[Total Solar Eclipse: 2013]
The 2002 Eclipse:
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The Total Solar Eclipse of 4 December 2002. The narrow 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 4 seconds. This occurs in the Indian Ocean. On either side of that point, the duration is less. To the West of greatest eclipse the eclipse will be total before local noon; East of it, totality will be seen after local noon. The umbra is widest around the time of greatest eclipse as the Earth is bulging out towards the Moon in that region.
The area on either side of the path of totality (in pale blue) will provide a partial eclipse, the magnitude decreasing with distance from the path of totality. Beyond that no eclipse is visible. The sub-solar point is the location where the Sun is overhead at the time of greatest eclipse; this point is well South of the equator in December. The parts in red are the regions where the eclipse occurs during sunrise (left) or sunset (right).
The path of totality begins in the southern Atlantic Ocean, crosses southern Africa, the Indian Ocean, ending in southern Australia. The umbra takes 3 hours 21 minutes to traverse its entire path.
The path of totality is the pair of black lines moving across Africa from left to right. The fainter red path is the total eclipse of June 2001.
In this part of the path the eclipse occurs before local noon. The path travels across Angola, part of northern Namibia, Botswana, southern Zimbabwe, northern South Africa, and Mozambique. It takes about 30 minutes for the umbra to cross Africa.
The ellipses and circles are the positions of the umbra at ten minute intervals (all in Universal Time which is essentially GMT). For each position, the accompanying boxes contain the time, the duration of totality, and the altitude of the Sun. The umbra becomes more circular from left to right as the meeting between the Earth and the umbra becomes more perpendicular.
The path of totality is the pair of red lines moving across Botswana from left to right.
The red ellipses are the positions of the umbra at two minute intervals. For each position, the accompanying boxes contain the time, the duration of totality, and the altitude of the Sun.
The two outer black lines are the path of totality and the middle line is the centre line. The maximum duration of totality is found along the centre line.
The jagged pair of lines at the upper right is the border between Botswana and Zimbabwe. The thin black lines are the roads in Botswana. The long straight road by itself on the lower right of the map is the Kasane to Nata road. The eclipse site was at the intersection of this road with the centre line of the umbra.
|Location||Kasane to Nata Road, Botswana|
|Latitude||19° 09' 15.6" S|
|Longitude||25° 45' 48.8" E|
|Distance from Centre Line||600 m|
|1st Contact (UT + 2)||07:07|
|Path Width||70 km|
|Major Axis||108 km|
|Minor Axis||62 km|
|Direction of Shadow||308°|
|Umbral Velocity||0.48 km/s|
|Position Angle: 2nd Contact||116°|
|Position Angle: 3rd Contact||296°|
|Saros Details||142 (22 / 72)|
The Location, Latitude, Longitude and Altitude (in metres) are for the observation site. The latter three figures were measured on a Garmin GPS 12 Personal Navigator.
The Distance from Centre Line was estimated using a map with the path of totality plotted from Fred Espenak data.
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. The times are in local time which, for this eclipse, is UT + 2 (GMT plus two hours).
The Duration of the eclipse at the observation site was 1 minute 14 seconds.
The Path Width is the width of the path of totality. The umbra itself is elliptical in shape. The Major Axis is the longest axis of the umbra; the Minor Axis is the shorter axis. The umbra at the observation site was 108km long and 62km wide and produced a path width of 70km. The path width was small enough to make the eclipse brighter than average.
The Direction of the Shadow indicates that the umbra approached the observation site from the North West. The Umbral Velocity was the speed of the Moon's shadow (480 metres per second) at the observation site. This and the umbral width determines the duration of the total eclipse.
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 Position Angles indicate the exact position of the Sun's disk where the Moon covers and uncovers the Sun at the beginning and end of totality.
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 142. It is the 22nd eclipse out of a total of 72 in the series (28 partial, 43 total and one hybrid). The first eclipse of the series was a small partial eclipse in the southern polar regions on 17 April 1624 and the last will occur on 5 January 2904 at the northern pole. On 28 May 2291, this series will produce a total eclipse 6m 34s long. Saros 142 will last for 1280 years.
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 -0.30204. This means that the shadow passes South of the Earth's centre, about a third of the way to the edge of the Earth. This, combined with the fact that in December, the Southern Hemisphere is tilted towards the Sun, produces an eclipse in the Southern Temperate 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 1.0181 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. It is a smallish figure so the total eclipse is not of long duration. If this figure was less than one a total eclipse could not occur because the Moon would appear smaller than the Sun. The Obscuration determines how much larger the Moon's apparent area is than the Sun's.