An annular solar eclipse will occur at the Moon's ascending node of orbit between Wednesday, March 10 and Thursday, March 11, 2100, with a magnitude of 0.9338. 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 2.9 days before apogee (on March 13, 2100, at 21:10 UTC), the Moon's apparent diameter will be smaller. The path of annularity will be visible from parts of northeastern Australia, Papua New Guinea, the Solomon Islands, Tuvalu, and Hawaii, California, Oregon, northwestern Nevada, Idaho, Montana, Wyoming, North Dakota, South Dakota, and Minnesota in the United States. A partial solar eclipse will also be visible for parts of Australia, Oceania, and North America.
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 2100 A penumbral lunar eclipse on February 24. An annular solar eclipse on March 10. A penumbral lunar eclipse on August 19. A total solar eclipse on September 4.
Metonic Preceded by: Solar eclipse of May 22, 2096 Followed by: Solar eclipse of December 29, 2103
Tzolkinex Preceded by: Solar eclipse of January 27, 2093 Followed by: Solar eclipse of April 23, 2107
Half-Saros Preceded by: Lunar eclipse of March 5, 2091 Followed by: Lunar eclipse of March 17, 2109
Tritos Preceded by: Solar eclipse of April 10, 2089 Followed by: Solar eclipse of February 8, 2111
Solar Saros 141 Preceded by: Solar eclipse of February 27, 2082 Followed by: Solar eclipse of March 22, 2118
Inex Preceded by: Solar eclipse of March 31, 2071 Followed by: Solar eclipse of February 18, 2129
Triad Preceded by: Solar eclipse of May 10, 2013 Followed by: Solar eclipse of January 9, 2187
Solar eclipses of 2098–2101 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 partial solar eclipse on October 24, 2098 occurs in the previous 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.
References
External links Earth visibility chart and eclipse statistics Eclipse Predictions by Fred Espenak, NASA/GSFC Google interactive map Besselian elements