rplanet.c

c源码

/* The following program reduces the heliocentric equatorial
 * rectangular coordinates of the earth and object that
 * were computed by kepler() and produces apparent geocentric
 * right ascension and declination.
 */

#include "kep.h"
extern double pobjb[], pearthb[];
extern double Clightaud;
extern double lighttime;

int reduce( elemnt, q, e )
struct orbit *elemnt;	/* orbital elements of q */
double q[], e[];	/* heliocentric coordinates */
{
double p[3], temp[3], polar[3];
double a, b, s;
int i;
double sqrt(), asin(), log();

/* Save the geometric coordinates at TDT
 */
for( i=0; i<3; i++ )
	temp[i] = q[i];

/* Display ecliptic longitude and latitude re equinox of date
 */
if( prtflg )
	lonlat( q, TDT, polar, 1 );

/* If the object position was computed from heliocentric orbital
 * elements, then say that earth's barycentric position
 * is the same as its heliocentric position.
 */
if( objnum == 99 )
	{
	for( i=0; i<3; i++ )
		pearthb[i] = e[i];
	}
/* Adjust for light time (planetary aberration)
*/
lightt( elemnt, q, e );
/* Apparent distance is the light time.  */
fprintf( ephfile, " %.10e", Clightaud * lighttime );

/* Find Euclidean vectors between earth, object, and the sun
 */
for( i=0; i<3; i++ )
	p[i] = pobjb[i] - pearthb[i];

angles( p, q, e );

if( prtflg )
	{
	a = 0.0;
	for( i=0; i<3; i++ )
		{
		b = temp[i] - e[i];
		a += b * b;
		}
	a = sqrt(a);
	printf( "true geocentric distance %.7f au    ", a ); /* was EO */
	printf( "equatorial diameter %.2f\"\n", 2.0*elemnt->sdiam/EO );


/* Calculate visual magnitude.
 * "Visual" refers to the spectrum of visible light.
 * Phase = 0.5(1+pq) = geometric fraction of disc illuminated.
 * where pq = cos( sun-object-earth angle )
 * The magnitude is
 *    V(1,0) + 2.5 log10( SE^2 SO^2 / Phase)
 * where V(1,0) = elemnt->mag is the magnitude at 1au from
 * both earth and sun and 100% illumination.
 */
	a = 0.5 * (1.0 + pq);
/* Fudge the phase for light leakage in magnitude estimation.
 * Note this phase term estimate does not reflect reality well.
 * Calculated magnitudes of Mercury and Venus are inaccurate.
 */
	b = 0.5 * (1.01 + 0.99*pq);
	s = elemnt->mag + 2.1715 * log( EO*SO ) - 1.085*log(b);
	printf( "approx. visual magnitude %.1f, phase %.3f\n", s, a );
	}

/* Find unit vector from earth in direction of object
 */
for( i=0; i<3; i++ )
	{
	p[i] /= EO;
	temp[i] = p[i];
	}

if( prtflg )
	{
/* Report astrometric position
 */
	showrd( "Astrometric J2000.0:", p, polar );

/* Also in 1950 coordinates
 */
	precess( temp, B1950, -1 );
	showrd( "Astrometric B1950.0:", temp, polar );
	}

/* Correct position for light deflection
 */
relativity( p, q, e );

/* Correct for annual aberration
 */
annuab( p );

/* Precession of the equinox and ecliptic
 * from J2000.0 to ephemeris date
 */
precess( p, TDT, -1 );

/* Ajust for nutation
 * at current ecliptic.
 */
epsiln( TDT );
nutate( TDT, p );


/* Display the final apparent R.A. and Dec.
 * for equinox of date.
 */
if( prtflg )
	printf ("%s.", whatconstel (p, TDT));
ephprint = 1;
showrd( "    Apparent:", p, polar );
ephprint = 0;

/* Go do topocentric reductions.
 */
polar[2] = EO;
altaz( polar, UT );
return(0);
}



extern struct orbit *elobject;
extern double robject[];

int doplanet()
{
  /* calculate heliocentric position of the object */
  kepler( TDT, elobject, robject, obpolar );
  /* apply correction factors and print apparent place */
  reduce( elobject, robject, rearth );
  return 0;
}