Solar eclipse of November 11, 1901

An annular solar eclipse occurred at the Moon's ascending node of orbit on Monday, November 11, 1901, with a magnitude of 0.9216. 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. Occurring about 4.5 hours before apogee (on November 11, 1901, at 12:00 UTC), the Moon's apparent diameter was smaller.

Annularity was visible from the Italian island Sicily, the whole British Malta (now Malta), Ottoman Tripolitania (now Libya), Egypt, Ottoman Empire (parts now belonging to Cretan State in Greece, Israel, Jordan and Saudi Arabia), Emirate of Jabal Shammar (now belonging to Saudi Arabia), Aden Protectorate (now belonging to Yemen), Muscat and Oman (now Oman), British Raj (the parts now belonging to India, Andaman and Nicobar Islands and Myanmar), British Ceylon (now Sri Lanka), Siam (name changed to Thailand later), French Indochina (the parts now belonging to Cambodia, southern tip of Laos and southern Vietnam, including Phnom Penh), Bombay Reef in the Paracel Islands, and Philippines. A partial eclipse was visible for parts of North Africa, East Africa, most of Asia, and Northern Australia.

Eclipse details

Shown below are two tables displaying details about this particular solar eclipse. The first table outlines times at which the Moon's penumbra or umbra attains the specific parameter, and the second table describes various other parameters pertaining to this eclipse.

Eclipse season

This eclipse is part of an eclipse season, a period, roughly every six months, when eclipses occur. Only two (or occasionally three) eclipse seasons occur each year, and each season lasts about 35 days and repeats just short of six months (173 days) later; thus two full eclipse seasons always occur each year. Either two or three eclipses happen each eclipse season. In the sequence below, each eclipse is separated by a fortnight.

Related eclipses

Eclipses in 1901

• A penumbral lunar eclipse on May 3.
• A total solar eclipse on May 18.
• A partial lunar eclipse on October 27.
• An annular solar eclipse on November 11.

Metonic

• Preceded by: Solar eclipse of January 22, 1898
• Followed by: Solar eclipse of August 30, 1905

Tzolkinex

• Preceded by: Solar eclipse of September 29, 1894
• Followed by: Solar eclipse of December 23, 1908

Half-Saros

• Preceded by: Lunar eclipse of November 4, 1892
• Followed by: Lunar eclipse of November 17, 1910

Tritos

• Preceded by: Solar eclipse of December 12, 1890
• Followed by: Solar eclipse of October 10, 1912

Solar Saros 141

• Preceded by: Solar eclipse of October 30, 1883
• Followed by: Solar eclipse of November 22, 1919

Inex

• Preceded by: Solar eclipse of November 30, 1872
• Followed by: Solar eclipse of October 21, 1930

Triad

• Preceded by: Solar eclipse of January 10, 1815
• Followed by: Solar eclipse of September 11, 1988

Solar eclipses of 1898–1902

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.

The solar eclipses on January 22, 1898 (total) and July 18, 1898 (annular) occur in the previous lunar year eclipse set, and the partial solar eclipse on April 8, 1902 occurs in the next lunar year eclipse set.

Saros 141

This eclipse is a part of Saros series 141, repeating every 18 years, 11 days, and containing 70 events. The series started with a partial solar eclipse on May 19, 1613. It contains annular eclipses from August 4, 1739 through October 14, 2640. There are no hybrid or total eclipses in this set. The series ends at member 70 as a partial eclipse on June 13, 2857. Its eclipses are tabulated in three columns; every third eclipse in the same column is one exeligmos apart, so they all cast shadows over approximately the same parts of the Earth.

The longest duration of annularity was produced by member 20 at 12 minutes, 9 seconds on December 14, 1955. All eclipses in this series occur at the Moon’s ascending node of orbit.

Metonic series

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). All eclipses in this table occur at the Moon's ascending node.

Tritos series

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.

Inex series

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.

Notes

• Eclipse Predictions by Fred Espenak, NASA/GSFC