Annularity was visible in Saudi Arabia, Qatar, United Arab Emirates, Oman, southern India, Sri Lanka, Malaysia, Indonesia, Singapore, the Northern Mariana Islands, and Guam. A partial eclipse was visible for parts of East Africa, Asia, and northern Australia.
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.[9]
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.
Astronomers Without Borders collected eclipse glasses for redistribution to Latin America and Asia for their 2019 eclipses from the Solar eclipse of August 21, 2017.[10]
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.[11]
The longest duration of annularity was produced by member 25 at 6 minutes, 56 seconds on May 9, 1641, and the longest duration of totality will be produced by member 61 at 2 minutes, 14 seconds on June 8, 2290. All eclipses in this series occur at the Moon''s descending node of orbit.[12]
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.
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.
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