Understanding > Astronomical calculations
This eclipse is the sixth partial eclipse of the XXIst century.
It is only visible from southern South America and from some part of the Antarctica.
To account for differences between the optical center and the center of mass of the Moon, positions of the Moon have been corrected of 0.50" in longitude and -0.25" in latitude.
Ephemeris used to calculate the positions of the Sun and the Earth are SLP98 ephemeris (G. Francou, 1998) developed within the Bureau des longitudes. In the lunar theory the tidal term has been changed from a fit to the observations. This change does not affect the calculation of recent eclipses but is necessary for the calculation of ancient eclipses. In this case the value of the TU-TE difference is selected as a function of the modification made. For this calculation the value of TE-TU was exceptionally forced. For calculating apparent positions we used the following theories: theory of the precession of Lieske, the theory of nutation of Wahr (1981) and the formula for calculating the sidereal time of Aoki (1992).
Julian day : 2454355.0712853568
Characteristics | Values |
---|---|
Right ascension of the Sun : | 11h 17m 31.462s. |
Declination of the Sun : | + 4° 34' 5.39". |
Right ascension of the Moon : | 11h 17m 31.462s. |
Declination of the Moon : | + 3° 23'38.66". |
Equatorial parallax of the Sun : | 8.73". |
Equatorial parallax of the Moon : | 55' 3.74". |
True semi-diameter of the Sun : | 15' 53.18". |
True semi-diameter of the Moon : | 15' 0.20". |
General circumstances of the eclipse
Magnitude : 0.7509
Circumstances | UT | Longitude | Latitude |
---|---|---|---|
Beginning of the general eclipse | the 11 at 10h25.7m | + 65°45.9' | -17°29.8' |
Maximum of the eclipse | the 11 at 12h31.3m | + 90°15.2' | -61° 9.8' |
End of the general eclipse | the 11 at 14h36,5m | - 33°34.8' | -74°17.8' |
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