1 // moonpos.cxx (basically, this is a slightly modified version of the 'sunpos.cxx' file, adapted from XEarth)
6 // code for calculating the position on the earth's surface for which
7 // the moon is directly overhead (adapted from _practical astronomy
8 // with your calculator, third edition_, peter duffett-smith,
9 // cambridge university press, 1988.)
11 // Copyright (C) 1989, 1990, 1993, 1994, 1995 Kirk Lauritz Johnson
13 // Parts of the source code (as marked) are:
14 // Copyright (C) 1989, 1990, 1991 by Jim Frost
15 // Copyright (C) 1992 by Jamie Zawinski <jwz@lucid.com>
17 // Permission to use, copy, modify and freely distribute xearth for
18 // non-commercial and not-for-profit purposes is hereby granted
19 // without fee, provided that both the above copyright notice and this
20 // permission notice appear in all copies and in supporting
23 // The author makes no representations about the suitability of this
24 // software for any purpose. It is provided "as is" without express or
27 // THE AUTHOR DISCLAIMS ALL WARRANTIES WITH REGARD TO THIS SOFTWARE,
28 // INCLUDING ALL IMPLIED WARRANTIES OF MERCHANTABILITY AND FITNESS,
29 // IN NO EVENT SHALL THE AUTHOR BE LIABLE FOR ANY SPECIAL, INDIRECT
30 // OR CONSEQUENTIAL DAMAGES OR ANY DAMAGES WHATSOEVER RESULTING FROM
31 // LOSS OF USE, DATA OR PROFITS, WHETHER IN AN ACTION OF CONTRACT,
32 // NEGLIGENCE OR OTHER TORTIOUS ACTION, ARISING OUT OF OR IN
33 // CONNECTION WITH THE USE OR PERFORMANCE OF THIS SOFTWARE.
42 #include <simgear/compiler.h>
44 #ifdef FG_HAVE_STD_INCLUDES
54 #include <simgear/constants.h>
55 #include <simgear/debug/logstream.hxx>
56 #include <simgear/math/fg_geodesy.hxx>
57 #include <simgear/math/point3d.hxx>
58 #include <simgear/math/polar3d.hxx>
59 #include <simgear/math/vector.hxx>
61 #include <Astro/solarsystem.hxx>
62 #include <Main/views.hxx>
63 #include <Scenery/scenery.hxx>
65 #include "fg_time.hxx"
66 #include "moonpos.hxx"
68 extern SolarSystem *solarSystem;
74 * the epoch upon which these astronomical calculations are based is
75 * 1990 january 0.0, 631065600 seconds since the beginning of the
76 * "unix epoch" (00:00:00 GMT, Jan. 1, 1970)
78 * given a number of seconds since the start of the unix epoch,
79 * DaysSinceEpoch() computes the number of days since the start of the
80 * astronomical epoch (1990 january 0.0)
83 #define EpochStart (631065600)
84 #define DaysSinceEpoch(secs) (((secs)-EpochStart)*(1.0/(24*3600)))
87 * assuming the apparent orbit of the moon about the earth is circular,
88 * the rate at which the orbit progresses is given by RadsPerDay --
89 * FG_2PI radians per orbit divided by 365.242191 days per year:
92 #define RadsPerDay (FG_2PI/365.242191)
95 * details of moon's apparent orbit at epoch 1990.0 (after
96 * duffett-smith, table 6, section 46)
98 * Epsilon_g (ecliptic longitude at epoch 1990.0) 279.403303 degrees
99 * OmegaBar_g (ecliptic longitude of perigee) 282.768422 degrees
100 * Eccentricity (eccentricity of orbit) 0.016713
103 #define Epsilon_g (279.403303*(FG_2PI/360))
104 #define OmegaBar_g (282.768422*(FG_2PI/360))
105 #define Eccentricity (0.016713)
108 * MeanObliquity gives the mean obliquity of the earth's axis at epoch
109 * 1990.0 (computed as 23.440592 degrees according to the method given
110 * in duffett-smith, section 27)
112 #define MeanObliquity (23.440592*(FG_2PI/360))
114 /* static double solve_keplers_equation(double); */
115 /* static double moon_ecliptic_longitude(time_t); */
116 static void ecliptic_to_equatorial(double, double, double *, double *);
117 static double julian_date(int, int, int);
118 static double GST(time_t);
121 * solve Kepler's equation via Newton's method
122 * (after duffett-smith, section 47)
