FACT++  1.0
plan94.c
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1 #include "erfa.h"
2 
3 int eraPlan94(double date1, double date2, int np, double pv[2][3])
4 /*
5 ** - - - - - - - - - -
6 ** e r a P l a n 9 4
7 ** - - - - - - - - - -
8 **
9 ** Approximate heliocentric position and velocity of a nominated major
10 ** planet: Mercury, Venus, EMB, Mars, Jupiter, Saturn, Uranus or
11 ** Neptune (but not the Earth itself).
12 **
13 ** Given:
14 ** date1 double TDB date part A (Note 1)
15 ** date2 double TDB date part B (Note 1)
16 ** np int planet (1=Mercury, 2=Venus, 3=EMB, 4=Mars,
17 ** 5=Jupiter, 6=Saturn, 7=Uranus, 8=Neptune)
18 **
19 ** Returned (argument):
20 ** pv double[2][3] planet p,v (heliocentric, J2000.0, AU,AU/d)
21 **
22 ** Returned (function value):
23 ** int status: -1 = illegal NP (outside 1-8)
24 ** 0 = OK
25 ** +1 = warning: year outside 1000-3000
26 ** +2 = warning: failed to converge
27 **
28 ** Notes:
29 **
30 ** 1) The date date1+date2 is in the TDB time scale (in practice TT can
31 ** be used) and is a Julian Date, apportioned in any convenient way
32 ** between the two arguments. For example, JD(TDB)=2450123.7 could
33 ** be expressed in any of these ways, among others:
34 **
35 ** date1 date2
36 **
37 ** 2450123.7 0.0 (JD method)
38 ** 2451545.0 -1421.3 (J2000 method)
39 ** 2400000.5 50123.2 (MJD method)
40 ** 2450123.5 0.2 (date & time method)
41 **
42 ** The JD method is the most natural and convenient to use in cases
43 ** where the loss of several decimal digits of resolution is
44 ** acceptable. The J2000 method is best matched to the way the
45 ** argument is handled internally and will deliver the optimum
46 ** resolution. The MJD method and the date & time methods are both
47 ** good compromises between resolution and convenience. The limited
48 ** accuracy of the present algorithm is such that any of the methods
49 ** is satisfactory.
50 **
51 ** 2) If an np value outside the range 1-8 is supplied, an error status
52 ** (function value -1) is returned and the pv vector set to zeroes.
53 **
54 ** 3) For np=3 the result is for the Earth-Moon Barycenter. To obtain
55 ** the heliocentric position and velocity of the Earth, use instead
56 ** the ERFA function eraEpv00.
57 **
58 ** 4) On successful return, the array pv contains the following:
59 **
60 ** pv[0][0] x }
61 ** pv[0][1] y } heliocentric position, AU
62 ** pv[0][2] z }
63 **
64 ** pv[1][0] xdot }
65 ** pv[1][1] ydot } heliocentric velocity, AU/d
66 ** pv[1][2] zdot }
67 **
68 ** The reference frame is equatorial and is with respect to the
69 ** mean equator and equinox of epoch J2000.0.
70 **
71 ** 5) The algorithm is due to J.L. Simon, P. Bretagnon, J. Chapront,
72 ** M. Chapront-Touze, G. Francou and J. Laskar (Bureau des
73 ** Longitudes, Paris, France). From comparisons with JPL
74 ** ephemeris DE102, they quote the following maximum errors
75 ** over the interval 1800-2050:
76 **
77 ** L (arcsec) B (arcsec) R (km)
78 **
79 ** Mercury 4 1 300
80 ** Venus 5 1 800
81 ** EMB 6 1 1000
82 ** Mars 17 1 7700
83 ** Jupiter 71 5 76000
84 ** Saturn 81 13 267000
85 ** Uranus 86 7 712000
86 ** Neptune 11 1 253000
87 **
88 ** Over the interval 1000-3000, they report that the accuracy is no
89 ** worse than 1.5 times that over 1800-2050. Outside 1000-3000 the
90 ** accuracy declines.
