Solar eclipse of August 30, 1905


A total solar eclipse occurred at the Moon's ascending node of orbit on Wednesday, August 30, 1905, with a magnitude of 1.0477. 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 1.9 days before perigee, the Moon's apparent diameter was larger.
Totality was visible from Canada, Newfoundland Colony, Spain, French Algeria, French Tunisia, Ottoman Tripolitania include the capital Tripoli, Egypt, Ottoman Empire including Mecca, Emirate of Jabal Shammar, Aden Protectorate, and Muscat and Oman. A partial eclipse was visible for parts of Eastern North America, Europe, Northern Africa, Central Africa, and West Asia.
This eclipse was observed from Alcalà de Xivert in Spain. It was also observed by members of the British Astronomical Association from various locations.

Observations

Teams of the United States Naval Observatory observed the eclipse from three different locations. Two were near the centerline of the path of totality: Daroca, Spain, at an altitude of, and Guelma, French Algeria, at an altitude of. The third was near the southern edge of the path of totality, at Porta Coeli Charterhouse, Valencia, Spain, at an altitude of. The leader and some team members departed from New York City by ship on July 3 and arrived at Grado, Asturias, a Spanish port on the northern coast, on July 20, while other team members had already arrived there in advance. The weather was clear at all three locations, and the observations were successful. The team took images of the corona and observed the spectrum.

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
First Penumbral External Contact1905 August 30 at 10:37:28.1 UTC
First Umbral External Contact1905 August 30 at 11:40:16.4 UTC
First Central Line1905 August 30 at 11:41:22.2 UTC
First Umbral Internal Contact1905 August 30 at 11:42:28.2 UTC
Equatorial Conjunction1905 August 30 at 12:50:08.0 UTC
Greatest Duration1905 August 30 at 13:07:15.3 UTC
Greatest Eclipse1905 August 30 at 13:07:25.8 UTC
Ecliptic Conjunction1905 August 30 at 13:13:19.1 UTC
Last Umbral Internal Contact1905 August 30 at 14:32:33.8 UTC
Last Central Line1905 August 30 at 14:33:41.6 UTC
Last Umbral External Contact1905 August 30 at 14:34:49.2 UTC
Last Penumbral External Contact1905 August 30 at 15:37:27.7 UTC

ParameterValue
Eclipse Magnitude1.04766
Eclipse Obscuration1.09759
Gamma0.57084
Sun Right Ascension10h32m53.1s
Sun Declination+09°08'33.0"
Sun Semi-Diameter15'50.7"
Sun Equatorial Horizontal Parallax08.7"
Moon Right Ascension10h33m31.6s
Moon Declination+09°41'25.8"
Moon Semi-Diameter16'22.5"
Moon Equatorial Horizontal Parallax1°00'05.8"
ΔT4.8 s

Eclipse season

This eclipse is part of an eclipse season, a period, roughly every six months, when eclipses occur. Only two eclipse seasons occur each year, and each season lasts about 35 days and repeats just short of six months 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.
August 15
Descending node 		August 30
Ascending node
Partial lunar eclipse
Lunar Saros 117		Total solar eclipse
Solar Saros 143

Related eclipses

Eclipses in 1905

Saros 143

Metonic series

Tritos series

Inex series