Solar eclipse of October 3, 2005

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Solar eclipse of October 3, 2005
Ecl-ann.jpg
Annular from Spain
SE2005Oct03A.png
Map
Type of eclipse
Nature Annular
Gamma 0.3306
Magnitude 0.9576
Maximum eclipse
Duration 4m 32s
Coordinates 12.9N 28.7E
Max. width of band 162 km
Times (UTC)
(P1) Partial begin 3:53:56
(U1) Total begin 18:40:59
Greatest eclipse 10:32:47
(U4) Total end 1:22:35
(P4) Partial end 24:27:52
References
Saros 134 (43 of 71)
Catalog # (SE5000) 9520
Satellite image of the eclipse over East Africa. Red dots show where fires were burning in vegetated areas.

An annular solar eclipse occurred on 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.

It was visible from a narrow corridor through the Iberian peninsula and Africa. A partial eclipse was seen from the much broader path of the Moon's penumbra, including all of Europe, Africa and southwestern Asia.

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.[1]

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.[1] The theoretical maximum duration for a modern solar eclipse is 7 minutes, 32 seconds.[2]

The motion of the shadow was supersonic and it generated gravity waves that were detectable as disturbances in the ionosphere. These gravity waves originate in the thermosphere at an altitude of about 180 km. Because of the obscuration of solar radiation, the ionization level dropped by 70% during the eclipse.[3][4] The eclipse caused a 1–1.4 K drop in the temperature of the ionosphere.[5]

Images[edit]

20051003sequence.jpg
Degania A, Israel : Partial

Related eclipses[edit]

Solar eclipses 2004-2008[edit]

Each member in a semester series of solar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternating nodes of the Moon's orbit.

Solar eclipse series sets from 2004–2007
Ascending node   Descending node
Saros Map Saros Map
119 2004 April 19
SE2004Apr19P.png
Partial (south)
124 2004 October 14
SE2004Oct14P.png
Partial (north)
129 2005 April 8
SE2005Apr08H.png
Hybrid
134
Ecl-ann.jpg
Annular from Spain
2005 October 3
SE2005Oct03A.png
Annular
139
Diamondring-eclipse-March03-29-2006.jpg
Totality from Side, Turkey
2006 March 29
SE2006Mar29T.png
Total
144
Helder da Rocha - Partial solar eclipse (by-sa).jpg
Partial from São Paulo, Brazil
2006 September 22
SE2006Sep22A.png
Annular
149 2007 March 19
SE2007Mar19P.png
Partial (north)
154 2007 September 11
SE2007Sep11P.png
Partial (south)

Saros 134[edit]

It is a part of Saros cycle 134, repeating every 18 years, 11 days, containing 71 events. The series started with partial solar eclipse on June 22, 1248. It contains total eclipses from October 9, 1428 through December 24, 1554 and hybrid eclipses from January 3, 1573 through June 27, 1843, and annular eclipses from July 8, 1861 through May 21, 2384. The series ends at member 71 as a partial eclipse on August 6, 2510. The longest duration of totality was 1 minutes, 30 seconds on October 9, 1428.[6]

Series members 38-48 occur between 1901 and 2100:

38 39 40
SE1915Aug10A.png
August 10, 1915
SE1933Aug21A.png
August 21, 1933
SE1951Sep01A.png
September 1, 1951
41 42 43
SE1969Sep11A.png
September 11, 1969
SE1987Sep23A.png
September 23, 1987
SE2005Oct03A.png
October 3, 2005
44 45 46
SE2023Oct14A.png
October 14, 2023
SE2041Oct25A.png
October 25, 2041
SE2059Nov05A.png
November 5, 2059
47 48
SE2077Nov15A.png
November 15, 2077
SE2095Nov27A.png
November 27, 2095

Metonic cycle[edit]

The metonic series repeats eclipses every 19 years (6939.69 days), lasting about 5 cycles. Eclipses occur in nearly the same calendar date. In addition the octon subseries repeats 1/5 of that or every 3.8 years (1387.94 days).

Notes[edit]

  1. ^ a b Espenak, Fred. "Annular Solar Eclipse of 2005 October 03". NASA/GSFC. Retrieved 2009-09-23. 
  2. ^ Meeus, J. (December 2003). "The maximum possible duration of a total solar eclipse". Journal of the British Astronomical Association 113 (6): 343–348. Bibcode:2003JBAA..113..343M. 
  3. ^ Jakowski, N.; et al. (April 2008). "Ionospheric behavior over Europe during the solar eclipse of 3 October 2005". Journal of Atmospheric and Solar-Terrestrial Physics 70 (6): 836–853. Bibcode:2008JASTP..70..836J. doi:10.1016/j.jastp.2007.02.016. 
  4. ^ Šauli, P.; et al. (December 2007). "Acoustic–gravity waves during solar eclipses: Detection and characterization using wavelet transforms". Journal of Atmospheric and Solar-Terrestrial Physics 69 (17–18): 2465–2484. Bibcode:2007JASTP..69.2465S. doi:10.1016/j.jastp.2007.06.012. 
  5. ^ Burmaka, V. P.; et al. (2007). "Tropospheric-ionospheric effects of the 3 October 2005 partial solar eclipse in Kharkiv". Kosmichna Nauka i Tekhnologiya 13 (6): 74–86. Bibcode:2007KosNT..13f..74B. 
  6. ^ http://eclipse.gsfc.nasa.gov/SEsaros/SEsaros134.html

References[edit]

Photos: