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Institut für Astronomie und Astrophysik

Abteilung Astronomie

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keplereq Source code in keplereq.pro

keplereq

Name
    keplereq
Purpose
    Solve Kepler's Equation
Description
    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
Category
    Celestial Mechanics
Calling Sequence
    eccanom=keplereq(m,ecc)
Input Parameters
    m    - Mean anomaly (radians; can be an array)
    ecc  - Eccentricity
Optional Input Parameters

KEYWORD INPUT PARAMETERS:
    thresh: stopping criterion for the Newton Raphson iteration; the
            iteration stops once abs(E-Eold)<thresh
Output Parameters
    the function returns the eccentric anomaly
KEYWORD OUTPUT PARAMETERS:

Common Blocks

Side Effects

Restrictions

Procedure

Revision History
  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

Last modified by pro2html on 2005 May 26 at 03:10 UTC

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Jörn Wilms (wilms@astro.uni-tuebingen.de)
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