Partial solar eclipse November 9, 1855
A partial solar eclipse occurred at the Moon's descending node of orbit on Friday, November 9, 1855, with a magnitude of 0.4892. 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 partial solar eclipse occurs in the polar regions of the Earth when the center of the Moon's shadow misses the Earth.
The partial solar eclipse was visible for parts of southern Oceania and Antarctica.
Description.
The eclipse was visible in Tasmania and the southeasternmost areas of Australia, New Zealand and its surrounding islands such as Chatham and Cook and much of Antarctica which most areas had a 24-hour daylight with the exception of the northernmost peninsular area (from the areas south of the Antarctic Circle) and its surrounding islands and the northernmost area at the 50th meridian east. It included a tiny southeast area of the Indian Ocean, the southwesternmost of the Pacific and the tiny portion of the southernmost Atlantic.
The eclipse started at sunrise west of New Zealand and ended at sunset off the coast of Antarctica. Areas that the eclipse ended slightly after or at sunrise included Sydney, Wollongong and Irvine in Australia. Areas that were in the rim of the eclipse included New Caledonia.
The greatest eclipse was in the Pacific Ocean hundreds of miles (or kilometers) north of Antarctica at 62.5 S &amp; 121 E at 19:12 UTC (3:12 AM local time on November 10).
The eclipse showed 25% obscuration in the south of South Island, New Zealand and up to 48% at the area of the greatest eclipse.
The subsolar marking was in the Pacific Ocean around the Tropic of Capricorn.
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.
Solar eclipses of 1852–1855.
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 January 21, 1852 occurs in the previous lunar year eclipse set.
Saros 150.
This eclipse is a part of Saros series 150, repeating every 18 years, 11 days, and containing 71 events. The series started with a partial solar eclipse on August 24, 1729. It contains annular eclipses from April 22, 2126 through June 22, 2829. There are no hybrid or total eclipses in this set. The series ends at member 71 as a partial eclipse on September 29, 2991. 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 will be produced by member 45 at 9 minutes, 58 seconds on December 19, 2522. All eclipses in this series occur at the Moon’s descending 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 descending 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.
 ;templatestyles src="Reflist/styles.css" / ;