Saros cycle 132, repeating every 18 years, 11 days, containing 71 events. The series started with partial solar eclipse on August 13, 1208. It contains annular eclipses from March 17, 1569 through March 12, 2146, hybrid on March 23, 2164 and April 3, 2183 and total eclipses from April 14, 2200 through June 19, 2308. The series ends at member 71 as a partial eclipse on September 25, 2470. The longest duration of annular was 6 minutes, 56 seconds on May 9, 1641, and totality will be 2 minutes, 14 seconds on June 8, 2290. All eclipses in this series occurs at the Moon’s descending node.
Saros cycle series 132 for solar eclipses occurs at the Moon's descending node, repeating every 18 years, 11 days, containing 71 events. All eclipses in this series occurs at the Moon’s descending node.
Series members 28-50 occur between 1690 and 2100: | ||
---|---|---|
28 | 29 | 30 |
June 11, 1695 | June 22, 1713 | July 4, 1731 |
31 | 32 | 33 |
July 14, 1749 | July 25, 1767 | August 5, 1783 |
34 | 35 | 36 |
August 17, 1803 | August 27, 1821 | September 7, 1839 |
37 | 38 | 39 |
September 18, 1857 | September 29, 1875 | October 9, 1893 |
40 | 41 | 42 |
October 22, 1911 | November 1, 1929 | November 12, 1947 |
43 | 44 | 45 |
November 23, 1965 | December 4, 1983 | December 14, 2001 |
46 | 47 | 48 |
December 26, 2019 | January 5, 2038 | January 16, 2056 |
49 | 50 | |
January 27, 2074 | February 7, 2092 |
An annular solar eclipse occurred on December 14, 2001. 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. It was visible across the Pacific ocean, southern Costa Rica, northern Nicaragua and San Andrés Island, Colombia. The central shadow passed just south of Hawaii in early morning and ended over Central America near sunset.
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A total solar eclipse occurred on February 5, 1962. 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 Indonesia, Netherlands New Guinea, the Territory of Papua New Guinea, British Solomon Islands, and Palmyra Atoll.
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An annular solar eclipse occurred on Friday, 24 February 1933. 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, Argentina, Portuguese Angola, French Equatorial Africa, Belgian Congo, Anglo-Egyptian Sudan, Ethiopia, French Somaliland, southeastern Italian Eritrea, and Mutawakkilite Kingdom of Yemen, Aden Protectorate and Aden Province in British Raj.
An annular solar eclipse occurred on March 7, 1932. 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.
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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