6097 VI/97 Solar and Lunar Eclipses: 1996-2020 F Espenak Bull. Inf. CDS in press ??? ??? 1999 1999 http://sunearth.gsfc.nasa.gov/eclipse/eclipse.html Espenak, F. 1989, Fifty Year Canon of Lunar Eclipses: 1986 - 2035, NASA Reference Publication 1216 Espenak F. 1987. Fifty Year Canon of Solar Eclipses: 1986 - 2035, NASA Reference Publication 1178 (1987) van den Bergh, G. 1955, Periodicity and Variation of Solar (and Lunar) Eclipses, Tjeenk Willink, Haarlem, Netherlands Sun Solar system Solar Eclipses - During the twenty-five year period 1996-2020, some portion of the Moon's shadow will sweep across the Earth a total of fifty-six times. Twenty-one of these events result in partial solar eclipses, seventeen of them are annular eclipses, sixteen more are total eclipses and the remaining two are both annular and total along sections of their narrow paths. Local circumstances at the instant of greatest eclipse1 for every event during this quarter century period are presented in solar.dat. The date and Universal Time of the instant of greatest eclipse are found in the first two columns. The eclipse type is given (T=Total, A=Annular, AT=Annular/Total or P=Partial) along with the Saros series, as defined by van den Bergh (1955). The magnitude of the eclipse is defined as the fraction of the Sun's diameter obscured at greatest eclipse. The latitude and longitude of the umbra are given for the instant of greatest eclipse, along with the Sun's altitude, the width of the path (kilometers) and the duration of totality or annularity. For partial eclipses, the latitude and longitude of the point closest to the umbra's axis at the instant of greatest eclipse are listed. The altitude of the Sun at this location is 0 degrees. Note: Greatest eclipse is defined as the instant when the axis of the Moon's shadow passes closest to the Earth's center. For total eclipses, the instant of greatest eclipse is virtually identical to the instants of greatest magnitude and greatest duration. However, for annular eclipses, the instant of greatest duration may occur at either the time of greatest eclipse or near the sunrise and sunset points of the eclipse path. Lunar Eclipses - During the twenty-five year period 1996-2020, the Moon will swing through some portion of Earth's shadow a total of fifty-eight times. Twenty-three of these events result in penumbral lunar eclipses, twelve of them are partial (umbral) eclipses, twenty-three more are total lunar eclipses. Local circumstances at the instant of greatest eclipse1 for every event during this quarter century period are presented in Table 1. The date and Universal Time of the instant of greatest eclipse are found in the first two columns. The eclipse type is given (T=Total, P=Partial [Umbral], or P=Penumbral) along with the Saros series, as defined by van den Bergh (1955). The penumbral and umbral magnitudes of the eclipse are defined as the fraction of the Moon's diameter obscured by either shadow at greatest eclipse. The partial and total semi-durations of the eclipse along with the Greenwich Siderial Time at midnight, and the Moon's Right Ascension and Declination are listed. The start and end times of the partial eclipse can be calculated by respectively subtracting and adding the partial semi-duration (i.e. - Par. SDur) to the instant of greatest eclipse. Likewise, the start and end times of the total eclipse can be calculated by respectively subtracting and adding the total semi-duration (i.e. - Total SDur) to the instant of greatest eclipse. Note: Greatest eclipse is defined as the instant when the Moon passes closest to the axis of Earth's shadow(s). This marks the instant when the Moon is deepest in Earth's shadow(s).

Year Calendar Year (Gregorian) at instant of Greatest Eclipse yr Month Calendar Month (Gregorian) at instant of Greatest Eclipse --- Day Calendar Day (Gregorian) at instant of Greatest Eclipse d Hour Hour (UT) of Greatest Eclipse h colon Hour/Minute separator --- Minute Minute of hour of Greatest Eclipse min Type Type of eclipse Type of eclipse where: T = Total Eclipse A = Annular Eclipse AT = Annular/Total Eclipse P = Partial Eclipse --- Saros Saros series of eclipse --- Gamma Distance of the shadow cone axis from the center of Earth (units of equatorial radii) --- Magnitude Fraction of Sun's diameter obscured by Moon --- Lat Latitude where greatest eclipse is seen deg LatHemi Latitude hemisphere (North or South) --- Long Longitude where greatest eclipse is seen deg LongHemi Longitude hemisphere (East or West) --- Alt Sun's altitude at greatest eclipse deg Width Width of the path of totality or annularity at greatest eclipse km DurMin Central duration of total or annular phase at greatest eclipse (minutes) min m Minutes label --- DurSec Central duration of total or annular phase at greatest eclipse (seconds) s s Seconds label --- Year Calendar Year (Gregorian) at instant of Greatest Eclipse yr Month Calendar Month (Gregorian) at instant of Greatest Eclipse --- Day Calendar Day (Gregorian) at instant of Greatest Eclipse d Hour Hour (UT) of Greatest Eclipse h colon Hour/Minute separator --- Minute Minute of hour of Greatest Eclipse min Type Type of eclipse T = Total Eclipse U = Partial (Umbral) Eclipse P = Penumbral Eclipse --- n_Type Note on type "m" = Middle eclipse of Saros series "+" = Central eclipse (Moon north of axis) "-" = Central eclipse (Moon south of axis) b = first penumbral eclipse of a new saros series ("b" = beginning) c = central total eclipse (Tc) --- Saros Saros series of eclipse --- Gamma Distance of Moon from the axis of Earth's shadow cone (units of equatorial radii) --- PenMag Fraction of Moon's diameter obscured by the penumbra --- UmbMag Fraction of Moon's diameter obscured by the umbra --- ParSDur Semi-duration of partial (umbral) eclipse min mP Minutes label --- TotSDur Semi-duration of total (umbral) eclipse min mT Minutes label --- GSTO Greenwich Siderial Time at 00:00 U.T. h RA Geocentric Right Ascension of the Moon at greatest eclipse h Dec Geocentric Declination of the Moon at greatest eclipse deg James E. Gass ADC/SSDOO 1998May12 UNKNOWN UNKNOWN 03-Apr-1998: Data and documentation were copied from the author's web site. The data tables were modified slightly to meet CDS/ADC standard practice (e.g., deleted header and spacer records). UNKNOWN UNKNOWN Notes: The altitude 'a' and azimuth 'A' of the Moon during any phase of an eclipse depends on the time and the observer's geographic coordinates. Neglecting the effects of atmospheric refraction and lunar parallax, 'a' and 'A' are calculated as follows: h = 15 (GST0 + UT - ra) + l a = ArcSin [Sin d Sin f + Cos d Cos h Cos f] A = ArcTan [- (Cos d Sin h) / (Sin d Cos f - Cos d Cos h Sin f)] where: h = Hour Angle of Sun or Moon a = Altitude A = Azimuth GST0 = Greenwich Sidereal Time at 0:00 UT UT = Universal Time ra = Right Ascension of Sun or Moon d = Declination of Sun or Moon l = Observer's Longitude (East +, West -) f = Observer's Latitude (North +, South -) VI_97.xml