Total eclipse
A total solar eclipse occurred at the Moon's descending node of orbit on Tuesday, June 30, 1992, with a magnitude of 1.0592. 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 1.5 days before perigee (on July 2, 1992, at 1:30 UTC), the Moon's apparent diameter was larger.
Totality was visible in southeastern Uruguay and southern tip of Rio Grande do Sul, Brazil. A partial eclipse was visible for parts of central South America, West Africa, Central Africa, and Southern Africa.
Observations.
The path of totality was mostly on the sea and covered very little land. From the only land covered by it in southeasern Uruguay and southern tip of Brazil, totality occurred shortly after sunrise, with the solar zenith angle less than 3°. Observation from an airplane over the middle of South Atlantic Ocean, near the location of maximum eclipse, could offer a duration of totality of up to 10 minutes with the guarantee of clear weather. However, due to the limitations in the cruising capabilities and the economic cost, a feasible flight plan was to see 5 to 6 minutes of totality on the airplane. 48 people from the United States, Canada, Brazil, Germany, Japan and Great Britain boarded a VASP airline DC-10 plane, departing from Rio de Janeiro, Brazil, flying over the South Atlantic Ocean and returning to Rio de Janeiro. The passengers got off and the captain flew the airplane back to São Paulo. Although adjustment in the flying speed had to be made according to the take-off time and wind speed, the pilot flew the airplane into Moon's umbra within 1 second of the predicted time, and the passengers on board successfully saw the total eclipse. Accidentally, one of the ground support personnel did not exit the airplane before takeoff, and she also saw the eclipse. The pilots were also attracted by the eclipse, still watching the moon shadow moving into the distance and forgetting to fly the airplane back return even minutes after the third contact (the end of the total phase). The captain described this as the most unusual flight he ever commanded. VASP airline also provided a Boeing 737 plane to the Rio de Janeiro Planetarium. Planetarium staff, of their astronomy club, local dignitaries, politicians and celebrities were also invited.
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 1990–1992.
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.
Saros 146.
This eclipse is a part of Saros series 146, repeating every 18 years, 11 days, and containing 76 events. The series started with a partial solar eclipse on September 19, 1541. It contains total eclipses from May 29, 1938 through October 7, 2154; hybrid eclipses from October 17, 2172 through November 20, 2226; and annular eclipses from November 30, 2244 through August 10, 2659. The series ends at member 76 as a partial eclipse on December 29, 2893. 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 totality was produced by member 26 at 5 minutes, 21 seconds on June 30, 1992, and the longest duration of annularity will be produced by member 63 at 3 minutes, 30 seconds on August 10, 2659. 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.
The partial solar eclipses on December 18, 2188 (part of Saros 164) and November 18, 2199 (part of Saros 165) are also a part of this series but are not included in the table below.
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.
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