• Source: Solar eclipse of April 13, 1801

    • A partial solar eclipse occurred at the Moon's ascending node of orbit on Monday, April 13, 1801, with a magnitude of 0.4208. 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 modern-day eastern Europe, the Middle East, Central Asia, and western Russia.


    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. The first and last eclipse in this sequence is separated by one synodic month.


    Related eclipses




    = Eclipses in 1801

    =
    A partial solar eclipse on March 14.
    A total lunar eclipse on March 30.
    A partial solar eclipse on April 13.
    A partial solar eclipse on September 8.
    A total lunar eclipse on September 22.
    A partial solar eclipse on October 7.


    = Metonic

    =
    Preceded by: Solar eclipse of June 24, 1797
    Followed by: Solar eclipse of January 30, 1805


    = Tzolkinex

    =
    Preceded by: Solar eclipse of March 1, 1794
    Followed by: Solar eclipse of May 25, 1808


    = Half-Saros

    =
    Preceded by: Lunar eclipse of April 7, 1792
    Followed by: Lunar eclipse of April 19, 1810


    = Tritos

    =
    Preceded by: Solar eclipse of May 14, 1790
    Followed by: Solar eclipse of March 13, 1812


    = Solar Saros 145

    =
    Preceded by: Solar eclipse of April 1, 1783
    Followed by: Solar eclipse of April 24, 1819


    = Inex

    =
    Preceded by: Solar eclipse of May 2, 1772
    Followed by: Solar eclipse of March 24, 1830


    = Triad

    =
    Preceded by: Solar eclipse of June 12, 1714
    Followed by: Solar eclipse of February 11, 1888


    = Solar eclipses of 1798–1801

    =
    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 eclipses on [h] occur in the previous lunar year eclipse set, and the partial solar eclipses on March 14, 1801 and September 8, 1801 occur in the next lunar year eclipse set.


    = Saros 145

    =
    This eclipse is a part of Saros series 145, repeating every 18 years, 11 days, and containing 77 events. The series started with a partial solar eclipse on January 4, 1639. It contains an annular eclipse on June 6, 1891; a hybrid eclipse on June 17, 1909; and total eclipses from June 29, 1927 through September 9, 2648. The series ends at member 77 as a partial eclipse on April 17, 3009. 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 15 at 6 seconds (by default) on June 6, 1891, and the longest duration of totality will be produced by member 50 at 7 minutes, 12 seconds on June 25, 2522. 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.


    See also


    List of solar eclipses in the 19th century


    References




    External links


    Google interactive maps
    Solar eclipse data

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