A total solar eclipse occurred at the Moon's ascending node of orbit between Thursday, June 17 and Friday, June 18, 1909,[1] [2] [3] [4] with a magnitude of 1.0065. It was a hybrid event, with only a fraction of its path as total, and longer sections at the start and end as an annular eclipse. 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. The Moon's apparent diameter was near the average diameter because it occurred 5.4 days after perigee (on June 12, 1909, at 16:00 UTC) and 7.5 days before apogee (on June 25, 1909, at 12:00 UTC).[5]
The path of totality crossed central Russia, the Arctic Ocean, northeastern Ellesmere Island in Canada, Greenland, and annularity crossed southern Siberia in Russia (now in northeastern Kazakhstan and southern Russia) and southern Greenland. A partial eclipse was visible for parts of East Asia and northern North America.
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.[6]
| First Penumbral External Contact | 1909 June 17 at 21:00:24.0 UTC | |
| First Umbral External Contact | 1909 June 17 at 22:30:16.6 UTC | |
| First Central Line | 1909 June 17 at 22:30:18.7 UTC | |
| First Umbral Internal Contact | 1909 June 17 at 22:30:20.9 UTC | |
| Greatest Duration | 1909 June 17 at 23:16:41.2 UTC | |
| Greatest Eclipse | 1909 June 17 at 23:18:38.1 UTC | |
| Ecliptic Conjunction | 1909 June 17 at 23:28:20.1 UTC | |
| Equatorial Conjunction | 1909 June 17 at 23:31:17.2 UTC | |
| Last Umbral Internal Contact | 1909 June 18 at 00:06:44.2 UTC | |
| Last Central Line | 1909 June 18 at 00:06:49.2 UTC | |
| Last Umbral External Contact | 1909 June 18 at 00:06:54.2 UTC | |
| Last Penumbral External Contact | 1909 June 18 at 01:36:52.5 UTC |
| Eclipse Magnitude | 1.00647 | |
| Eclipse Obscuration | 1.01299 | |
| Gamma | 0.89568 | |
| Sun Right Ascension | 05h42m52.5s | |
| Sun Declination | +23°23'35.6" | |
| Sun Semi-Diameter | 15'44.3" | |
| Sun Equatorial Horizontal Parallax | 08.7" | |
| Moon Right Ascension | 05h42m23.6s | |
| Moon Declination | +24°14'45.8" | |
| Moon Semi-Diameter | 15'44.1" | |
| Moon Equatorial Horizontal Parallax | 0°57'44.9" | |
| ΔT | 9.7 s |
See also: Eclipse cycle. 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.