125 static double solve_keplers_equation(double M) {
131 delta = E - Eccentricity*sin(E) - M;
132 if (fabs(delta) <= 1e-10) break;
133 E -= delta / (1 - Eccentricity*cos(E));
141 /* compute ecliptic longitude of moon (in radians) (after
142 * duffett-smith, section 47) */
144 static double moon_ecliptic_longitude(time_t ssue) {
145 // time_t ssue; // seconds since unix epoch
150 D = DaysSinceEpoch(ssue);
154 if (N < 0) N += FG_2PI;
156 M_moon = N + Epsilon_g - OmegaBar_g;
157 if (M_moon < 0) M_moon += FG_2PI;
159 E = solve_keplers_equation(M_moon);
160 v = 2 * atan(sqrt((1+Eccentricity)/(1-Eccentricity)) * tan(E/2));
162 return (v + OmegaBar_g);
167 /* convert from ecliptic to equatorial coordinates (after
168 * duffett-smith, section 27) */
170 static void ecliptic_to_equatorial(double lambda, double beta,
171 double *alpha, double *delta) {
172 /* double lambda; ecliptic longitude */
173 /* double beta; ecliptic latitude */
174 /* double *alpha; (return) right ascension */
175 /* double *delta; (return) declination */
180 sin_e = sin(MeanObliquity);
181 cos_e = cos(MeanObliquity);
185 *alpha = atan2(sin_l*cos_e - tan(beta)*sin_e, cos_l);
186 *delta = asin(sin(beta)*cos_e + cos(beta)*sin_e*sin_l);
190 /* computing julian dates (assuming gregorian calendar, thus this is
191 * only valid for dates of 1582 oct 15 or later) (after duffett-smith,
194 static double julian_date(int y, int m, int d) {
195 /* int y; year (e.g. 19xx) */
196 /* int m; month (jan=1, feb=2, ...) */
197 /* int d; day of month */
202 /* lazy test to ensure gregorian calendar */
204 FG_LOG( FG_EVENT, FG_ALERT,
205 "WHOOPS! Julian dates only valid for 1582 oct 15 or later" );
208 if ((m == 1) || (m == 2)) {
215 C = (int)(365.25 * y);
216 D = (int)(30.6001 * (m + 1));
218 JD = B + C + D + d + 1720994.5;
224 /* compute greenwich mean sidereal time (GST) corresponding to a given
225 * number of seconds since the unix epoch (after duffett-smith,
227 static double GST(time_t ssue) {
228 /* time_t ssue; seconds since unix epoch */
237 JD = julian_date(tm->tm_year+1900, tm->tm_mon+1, tm->tm_mday);
238 T = (JD - 2451545) / 36525;
240 T0 = ((T + 2.5862e-5) * T + 2400.051336) * T + 6.697374558;
243 if (T0 < 0) T0 += 24;
245 UT = tm->tm_hour + (tm->tm_min + tm->tm_sec / 60.0) / 60.0;
247 T0 += UT * 1.002737909;
249 if (T0 < 0) T0 += 24;
255 /* given a particular time (expressed in seconds since the unix
256 * epoch), compute position on the earth (lat, lon) such that moon is
257 * directly overhead. (lat, lon are reported in radians */
259 void fgMoonPosition(time_t ssue, double *lon, double *lat) {
260 /* time_t ssue; seconds since unix epoch */
261 /* double *lat; (return) latitude */
262 /* double *lon; (return) longitude */
268 /* lambda = moon_ecliptic_longitude(ssue); */
269 /* ecliptic_to_equatorial(lambda, 0.0, &alpha, &delta); */
270 //ecliptic_to_equatorial (solarPosition.lonMoon, 0.0, &alpha, &delta);
272 /* **********************************************************************
273 * NOTE: in the next function, each time the moon's position is updated, the
274 * the moon's longitude is returned from solarSystem->moon. Note that the
275 * moon's position is updated at a much higher frequency than the rate at
276 * which the solar system's rebuilds occur. This is not a problem, however,
277 * because the fgMoonPosition we're talking about here concerns the changing
278 * position of the moon due to the daily rotation of the earth.
279 * The ecliptic longitude, however, represents the position of the moon with
280 * respect to the stars, and completes just one cycle over the course of a
281 * year. Its therefore pretty safe to update the moon's longitude only once
282 * every ten minutes. (Comment added by Durk Talsma).
