A total solar eclipse occurred at the Moon's descending node of orbit between Tuesday, June 8 and Wednesday, June 9, 1937,[1] with a magnitude of 1.0751. 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 only about 16 hours after perigee (on June 8, 1937, at 4:30 UTC), the Moon's apparent diameter was larger.[2]
With a maximum eclipse of 7 minutes and 4.06 seconds, this was the longest total solar eclipse since July 1, 1098, which lasted 7 minutes and 5.34 seconds. A longer total solar eclipse occurred on June 20, 1955.
The path of totality crossed the Pacific Ocean starting in Gilbert and Ellice Islands (now belonging to Tuvalu and Kiribati) on June 9 (Wednesday), and ending at sunset in Peru on June 8 (Tuesday). At sunrise totality lasted 3 minutes, 6.8 seconds and at sunset totality lasted 3 minutes, 5.1 seconds. A partial eclipse was visible for parts of Oceania, Hawaii, southern North America, Central America, the Caribbean, and western South America. American astronomy professor Ethelwynn Rice Beckwith traveled to Peru to see this eclipse, and described the event in detail for the Oberlin Alumnae Magazine in 1937, in an article titled "Three Minutes in Peru."
Scientists from the United States, United Kingdom and New Zealand observed the total eclipse in Canton Island, Phoenix Islands. The American expedition was organized by the National Geographic Society and assisted by the United States Navy. This total solar eclipse was memorable for three reasons: first, the duration of totality was particularly long with the longest point in eastern Pacific exceeding 7 minutes; second, despite being in the tropics, weather was good for all observation sites; third, broadcasts were made through radio before, during and after the eclipse through long distances so people could hear the details.[3] [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 | 1937 June 08 at 18:04:51.1 UTC | |
| First Umbral External Contact | 1937 June 08 at 18:59:01.4 UTC | |
| First Central Line | 1937 June 08 at 19:00:34.9 UTC | |
| First Umbral Internal Contact | 1937 June 08 at 19:02:08.4 UTC | |
| First Penumbral Internal Contact | 1937 June 08 at 19:58:44.5 UTC | |
| Greatest Duration | 1937 June 08 at 20:40:34.6 UTC | |
| Greatest Eclipse | 1937 June 08 at 20:41:01.5 UTC | |
| Equatorial Conjunction | 1937 June 08 at 20:41:09.6 UTC | |
| Ecliptic Conjunction | 1937 June 08 at 20:43:19.5 UTC | |
| Last Penumbral Internal Contact | 1937 June 08 at 21:23:18.0 UTC | |
| Last Umbral Internal Contact | 1937 June 08 at 22:19:55.6 UTC | |
| Last Central Line | 1937 June 08 at 22:21:28.3 UTC | |
| Last Umbral External Contact | 1937 June 08 at 22:23:00.9 UTC | |
| Last Penumbral External Contact | 1937 June 08 at 23:17:13.7 UTC |
| Eclipse Magnitude | 1.07513 | |
| Eclipse Obscuration | 1.15590 | |
| Gamma | −0.22532 | |
| Sun Right Ascension | 05h06m06.4s | |
| Sun Declination | +22°52'06.5" | |
| Sun Semi-Diameter | 15'45.2" | |
| Sun Equatorial Horizontal Parallax | 08.7" | |
| Moon Right Ascension | 05h06m06.1s | |
| Moon Declination | +22°38'22.0" | |
| Moon Semi-Diameter | 16'39.4" | |
| Moon Equatorial Horizontal Parallax | 1°01'08.0" | |
| ΔT | 23.9 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.