keplereq

    Solve Kepler's Equation

    Solve Kepler's Equation. Method by S. Mikkola (1987) Celestial
       Mechanics, 40 , 329-334.
    result from Mikkola then used as starting value for
       Newton-Raphson iteration to extend the applicability of this
       function to higher eccentricities

    Celestial Mechanics

    eccanom=keplereq(m,ecc)

    m    - Mean anomaly (radians; can be an array)
    ecc  - Eccentricity

    thresh: stopping criterion for the Newton Raphson iteration; the
            iteration stops once abs(E-Eold)<thresh

    the function returns the eccentric anomaly

  2002/05/29 - Marc W. Buie, Lowell Observatory.  Ported from fortran routines
    supplied by Larry Wasserman and Ted Bowell.
    http://www.lowell.edu/users/buie/
  2002-09-09 -- Joern Wilms, IAA Tuebingen, Astronomie.
    use analytical values obtained for the low eccentricity case as
    starting values for a Newton-Raphson method to allow high
    eccentricity values as well
  $Log: keplereq.pro,v $
  Revision 1.3  2005/05/25 16:11:35  wilms
  speed up: Newton Raphson is only done if necessary
  (i.e., almost never)
  Revision 1.2  2004/08/05 10:02:05  wilms
  now also works for more than 32000 time values
  Revision 1.1  2002/09/09 14:54:11  wilms
  initial release into aitlib

[Home Page] [Software, Documentation] [IDL Documentation] [Quick Reference] [Feedback]