• Source: Solar eclipse of February 15, 1961

      • A total solar eclipse occurred at the Moon's descending node of orbit on Wednesday, February 15, 1961, with a magnitude of 1.036. 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. Occurring about 21 hours after perigee (on February 14, 1961, at 11:30 UTC), the Moon's apparent diameter was larger.
      Totality was visible from France, Monaco, Italy, San Marino, SFR Yugoslavia (parts now belonging to Croatia, Bosnia and Herzegovina, Montenegro, Serbia and Kosovo, North Macedonia), Albania, Bulgaria including the capital city Sofia, Romania including the capital city Bucharest, and the Soviet Union (parts now belonging to Ukraine, Russia and Kazakhstan). The maximum eclipse was recorded near Novocherkassk (Russian SFSR). A partial eclipse was visible for parts of Europe, North Africa, Northeast Africa, West Asia, Central Asia, and South Asia.


      Observation


      A team from the University of Texas observed the total eclipse in Pisa, Italy, mostly studying the solar irradiance with a wavelength below 1 centimeter. At that time, coronagraphs had already allowed coronal observation in the visible light band so it could be observed at any time, not just during total solar eclipses, but instruments allowing millimeter-wave band observations were still lacking. Therefore, it was still necessary to make such observations during a total solar eclipse. Arcetri Observatory in Florence, Italy also made observations.


      In popular culture



      The crucifixion scene in the 1961 film Barabbas was shot during this eclipse.


      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 1961

      =
      A total solar eclipse on February 15.
      A partial lunar eclipse on March 2.
      An annular solar eclipse on August 11.
      A partial lunar eclipse on August 26.


      = Metonic

      =
      Preceded by: Solar eclipse of April 30, 1957
      Followed by: Solar eclipse of December 4, 1964


      = Tzolkinex

      =
      Preceded by: Solar eclipse of January 5, 1954
      Followed by: Solar eclipse of March 28, 1968


      = Half-Saros

      =
      Preceded by: Lunar eclipse of February 11, 1952
      Followed by: Lunar eclipse of February 21, 1970


      = Tritos

      =
      Preceded by: Solar eclipse of March 18, 1950
      Followed by: Solar eclipse of January 16, 1972


      = Solar Saros 120

      =
      Preceded by: Solar eclipse of February 4, 1943
      Followed by: Solar eclipse of February 26, 1979


      = Inex

      =
      Preceded by: Solar eclipse of March 7, 1932
      Followed by: Solar eclipse of January 26, 1990


      = Triad

      =
      Preceded by: Solar eclipse of April 16, 1874
      Followed by: Solar eclipse of December 16, 2047


      = Solar eclipses of 1961–1964

      =
      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 June 10, 1964 and December 4, 1964 occur in the next lunar year eclipse set.


      = Saros 120

      =
      This eclipse is a part of Saros series 120, repeating every 18 years, 11 days, and containing 71 events. The series started with a partial solar eclipse on May 27, 933 AD. It contains annular eclipses from August 11, 1059 through April 26, 1492; hybrid eclipses from May 8, 1510 through June 8, 1564; and total eclipses from June 20, 1582 through March 30, 2033. The series ends at member 71 as a partial eclipse on July 7, 2195. 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 11 at 6 minutes, 24 seconds on September 11, 1113, and the longest duration of totality was produced by member 60 at 2 minutes, 50 seconds on March 9, 1997. 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.


      See also


      List of solar eclipses visible from Russia
      List of solar eclipses visible from Ukraine


      Notes




      References


      Earth visibility chart and eclipse statistics Eclipse Predictions by Fred Espenak, NASA/GSFC
      Google interactive map
      Besselian elements
      Solar eclipse of February 15, 1961 in Russia Archived December 10, 2009, at the Wayback Machine

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