91 **
92 ** Comparisons of the present function with the JPL DE200 ephemeris
93 ** give the following RMS errors over the interval 1960-2025:
94 **
95 ** position (km) velocity (m/s)
96 **
97 ** Mercury 334 0.437
98 ** Venus 1060 0.855
99 ** EMB 2010 0.815
100 ** Mars 7690 1.98
101 ** Jupiter 71700 7.70
102 ** Saturn 199000 19.4
103 ** Uranus 564000 16.4
104 ** Neptune 158000 14.4
105 **
106 ** Comparisons against DE200 over the interval 1800-2100 gave the
107 ** following maximum absolute differences. (The results using
108 ** DE406 were essentially the same.)
109 **
110 ** L (arcsec) B (arcsec) R (km) Rdot (m/s)
111 **
112 ** Mercury 7 1 500 0.7
113 ** Venus 7 1 1100 0.9
114 ** EMB 9 1 1300 1.0
115 ** Mars 26 1 9000 2.5
116 ** Jupiter 78 6 82000 8.2
117 ** Saturn 87 14 263000 24.6
118 ** Uranus 86 7 661000 27.4
119 ** Neptune 11 2 248000 21.4
120 **
121 ** 6) The present ERFA re-implementation of the original Simon et al.
122 ** Fortran code differs from the original in the following respects:
123 **
124 ** * C instead of Fortran.
125 **
126 ** * The date is supplied in two parts.
127 **
128 ** * The result is returned only in equatorial Cartesian form;
129 ** the ecliptic longitude, latitude and radius vector are not
130 ** returned.
131 **
132 ** * The result is in the J2000.0 equatorial frame, not ecliptic.
133 **
134 ** * More is done in-line: there are fewer calls to subroutines.
135 **
136 ** * Different error/warning status values are used.
137 **
138 ** * A different Kepler's-equation-solver is used (avoiding
139 ** use of double precision complex).
140 **
141 ** * Polynomials in t are nested to minimize rounding errors.
142 **
143 ** * Explicit double constants are used to avoid mixed-mode
144 ** expressions.
145 **
146 ** None of the above changes affects the result significantly.
147 **
148 ** 7) The returned status indicates the most serious condition
149 ** encountered during execution of the function. Illegal np is
150 ** considered the most serious, overriding failure to converge,
151 ** which in turn takes precedence over the remote date warning.
152 **
153 ** Called:
154 ** eraAnp normalize angle into range 0 to 2pi
155 **
156 ** Reference: Simon, J.L, Bretagnon, P., Chapront, J.,
157 ** Chapront-Touze, M., Francou, G., and Laskar, J.,
158 ** Astron. Astrophys. 282, 663 (1994).
159 **
160 ** Copyright (C) 2013-2015, NumFOCUS Foundation.
161 ** Derived, with permission, from the SOFA library. See notes at end of file.
