The timings of the phases of the overall eclipse worldwide are as follows. In any particular place it would have been seen for a significantly shorter duration as the shadow moved across the Earth:
|Partial eclipse began:||10:33:21 UT|
|Total eclipse began:||11:28:26 UT|
|Maximum eclipse:||13:08:34 UT|
|Total eclipse ended:||14:48:42 UT|
|Partial eclipse ended:||15:43:49 UT|
During this eclipse the Sun was 0.526° in apparent diameter, 1.3% smaller than average. The Moon was just a day past perigee, making it extremely large. At the start and end of the eclipse the Moon was 0.554°, and at maximum eclipse 0.564°, which is 6.2% larger than average; hence it covered the Sun, making this a total eclipse. The statistics page has information on the ranges of the sizes of the Sun and Moon.
This eclipse was used in a historic test of Einstein's General Relativity by Arthur Eddington and his team. In their observations of the eclipse from Principe and Brazil, they confirmed the bending of starlight by gravity as predicted by Einstein in his general theory of relativity. The results were not completely clear-cut, and were not immediately accepted; follow-up expeditions, such as to the 1922 eclipse, helped to confirm that Eddington's observations were in fact correct. See Wikipedia.
This map shows the visibility of the eclipse. The shaded area saw the total solar eclipse; however, near the edges of this area, the eclipse was very short. The bold line shows the centre of the path, where the eclipse lasted longest.
Use the zoom controls to zoom in and out; hover your mouse over any point on the centreline to see the time and duration of the eclipse at that point. You can pan and zoom the map to see detail for any part of the eclipse path.
This map sourced from NASA's Eclipse Web Site shows the visibility of the total solar eclipse. It also shows the broader area in which a partial eclipse was seen. (Click on it for the full-sized version.)
This eclipse season contains 2 eclipses:
This was the 32nd eclipse in solar Saros series 136.The surrounding eclipses in this Saros series are:
|UT Date/time (max)||13:08:34 on 29 May UT||TDT Date/time (max)||13:08:55 on 29 May TDT|
|Saros Series||136||Number in Series||31|
|Penumbral Magnitiude||Central Magnitiude||1.0719|
|Gamma||-0.2955||Path Width (km)||244|
|Delta T||0m21s||Error||± 0m00s (95%)|
|Penumbral Duration||Partial Duration|
|Partial Rating||Total Rating|
|Sun Distance||151650268 km (94.2%)||Moon Distance||359109 km (5.4%)|
|Sun Diameter||0.526°||Moon Diameter||0.554° - 0.564°|
|Perigee||17:14 on 28 May UT||Apogee||06:26 on 10 Jun UT|
|Contact p1||10:33:21 on 29 May UT||Contact p2||12:31:17 on 29 May UT|
|Contact u1||11:28:26 on 29 May UT||Contact u2||11:31:28 on 29 May UT|
|Max eclipse||13:08:34 on 29 May UT|
|Contact u3||14:45:42 on 29 May UT||Contact u4||14:48:42 on 29 May UT|
|Contact p3||13:45:53 on 29 May UT||Contact p4||15:43:49 on 29 May UT|
The Sun and Moon distances are shown in km, and as a percentage of their minimum - maximum distances; hence 0% is the closest possible (Earth's perihelion, or the Moon's closest possible perigee) and 100% is the farthest (aphelion, the farthest apogee). The statistics page has information on the ranges of sizes of the Sun and Moon.
Data last updated: 2015-06-21 22:11:46 UTC.