[Total Solar Eclipse: 2012]
The 1995 Eclipse:
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The Total Solar Eclipse of 24 October 1995. The dark blue region is the path of totality (also known as the umbra).
The umbra shadow travels from west to east (left to right on the map). At the point of greatest eclipse, totality is at local midday. The duration of totality at greatest eclipse is 2 minutes 10 seconds. This occurs in the South China Sea. On either side of that point, the duration is less. To the West of greatest eclipse the eclipse will be total before local noon; to the East, the eclipse will be total after local noon. The umbra is widest around the time of greatest eclipse as the surface of the Earth is bulging out towards the Moon in that region.
The area on either side of the path of totality (in pale blue) provides a partial eclipse, the magnitude decreasing with distance from the path of totality. Outside the blue region no eclipse is visible. The sub-solar point is the location where the Sun is overhead at the time of greatest eclipse. The overhead Sun is South of the equator during October. The red regions are the areas where the eclipse occurs during sunrise (left) or sunset (right).
The path of totality begins in Asia (central Iran), crosses South Asia (including the Bay of Bengal), South East Asia, the South China Sea and the Pacific Ocean. The umbra takes 3 hours 20 minutes to traverse its entire path.
The Moon is further from the Earth than average making the path of totality narrower than average and the duration of totality very short.
The path of totality is the pair of dark lines in the centre, moving across Asia from left to right.
In this part of the path the eclipse occurs before local noon. The path travels across Iran, Afghanistan, Pakistan, northern India, the extreme south of Bangladesh, Burma, Thailand, Cambodia and Vietnam. It takes about 1 hour 30 minutes for the umbra to cross this land area.
The circlular regions are the positions of the umbra at ten minute intervals.
The two black lines shaded in gray are the path of totality.
The circlular regions are the positions of the umbra at five minute intervals. Under each one is the duration of totality at the point. The umbra becomes less circular from left to right as the meeting between the Earth and the umbra becomes less perpendicular.
The eclipse site was along the centre of the path of totality approximately 35km south of the city of Agra.
This is the sky during totality close to our observation location.
The Sun is very low as the eclipse was early in the morning. Venus was the only planet visible.
|Location||Khanua, northern India|
|Latitude||27° 02.0' N|
|Longitude||77° 32.5' W|
|Distance from Centre Line||< 1 km|
|1st Contact (UT + 5.5)||07:25|
|Path Width||43 km|
|Umbral Velocity||1.7 km/s|
|Saros Details||143 (23 / 73)|
The Distance from Centre Line was a few hundred metres.
First Contact is the beginning of the eclipse when the first "bite" appears on the Sun's disk; it is the beginning of the partial phase. Second Contact is the beginning of totality. Third Contact is the end of totality. Fourth Contact is the end of the partial eclipse - at this time we had left the observation site and were talking to the villagers. The times are in local time which, for this eclipse, is UT + 5.5 (GMT plus five and a half hours).
The Duration of the eclipse at the observation site was 0 minutes 54 seconds.
The Path Width is the width of the path of totality. This was quite narrow for this eclipse, at 43km. The small size of the umbra produced a fairly bright totality and a short duration.
The Umbral Velocity is the speed of the Moon's shadow which was 1.7 kilometres per second at the observation site. This high speed and the small width of the umbra produced a total eclipse of short duration.
The Sun's Altitude is measured from the horizon; the Azimuth is the direction of the Sun measured clockwise from North. The figures are for mid-eclipse.
The Saros is a collection of eclipses belonging to a series. Each member of the series is followed by a similar eclipse approximately 18 years, 11 days and 8 hours later. This eclipse is a member of Saros number 143. It is the 23rd eclipse out a series of 73.
Saros 143 began with a small partial eclipse in high northern latitudes on 7 March 1617. There followed nine further partial eclipses. The first total eclipse took place with the 11th eclipse of the series on 24 June 1797 (duration 2m 47s). The subsequent eclipses had longer durations until the longest total eclipse of the series occurred on 19 August 1887 (the 16th eclipse, duration 3m 50s).
After this the duration of totality decreased as the Moon was moving away from the Earth for each successive eclipse. This eclipse (the 22nd) is the final purely total eclipse of the series (maximum duration 2m 10s). The next four eclipses will be hybrid - that is annular over part of the path and total over the rest of the path. The first purely annular eclipse will be the 27th on 16 December 2085, with a duration of 0m 19s. The duration of the annular eclispes will increase until the 51st eclipse (6 September 2518, 4m 54s). The 52nd eclipse will be the final annular eclipse of the series. There will then follow 20 partial eclipses of decreasing magnitude in the southern polar regions until the final eclipse of Saros 143 on 23 April 2897. The series will end 1280 years after it began.
Gamma determines how the Moon's shadow, if extended, would pass through the Earth. A Gamma of zero implies that the shadow would pass through the exact centre of the Earth. A Gamma of greater than 1 misses the Earth and no total eclipse would occur. A positive Gamma passes North of the Earth's centre; a negative Gamma passes South of the Earth's centre. The value of Gamma for this eclipse is 0.3517. This means that the shadow passes North of the Earth's centre, about a third of the way to the edge of the Earth. This, combined with the fact that in October, the Southern Hemisphere is tilted slightly towards the Sun, produces an eclipse in the Northern Tropical Zone.
The Diameter Ratio determines how much bigger the Moon's apparent radius is than the Sun's. In this case, the Moon's radius is 1.012 that of the Sun's. A total eclipse can only occur if this figure is greater than 1. The Moon would then appear larger than the Sun and could cover it completely. If this figure was less than one a total eclipse could not occur because the Moon would appear smaller than the Sun. According to this figure, the Moon is a mere 1.2% larger than the Sun. This produced an eclipse where the inner levels of the Sun's atmosphere could be seen.