An annular solar eclipse occurred at the Moon's ascending node of orbit on Sunday, February 14, 1915, with a magnitude of 0.9789. 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. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide. The Moon's apparent diameter was near the average diameter because it occurred 6.7 days after perigee (on February 7, 1915, at 13:20 UTC) and 7.1 days before apogee (on February 21, 1915, at 5:50 UTC).
Annularity was visible from Australia, Papua in Dutch East Indies (today's Indonesia), German New Guinea (now belonging to Papua New Guinea), and the South Seas Mandate of Japan (the parts now belonging to FS Micronesia and Marshall Islands, including Palikir). A partial eclipse was visible for parts of Antarctica, Australia, Oceania, and Southeast Asia.
The eclipse occurred on February 14 in the whole path of annularity, and also most of the places where a partial eclipse was visible. It was on February 13 only in a small part east of the International Date Line.
The date of this eclipse visible from Asia, February 14, was also Lunar New Year, celebrated in multiple countries.
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.
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.