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      Compute (low-precision) heliocentric coordinates for the planets.


      The mean orbital elements for epoch J2000 are used. These are derived
      from a 250 yr least squares fit of the DE 200 planetary ephemeris to a
      Keplerian orbit where each element is allowed to vary linearly with
      time. For dates between 1800 and 2050, this solution fits the
      terrestrial planet orbits to ~25" or better, but achieves only ~600"
      for Saturn.
      Use PLANET_COORDS (which calls HELIO) to get celestial (RA, Dec)
      coordinates of the planets

Calling Sequence



      JD = Julian date, double precision scalar or vector
      LIST = List of planets array. May be a single number.
              1 = merc, 2 = venus, ... 9 = pluto.


      HRAD = array of Heliocentric radii (A.U).
      HLONG = array of Heliocentric (ecliptic) longitudes (degrees).
      HLAT = array of Heliocentric latitudes (degrees).
            These output parameters will be dimensioned Nplanet by Ndate,
            where Nplanet is the number of elements of list, and Ndate is
            the number of elements of JD.

Optional Input Keyword

      /RADIAN - If set, then the output longitude and latitude are given in


      (1) Find the current heliocentric positions of all the planets
        IDL> GET_JULDATE, jd ;Get current Julian date
        IDL> HELIO,jd,indgen(9)+1,hrad,hlong,hlat ;Get radius, long, and lat
      (2) Find heliocentric position of Mars on August 23, 2000
        IDL> JDCNV, 2000,08,23,0,jd
                  ===> hrad = 1.6407 AU hlong = 124.3197 hlat = 1.7853
        For comparison, the JPL ephemeris gives
                      hrad = 1.6407 AU hlong = 124.2985 hlat = 1.7845
      (3) Find the heliocentric positions of Mars and Venus for every day in
          November 2000
        IDL> JDCNV, 2000, 11, 1, 0, jd ;Julian date of November 1, 2000
        IDL> helio, jd+indgen(30), [4,2], hrad,hlong,hlat ;Mars=4, Venus=2
                  hrad, hlong, and hlat will be dimensioned [2,30]
                  first column contains Mars data, second column Venus

Common Blocks


Routines Used

      CIRRANGE - force angle between 0 and 2*!PI


      (1) The calling sequence for this procedure was changed in August 2000
      (2) This program is based on the two-body model and thus neglects
          interactions between the planets. This is why the worst results
          are for Saturn. Use the procedure JPLEPHINTERp for more accurate
          positions using the JPL ephemeris. Also see
          http://ssd.jpl.nasa.gov/cgi-bin/eph for a more accurate ephemeris
          generator online.
      (3) The coordinates are given for equinox 2000 and *not* the equinox
          of the supplied date(s)

Modification History

      R. Sterner. 20 Aug, 1986.
      Code cleaned up a bit W. Landsman December 1992
      Major rewrite, use modern orbital elements, vectorize, more accurate
        solution to Kepler's equation W. Landsman August 2000
      Wasn't working for planet vectors W. Landsman August 2000
      Work for more than 32767 positions S. Leach Jan 2009

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