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Solar eclipse of June 8, 1937

Total eclipse

Summary

Total eclipse

FieldValue
imageFile:Kanton total eclipse June8, 1937.jpg
captionThe solar eclipse as viewed from Kanton Island.
previousSolar eclipse of December 13, 1936
nextSolar eclipse of December 2, 1937

A total solar eclipse occurred at the Moon's descending node of orbit between Tuesday, June 8 and Wednesday, June 9, 1937, 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 about 16 hours after perigee (on June 8, 1937, at 4:30 UTC), the Moon's apparent diameter was larger.

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."

Observations

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.

Eclipse details

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.

EventTime (UTC)
First Penumbral External Contact1937 June 8 at 18:04:51.1 UTC
First Umbral External Contact1937 June 8 at 18:59:01.4 UTC
First Central Line1937 June 8 at 19:00:34.9 UTC
First Umbral Internal Contact1937 June 8 at 19:02:08.4 UTC
First Penumbral Internal Contact1937 June 8 at 19:58:44.5 UTC
Greatest Duration1937 June 8 at 20:40:34.6 UTC
Greatest Eclipse1937 June 8 at 20:41:01.5 UTC
Equatorial Conjunction1937 June 8 at 20:41:09.6 UTC
Ecliptic Conjunction1937 June 8 at 20:43:19.5 UTC
Last Penumbral Internal Contact1937 June 8 at 21:23:18.0 UTC
Last Umbral Internal Contact1937 June 8 at 22:19:55.6 UTC
Last Central Line1937 June 8 at 22:21:28.3 UTC
Last Umbral External Contact1937 June 8 at 22:23:00.9 UTC
Last Penumbral External Contact1937 June 8 at 23:17:13.7 UTC
ParameterValue
Eclipse Magnitude1.07513
Eclipse Obscuration1.15590
Gamma−0.22532
Sun Right Ascension05h06m06.4s
Sun Declination+22°52'06.5"
Sun Semi-Diameter15'45.2"
Sun Equatorial Horizontal Parallax08.7"
Moon Right Ascension05h06m06.1s
Moon Declination+22°38'22.0"
Moon Semi-Diameter16'39.4"
Moon Equatorial Horizontal Parallax1°01'08.0"
ΔT23.9 s

Eclipse season

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.

May 25
Ascending node (full moon)June 8
Descending node (new moon)
[[File:Lunar eclipse chart close-1937May25.png200px]][[File:SE1937Jun08T.png200px]]
Penumbral lunar eclipse
Lunar Saros 110Total solar eclipse
Solar Saros 136

Notes

| access-date = 2023-10-17 | access-date = 2023-10-17 | access-date = 2023-10-17 | access-date = 2023-10-17

References

References

  1. "June 8, 1937 Total Solar Eclipse". timeanddate.
  2. "Moon Distances for London, United Kingdom, England". timeanddate.
  3. Mitchell, S. A.. (February 1938). "The Total Eclipse Observed on Canton Island". Publications of the Astronomical Society of the Pacific.
  4. Michie, C. B.. (1 December 1938). "Report of the New Zealand Total Solar Eclipse Expedition to Canton Island, 1937 June 8". Monthly Notices of the Royal Astronomical Society.
  5. "Total Solar Eclipse of 1937 Jun 08". EclipseWise.com.
Wikipedia Source

This article was imported from Wikipedia and is available under the Creative Commons Attribution-ShareAlike 4.0 License. Content has been adapted to SurfDoc format. Original contributors can be found on the article history page.

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