Solar eclipse of October 3, 2005

Solar eclipse of October 3, 2005

Annular from Spain
Map
Type of eclipse
Nature Annular
Gamma 0.3306
Magnitude 0.9576
Maximum eclipse
Duration 272 sec (4 m 32 s)
Coordinates 12°54′N 28°42′E / 12.9°N 28.7°E / 12.9; 28.7
Max. width of band 162 km (101 mi)
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


Degania A, Israel : Partial

Solar eclipses 2004-2008

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
SarosMap SarosMap
119 2004 April 19

Partial (south)		 124 2004 October 14

Partial (north)
129 2005 April 8

Hybrid		 134

Annular from Spain		 2005 October 3

Annular
139

Total from Side, Turkey		 2006 March 29

Total		 144

Partial from São Paulo, Brazil		 2006 September 22

Annular
149 2007 March 19

Partial (north)		 154 2007 September 11

Partial (south)

Saros 134

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]

Metonic cycle

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

  1. 1 2 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

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