283 ************************************************************************/
285 ecliptic_to_equatorial( SolarSystem::theSolarSystem->getMoon()->getLon(),
286 0.0, &alpha, &delta );
287 tmp = alpha - (FG_2PI/24)*GST(ssue);
290 while (tmp < -FG_PI);
291 } else if (tmp > FG_PI) {
293 while (tmp < -FG_PI);
301 /* given a particular time expressed in side real time at prime
302 * meridian (GST), compute position on the earth (lat, lon) such that
303 * moon is directly overhead. (lat, lon are reported in radians */
305 static void fgMoonPositionGST(double gst, double *lon, double *lat) {
306 /* time_t ssue; seconds since unix epoch */
307 /* double *lat; (return) latitude */
308 /* double *lon; (return) longitude */
314 /* lambda = moon_ecliptic_longitude(ssue); */
315 /* ecliptic_to_equatorial(lambda, 0.0, &alpha, &delta); */
316 //ecliptic_to_equatorial (solarPosition.lonMoon, 0.0, &alpha, &delta);
317 ecliptic_to_equatorial( SolarSystem::theSolarSystem->getMoon()->getLon(),
318 SolarSystem::theSolarSystem->getMoon()->getLat(),
321 // tmp = alpha - (FG_2PI/24)*GST(ssue);
322 tmp = alpha - (FG_2PI/24)*gst;
325 while (tmp < -FG_PI);
326 } else if (tmp > FG_PI) {
328 while (tmp < -FG_PI);
336 // update the cur_time_params structure with the current moon position
337 void fgUpdateMoonPos( void ) {
341 sgVec3 nup, nmoon, v0, surface_to_moon;
342 Point3D p, rel_moonpos;
343 double dot, east_dot;
344 double moon_gd_lat, sl_radius;
346 l = &cur_light_params;
347 t = FGTime::cur_time_params;
350 FG_LOG( FG_EVENT, FG_INFO, " Updating Moon position" );
352 // (not sure why there was two)
353 // fgMoonPosition(t->cur_time, &l->moon_lon, &moon_gd_lat);
354 fgMoonPositionGST(t->getGst(), &l->moon_lon, &moon_gd_lat);
356 fgGeodToGeoc(moon_gd_lat, 0.0, &sl_radius, &l->moon_gc_lat);
358 p = Point3D( l->moon_lon, l->moon_gc_lat, sl_radius );
359 l->fg_moonpos = fgPolarToCart3d(p);
361 FG_LOG( FG_EVENT, FG_INFO, " t->cur_time = " << t->get_cur_time() );
362 FG_LOG( FG_EVENT, FG_INFO,
363 " Moon Geodetic lat = " << moon_gd_lat
364 << " Geocentric lat = " << l->moon_gc_lat );
366 // update the sun light vector
367 sgSetVec4( l->moon_vec,
368 l->fg_moonpos.x(), l->fg_moonpos.y(), l->fg_moonpos.z(), 0.0 );
369 sgNormalizeVec4( l->moon_vec );
370 sgCopyVec4( l->moon_vec_inv, l->moon_vec );
371 sgNegateVec4( l->moon_vec_inv );
373 // make sure these are directional light sources only
374 l->moon_vec[3] = l->moon_vec_inv[3] = 0.0;
375 // cout << " l->moon_vec = " << l->moon_vec[0] << "," << l->moon_vec[1]
376 // << ","<< l->moon_vec[2] << endl;
378 // calculate the moon's relative angle to local up
379 sgCopyVec3( nup, v->get_local_up() );
380 sgSetVec3( nmoon, l->fg_moonpos.x(), l->fg_moonpos.y(), l->fg_moonpos.z() );
381 sgNormalizeVec3(nup);
382 sgNormalizeVec3(nmoon);
383 // cout << "nup = " << nup[0] << "," << nup[1] << ","
384 // << nup[2] << endl;
385 // cout << "nmoon = " << nmoon[0] << "," << nmoon[1] << ","
386 // << nmoon[2] << endl;
388 l->moon_angle = acos( sgScalarProductVec3( nup, nmoon ) );
389 cout << "moon angle relative to current location = "
390 << l->moon_angle << endl;
392 // calculate vector to moon's position on the earth's surface
393 rel_moonpos = l->fg_moonpos - (v->get_view_pos() + scenery.center);
394 v->set_to_moon( rel_moonpos.x(), rel_moonpos.y(), rel_moonpos.z() );
395 // printf( "Vector to moon = %.2f %.2f %.2f\n",
396 // v->to_moon[0], v->to_moon[1], v->to_moon[2]);
398 // make a vector to the current view position
399 Point3D view_pos = v->get_view_pos();
400 sgSetVec3( v0, view_pos.x(), view_pos.y(), view_pos.z() );
402 // Given a vector from the view position to the point on the
403 // earth's surface the moon is directly over, map into onto the
404 // local plane representing "horizontal".
406 sgmap_vec_onto_cur_surface_plane( v->get_local_up(), v0,
407 v->get_to_moon(), surface_to_moon );
408 sgNormalizeVec3(surface_to_moon);
409 v->set_surface_to_moon( surface_to_moon[0], surface_to_moon[1],
410 surface_to_moon[2] );
411 // cout << "(sg) Surface direction to moon is "
412 // << surface_to_moon[0] << ","
413 // << surface_to_moon[1] << ","
414 // << surface_to_moon[2] << endl;
415 // cout << "Should be close to zero = "
416 // << sgScalarProductVec3(nup, surface_to_moon) << endl;
418 // calculate the angle between v->surface_to_moon and
419 // v->surface_east. We do this so we can sort out the acos()
420 // ambiguity. I wish I could think of a more efficient way ... :-(
421 east_dot = sgScalarProductVec3( surface_to_moon, v->get_surface_east() );
422 // cout << " East dot product = " << east_dot << endl;
424 // calculate the angle between v->surface_to_moon and
425 // v->surface_south. this is how much we have to rotate the sky
426 // for it to align with the moon
427 dot = sgScalarProductVec3( surface_to_moon, v->get_surface_south() );
428 // cout << " Dot product = " << dot << endl;
430 if ( east_dot >= 0 ) {
431 l->moon_rotation = acos(dot);
433 l->moon_rotation = -acos(dot);
435 // cout << " Sky needs to rotate = " << angle << " rads = "
436 // << angle * RAD_TO_DEG << " degrees." << endl;