Solar eclipse of October 3, 2005

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. Occurring only 4.8 days after apogee (September 28, 2005), the Moon's apparent diameter was smaller. 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 Sun was 96% covered in a moderate annular eclipse, lasting 4 minutes and 32 seconds and covering a broad path up to 162 km wide. The next solar eclipse in Africa occurred just 6 months later.

Solar eclipse of October 3, 2005
Annular from Madrid, Spain
Map
Type of eclipse
NatureAnnular
Gamma0.3306
Magnitude0.9576
Maximum eclipse
Duration272 sec (4 m 32 s)
Coordinates12.9°N 28.7°E / 12.9; 28.7
Max. width of band162 km (101 mi)
Times (UTC)
(P1) Partial begin3:53:56
(U1) Total begin18:40:59
Greatest eclipse10:32:47
(U4) Total end1:22:35
(P4) Partial end24:27:52
References
Saros134 (43 of 71)
Catalog # (SE5000)9520
Satellite image of the eclipse over East Africa. Red dots show where fires were burning in vegetated areas.

It was the 43rd eclipse of the 134th Saros cycle, which began with a partial eclipse on June 22, 1248 and will conclude with a partial eclipse on August 6, 2510.

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 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.[2][3] The eclipse caused a 1–1.4 K drop in the temperature of the ionosphere.[4]

Information and details

Eclipse Characteristics

Eclipse Magnitude: 0.95759

Eclipse Obscuration: 0.91698

Gamma: 0.33058

Saros Series: 134th (43 of 71)

Conjunction Times

Greatest Eclipse: 03 Oct 2005 10:31:42.5 UTC (10:32:47.3 TD)

Ecliptic Conjunction: 03 Oct 2005 10:27:52.4 UTC (10:28:57.3 TD)

Equatorial Conjunction: 03 Oct 2005 10:10:42.1 UTC (10:11:46.9 TD)

Geocentric Coordinates of Sun and Moon

Sun right ascension: 12.63

Sun declination: -4.1

Sun diameter: 1918.2 arcseconds

Moon right ascension: 12.64

Moon declination: -3.8

Moon diameter: 1810.4 arcseconds

Geocentric Libration of Moon

Latitude: 3.9 degrees south

Longitude: 0.4 degrees west

Direction: 21.5 (NNE)

Images


Degania A, Israel : Partial

Eclipses of 2005

Tzolkinex

Half-Saros

Tritos

Solar Saros 134

Inex

Solar eclipses 2004–2007

This eclipse is a member of a semester series. An eclipse 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.[5]

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. All eclipses in this series occurs at the Moon’s descending node.[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). All eclipses in this table occur at the Moon's descending node.

Notes
  1. Espenak, Fred. "Annular Solar Eclipse of 2005 October 03". NASA/GSFC. Retrieved 2009-09-23.
  2. 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.
  3. Šauli, P.; et al. (December 2007). "Acoustic–gravity waves during solar eclipses: Detection and characterization using wavelet transforms" (PDF). Journal of Atmospheric and Solar-Terrestrial Physics. 69 (17–18): 2465–2484. Bibcode:2007JASTP..69.2465S. doi:10.1016/j.jastp.2007.06.012.
  4. 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. doi:10.15407/knit2007.06.074.
  5. van Gent, R.H. "Solar- and Lunar-Eclipse Predictions from Antiquity to the Present". A Catalogue of Eclipse Cycles. Utrecht University. Retrieved 6 October 2018.
  6. http://eclipse.gsfc.nasa.gov/SEsaros/SEsaros134.html

References

Photos:

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