A total solar eclipse occurred at the Moon's ascending node of orbit between Monday, September 10, and Tuesday, September 11, 1923,[1] with a magnitude of 1.043. 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 2.1 days before perigee (on September 12, 1923, at 23:20 UTC), the Moon's apparent diameter was larger.[2]
The path of totality started at the southeastern tip of Shiashkotan in Japan (now in Russia) on September 11, and crossed the Pacific Ocean, southwestern California including the whole Channel Islands, northwestern and northern Mexico, Yucatan Peninsula, British Honduras (today's Belize), Swan Islands, Honduras, and Serranilla Bank and Bajo Nuevo in Colombia on September 10. The eclipse was over 90% in Los Angeles, San Diego, and Santa Barbara on the Southern California coast. A partial eclipse was visible for parts of far east Russia, North America, Central America, the Caribbean, and northern South America.
At Santa Catalina Island, off the coast of California, a large group of scientists gathered to observe the eclipse were foiled by clouds, with the Los Angeles Times saying that "nothing of the eclipse was seen save two glimpses that showed the crescent of the sun, a sickly, white watermelon rind with the wavering black moon and a few rags of black clouds fast blotting out the white light":
All day the scientists from Yerkes Observatory of the University of Chicago, from the University of Wisconsin, from Dearborn University, from Drake University and Carleton College, had rehearsed and rehearsed to the counting of the seconds and there they stood now while the moon covered the sun and the world was dark and still, and though the counter counted there was no possibility of taking pictures; no chance of seeing anything but that gray, blue, purple shadow moving across the sky.In Bakersfield, where the last eclipse of the Sun had taken place 123 years earlier, many watched the eclipse from streets, chickens were confused, and "all the astronomical apparatus of Bakersfield" was trained on the eclipse. In New York City the eclipse, while partial, was viewed successfully; in the area of totality, it was "studied by astronomers who [were] depending on it to help them test out Einstein's famous theory of relativity and whether light rays are bent by the attraction of gravity".
Even as late as 11:30 when the eclipse began, the scientists had hopes. They had come thousands of miles, had worked hard, had spent much money, all for a few minutes of clear sky. They had worked in the sweltering sun for weeks and weeks 1302 feet above the sea. There had not been one moment of one day that was not flooded with sunshine. "And surely," said Prof. Edwin Frost of the University of Chicago, "surely we will have these few minutes today."
A team from the University of Arizona took images of the corona in Puerto Libertad, Sonora, Mexico, on the east coast of the Gulf of California.[3] A team from Sproul Observatory observed it in Yerbanís in eastern Durango state, Mexico.[4]
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.[5]
| First Penumbral External Contact | 1923 September 10 at 18:14:41.7 UTC | |
| First Umbral External Contact | 1923 September 10 at 19:16:26.6 UTC | |
| First Central Line | 1923 September 10 at 19:17:19.8 UTC | |
| First Umbral Internal Contact | 1923 September 10 at 19:18:13.2 UTC | |
| Equatorial Conjunction | 1923 September 10 at 20:30:34.7 UTC | |
| Greatest Eclipse | 1923 September 10 at 20:47:29.1 UTC | |
| Greatest Duration | 1923 September 10 at 20:47:52.3 UTC | |
| Ecliptic Conjunction | 1923 September 10 at 20:52:49.7 UTC | |
| Last Umbral Internal Contact | 1923 September 10 at 22:16:55.2 UTC | |
| Last Central Line | 1923 September 10 at 22:17:50.4 UTC | |
| Last Umbral External Contact | 1923 September 10 at 22:18:45.5 UTC | |
| Last Penumbral External Contact | 1923 September 10 at 23:20:20.4 UTC |
| Eclipse Magnitude | 1.04302 | |
| Eclipse Obscuration | 1.08790 | |
| Gamma | 0.51493 | |
| Sun Right Ascension | 11h12m32.0s | |
| Sun Declination | +05°05'47.3" | |
| Sun Semi-Diameter | 15'53.2" | |
| Sun Equatorial Horizontal Parallax | 08.7" | |
| Moon Right Ascension | 11h13m08.8s | |
| Moon Declination | +05°35'11.3" | |
| Moon Semi-Diameter | 16'20.1" | |
| Moon Equatorial Horizontal Parallax | 0°59'57.1" | |
| ΔT | 23.3 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.