162 */
163 {
164 /* Gaussian constant */
165  static const double GK = 0.017202098950;
166 
167 /* Sin and cos of J2000.0 mean obliquity (IAU 1976) */
168  static const double SINEPS = 0.3977771559319137;
169  static const double COSEPS = 0.9174820620691818;
170 
171 /* Maximum number of iterations allowed to solve Kepler's equation */
172  static const int KMAX = 10;
173 
174  int jstat, i, k;
175  double t, da, dl, de, dp, di, dom, dmu, arga, argl, am,
176  ae, dae, ae2, at, r, v, si2, xq, xp, tl, xsw,
177  xcw, xm2, xf, ci2, xms, xmc, xpxq2, x, y, z;
178 
179 /* Planetary inverse masses */
180  static const double amas[] = { 6023600.0, /* Mercury */
181  408523.5, /* Venus */
182  328900.5, /* EMB */
183  3098710.0, /* Mars */
184  1047.355, /* Jupiter */
185  3498.5, /* Saturn */
186  22869.0, /* Uranus */
187  19314.0 }; /* Neptune */
188 
189 /*
190 ** Tables giving the mean Keplerian elements, limited to t^2 terms:
191 **
192 ** a semi-major axis (AU)
193 ** dlm mean longitude (degree and arcsecond)
194 ** e eccentricity
195 ** pi longitude of the perihelion (degree and arcsecond)
196 ** dinc inclination (degree and arcsecond)
197 ** omega longitude of the ascending node (degree and arcsecond)
198 */
199 
200  static const double a[][3] = {
201  { 0.3870983098, 0.0, 0.0 }, /* Mercury */
202  { 0.7233298200, 0.0, 0.0 }, /* Venus */
203  { 1.0000010178, 0.0, 0.0 }, /* EMB */
204  { 1.5236793419, 3e-10, 0.0 }, /* Mars */
205  { 5.2026032092, 19132e-10, -39e-10 }, /* Jupiter */
206  { 9.5549091915, -0.0000213896, 444e-10 }, /* Saturn */
207  { 19.2184460618, -3716e-10, 979e-10 }, /* Uranus */
208  { 30.1103868694, -16635e-10, 686e-10 } /* Neptune */
209  };
210 
211  static const double dlm[][3] = {
212  { 252.25090552, 5381016286.88982, -1.92789 },
213  { 181.97980085, 2106641364.33548, 0.59381 },
214  { 100.46645683, 1295977422.83429, -2.04411 },
215  { 355.43299958, 689050774.93988, 0.94264 },
216  { 34.35151874, 109256603.77991, -30.60378 },
217  { 50.07744430, 43996098.55732, 75.61614 },
218  { 314.05500511, 15424811.93933, -1.75083 },
219  { 304.34866548, 7865503.20744, 0.21103 }
220  };
221 
222  static const double e[][3] = {
223  { 0.2056317526, 0.0002040653, -28349e-10 },
224  { 0.0067719164, -0.0004776521, 98127e-10 },
225  { 0.0167086342, -0.0004203654, -0.0000126734 },
226  { 0.0934006477, 0.0009048438, -80641e-10 },
227  { 0.0484979255, 0.0016322542, -0.0000471366 },
228  { 0.0555481426, -0.0034664062, -0.0000643639 },
229  { 0.0463812221, -0.0002729293, 0.0000078913 },
230  { 0.0094557470, 0.0000603263, 0.0 }
231  };
232 
233  static const double pi[][3] = {
234  { 77.45611904, 5719.11590, -4.83016 },
235  { 131.56370300, 175.48640, -498.48184 },
236  { 102.93734808, 11612.35290, 53.27577 },
237  { 336.06023395, 15980.45908, -62.32800 },
238  { 14.33120687, 7758.75163, 259.95938 },
239  { 93.05723748, 20395.49439, 190.25952 },
240  { 173.00529106, 3215.56238, -34.09288 },
241  { 48.12027554, 1050.71912, 27.39717 }
242  };
243 
244  static const double dinc[][3] = {
245  { 7.00498625, -214.25629, 0.28977 },
246  { 3.39466189, -30.84437, -11.67836 },
247  { 0.0, 469.97289, -3.35053 },
248  { 1.84972648, -293.31722, -8.11830 },
