A total solar eclipse occurred at the Moon's ascending node of orbit on Monday, May 9, 1910,[1] [2] [3] [4] with a magnitude of 1.06. 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 10 hours after perigee (on May 8, 1910, at 19:20 UTC), the Moon's apparent diameter was larger.[5]
Totality was visible from part of Wilkes Land in Antarctica and Tasmania in Australia. A partial eclipse was visible for parts of Antarctica, Australia, and Southeast Asia.
Except for Antarctica, the only land covered by the path of totality was the central and southern parts of Tasmania. The eclipse occurred in winter when Tasmania is usually rainy with bad observation conditions. However, British pioneer aviator Francis McClean still organized and led a team to Port Davey on the southwestern coast of Tasmania, but in the end failed to make observations due to rainy weather. In addition, observations on Bruny Island, southeast of Tasmania also failed due to the weather. Zeehan and Strahan on the west coast of Tasmania were clear during the partial phase, but had poor weather during the total phase. Queenstown, located slightly inland, was one of the few places where the entire process of the eclipse was seen. Some observers took images of the corona there.[6] [7]
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.[8]
| First Penumbral External Contact | 1910 May 09 at 03:38:20.0 UTC | |
| Equatorial Conjunction | 1910 May 09 at 05:03:20.8 UTC | |
| First Umbral External Contact | 1910 May 09 at 05:04:55.4 UTC | |
| First Central Line | 1910 May 09 at 05:09:08.5 UTC | |
| First Umbral Internal Contact | 1910 May 09 at 05:13:54.4 UTC | |
| Ecliptic Conjunction | 1910 May 09 at 05:32:47.7 UTC | |
| Greatest Eclipse | 1910 May 09 at 05:42:12.6 UTC | |
| Greatest Duration | 1910 May 09 at 05:42:47.5 UTC | |
| Last Umbral Internal Contact | 1910 May 09 at 06:10:56.2 UTC | |
| Last Central Line | 1910 May 09 at 06:15:41.3 UTC | |
| Last Umbral External Contact | 1910 May 09 at 06:19:53.6 UTC | |
| Last Penumbral External Contact | 1910 May 09 at 07:46:22.1 UTC |
| Eclipse Magnitude | 1.06000 | |
| Eclipse Obscuration | 1.12360 | |
| Gamma | –0.94372 | |
| Sun Right Ascension | 03h01m00.1s | |
| Sun Declination | +17°07'25.6" | |
| Sun Semi-Diameter | 15'50.4" | |
| Sun Equatorial Horizontal Parallax | 08.7" | |
| Moon Right Ascension | 03h02m29.5s | |
| Moon Declination | +16°13'49.4" | |
| Moon Semi-Diameter | 16'42.2" | |
| Moon Equatorial Horizontal Parallax | 1°01'18.1" | |
| ΔT | 10.8 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. The first and last eclipse in this sequence is separated by one synodic month.