int DLL_FUNC calc_planet_orientation( int planet_no, int system_no, double jd,
double *matrix)
#endif
{
static int prev_planet_no = -1, prev_system_no = -1, prev_rval = 0;
static double prev_jd = -1.;
static double prev_matrix[9];
int i, rval, is_retrograde;
double pole_ra, pole_dec, omega;
if( planet_no == prev_planet_no && system_no == prev_system_no
&& jd == prev_jd)
{
memcpy( matrix, prev_matrix, 9 * sizeof( double));
return( prev_rval);
}
prev_planet_no = planet_no;
prev_system_no = system_no;
prev_jd = jd;
if( planet_no == 3) /* handle earth with "normal" precession: */
{
const double J2000 = 2451545.; /* 1.5 Jan 2000 = JD 2451545 */
const double t_cen = (jd - J2000) / 36525.;
int i;
setup_precession( matrix, 2000., 2000. + t_cen * 100.);
for( i = 3; i < 6; i++)
matrix[i] = -matrix[i];
spin_matrix( matrix, matrix + 3, green_sidereal_time( jd));
memcpy( prev_matrix, matrix, 9 * sizeof( double));
prev_rval = 0;
return( 0);
}
/* For everybody else, we use TD. Only the earth uses UT. */
/* (This correction added 5 Nov 98, after G Seronik pointed */
/* out an error in the Saturn central meridian.) */
jd += td_minus_ut( jd) / 86400.; /* correct from UT to TD */
rval = get_cospar_data_from_text_file( planet_no, system_no, jd,
&pole_ra, &pole_dec, &omega, &is_retrograde);
pole_ra *= PI / 180.;
pole_dec *= PI / 180.;
polar3_to_cartesian( matrix, pole_ra - PI / 2., 0.);
polar3_to_cartesian( matrix + 3, pole_ra - PI, PI / 2. - pole_dec);
polar3_to_cartesian( matrix + 6, pole_ra, pole_dec);
spin_matrix( matrix, matrix + 3, omega * PI / 180. + PI);
if( is_retrograde)
for( i = 3; i < 6; i++)
matrix[i] *= -1.;
memcpy( prev_matrix, matrix, 9 * sizeof( double));
prev_rval = rval;
return( rval);
}
int fill_planet_data( PLANET_DATA *pdata, const int planet_no, const double jd,
const double observer_lat, const double observer_lon,
const char *vsop_data)
{
double loc_sidereal_time = green_sidereal_time( jd) + observer_lon;
double t_centuries = (jd - J2000) / 36525.;
double obliquity = mean_obliquity( t_centuries);
double loc[3];
pdata->jd = jd;
if( planet_no == 10) /* get lunar data, not VSOP */
{
double fund[N_FUND];
lunar_fundamentals( vsop_data, t_centuries, fund);
lunar_lon_and_dist( vsop_data, fund, &pdata->ecliptic_lon, &pdata->r, 0L);
pdata->ecliptic_lon *= pi / 180.;
pdata->ecliptic_lat = lunar_lat( vsop_data, fund, 0L) * pi / 180.;
}
else
{
/* What we _really_ want is the location of the sun as */
/* seen from the earth. VSOP gives us the opposite, */
/* i.e., where the _earth_ is as seen from the _sun_. */
/* To evade this, we add PI to the longitude and */
/* negate the latitude. */
pdata->ecliptic_lon =
calc_vsop_loc( vsop_data, planet_no, 0, t_centuries, 0.) + pi;
pdata->ecliptic_lat =
-calc_vsop_loc( vsop_data, planet_no, 1, t_centuries, 0.);
pdata->r = calc_vsop_loc( vsop_data, planet_no, 2, t_centuries, 0.);
}
polar3_to_cartesian( loc, pdata->ecliptic_lon, pdata->ecliptic_lat);
memcpy( pdata->ecliptic_loc, loc, 3 * sizeof( double));
/* At this point, loc is a unit vector in ecliptic */
/* coords of date. Rotate it by 'obliquity' to get */
/* a vector in equatorial coords of date: */
rotate_vector( loc, obliquity, 0);
memcpy( pdata->equatorial_loc, loc, 3 * sizeof( double));
/* The following two rotations take us from a vector in */
/* equatorial coords of date to an alt/az vector: */
rotate_vector( loc, -loc_sidereal_time, 2);
/* printf( "LST: %lf\n", fmod( loc_sidereal_time * 180. / pi, 360.)); */
pdata->hour_angle = atan2( loc[1], loc[0]);
rotate_vector( loc, observer_lat - pi / 2., 1);
memcpy( pdata->altaz_loc, loc, 3 * sizeof( double));
return( 0);
}
