Canon of Mercury transits

For the computation of this canon, we have used the following physical parameters :

• Equatorial horizontal parallax of the Sun at one AU = 8.794148".
• Semi-diameter of the Sun = 15´ 59.63".
• Quotient of the semi-diameter of Mercury by the equatorial semi-diameter of the Earth : k = 0.3825096.
• Equatorial semi-diameter of the Earth = 6378140m.
• Square of ellipticity of the Earth's ellipsoid = 0.00669438.

Computations are based on planetary theories developped at the Institut de M canique Cleste in Paris.

• Planetary theories SLP98 use Chebyshev polynomials representation for the coordinates of the bodies computed by G. Francou from the planetary theories VSOP87 (P. Bretagnon and G. Francou, 1988).
• Precession theory of Lieske (1976).
• Nutation theory of Wahr (1981).
• Sideral time formula of Aoki (1992).
• The difference between TT and UT is quadratically extrapolated in the distant past (formulae given by J. Chapront, M. Chapront et G. Francou, 1997) or in the future from known values of TT - UT.

For each transit, the following data are given : :

• Date of least topocentric distance between the center of the planet and the center of the Sun (in UTC).
• Time of least topocentric distance between the center of the planet and the center of the Sun (in UTC).
• Type of transit (P : partial, C : central, NC : no-central).
• Least angular topocentric distance between the center of the planet and the center of the Sun in minute and second of degrees.
• Duration of general phase of transit.
• For each Saros :
  
  • Number of Saros series to which the transit belongs (* after number indicate that the series is not full).
  • Place of the transit in the Saros series.