Solar eclipse of October 3, 2005

An annular solar eclipse occurred at the Moon's descending node of orbit on Monday, October 3, 2005, with a magnitude of 0.958. 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. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide. Occurring about 4.75 days after apogee, the Moon's apparent diameter was smaller.

Visibility

The path of the eclipse began in the North Atlantic ocean at 08:41 universal time (UT). The antumbra reached Madrid, Spain at 08:56 UT, lasting four minutes and eleven seconds and 90% of the Sun was covered by the Moon. The antumbra reached Algiers at 09:05 UT, then passed through Tunisia and Libya before heading southeast through Sudan, Kenya and Somalia. The shadow then moved out over the Indian Ocean until it terminated at sunset, 12:22 UT. The maximum eclipse duration occurred in central Sudan at 10:31:42 UT, where it lasted for 4m 31s when the Sun was 71° above the horizon. The eclipse caused a 1–1.4 K drop in the temperature of the ionosphere. == Eclipse timing ==

Eclipse timing

Places experiencing annular eclipse Places experiencing partial eclipse == Gallery ==

Gallery

File:Eclipse EastAfrica AMO 20051003.jpg|Satellite image showing the Moon's shadow over East Africa Image:Eclipse anular.gif|Animation from Medina del Campo, Spain Image:Solar Eclipse Oct05.jpg|Santa Maria de Lamas, Portugal (9:00 UTC) Image:IMG 1650 zonsverduistering Malta.JPG|Eclipse projection through leaves in St. Julian's, Malta Image:EclipseSoudeur.jpg|Saintes, France (9:36 UTC) Image:Partial Eclipse Chennai Oct2005.jpg|Chennai, India (11:33 UTC) Image:20051003sequence.jpg|Eclipse sequence from Degania A, Israel == Eclipse 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. == Eclipse season ==

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. == Related eclipses ==

Related eclipses

Source: Wikipedia ↗

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