249  { 1.30326698, -71.55890, 11.95297 },
250  { 2.48887878, 91.85195, -17.66225 },
251  { 0.77319689, -60.72723, 1.25759 },
252  { 1.76995259, 8.12333, 0.08135 }
253  };
254 
255  static const double omega[][3] = {
256  { 48.33089304, -4515.21727, -31.79892 },
257  { 76.67992019, -10008.48154, -51.32614 },
258  { 174.87317577, -8679.27034, 15.34191 },
259  { 49.55809321, -10620.90088, -230.57416 },
260  { 100.46440702, 6362.03561, 326.52178 },
261  { 113.66550252, -9240.19942, -66.23743 },
262  { 74.00595701, 2669.15033, 145.93964 },
263  { 131.78405702, -221.94322, -0.78728 }
264  };
265 
266 /* Tables for trigonometric terms to be added to the mean elements of */
267 /* the semi-major axes */
268 
269  static const double kp[][9] = {
270  { 69613, 75645, 88306, 59899, 15746, 71087, 142173, 3086, 0 },
271  { 21863, 32794, 26934, 10931, 26250, 43725, 53867, 28939, 0 },
272  { 16002, 21863, 32004, 10931, 14529, 16368, 15318, 32794, 0 },
273  { 6345, 7818, 15636, 7077, 8184, 14163, 1107, 4872, 0 },
274  { 1760, 1454, 1167, 880, 287, 2640, 19, 2047, 1454 },
275  { 574, 0, 880, 287, 19, 1760, 1167, 306, 574 },
276  { 204, 0, 177, 1265, 4, 385, 200, 208, 204 },
277  { 0, 102, 106, 4, 98, 1367, 487, 204, 0 }
278  };
279 
280  static const double ca[][9] = {
281  { 4, -13, 11, -9, -9, -3, -1, 4, 0 },
282  { -156, 59, -42, 6, 19, -20, -10, -12, 0 },
283  { 64, -152, 62, -8, 32, -41, 19, -11, 0 },
284  { 124, 621, -145, 208, 54, -57, 30, 15, 0 },
285  { -23437, -2634, 6601, 6259, -1507,-1821, 2620, -2115, -1489 },
286  { 62911,-119919, 79336,17814,-24241,12068, 8306, -4893, 8902 },
287  { 389061,-262125,-44088, 8387,-22976,-2093, -615, -9720, 6633 },
288  { -412235,-157046,-31430,37817, -9740, -13, -7449, 9644, 0 }
289  };
290 
291  static const double sa[][9] = {
292  { -29, -1, 9, 6, -6, 5, 4, 0, 0 },
293  { -48, -125, -26, -37, 18, -13, -20, -2, 0 },
294  { -150, -46, 68, 54, 14, 24, -28, 22, 0 },
295  { -621, 532, -694, -20, 192, -94, 71, -73, 0 },
296  { -14614,-19828, -5869, 1881, -4372, -2255, 782, 930, 913 },
297  { 139737, 0, 24667, 51123, -5102, 7429, -4095, -1976, -9566 },
298  { -138081, 0, 37205,-49039,-41901,-33872,-27037,-12474, 18797 },
299  { 0, 28492,133236, 69654, 52322,-49577,-26430, -3593, 0 }
300  };
301 
302 /* Tables giving the trigonometric terms to be added to the mean */
303 /* elements of the mean longitudes */
304 
305  static const double kq[][10] = {
306  { 3086,15746,69613,59899,75645,88306, 12661, 2658, 0, 0 },
307  { 21863,32794,10931, 73, 4387,26934, 1473, 2157, 0, 0 },
308  { 10,16002,21863,10931, 1473,32004, 4387, 73, 0, 0 },
309  { 10, 6345, 7818, 1107,15636, 7077, 8184, 532, 10, 0 },
310  { 19, 1760, 1454, 287, 1167, 880, 574, 2640, 19, 1454 },
311  { 19, 574, 287, 306, 1760, 12, 31, 38, 19, 574 },
312  { 4, 204, 177, 8, 31, 200, 1265, 102, 4, 204 },
313  { 4, 102, 106, 8, 98, 1367, 487, 204, 4, 102 }
314  };
315 
316  static const double cl[][10] = {
317  { 21, -95, -157, 41, -5, 42, 23, 30, 0, 0 },
318  { -160, -313, -235, 60, -74, -76, -27, 34, 0, 0 },
319  { -325, -322, -79, 232, -52, 97, 55, -41, 0, 0 },
320  { 2268, -979, 802, 602, -668, -33, 345, 201, -55, 0 },
321  { 7610, -4997,-7689,-5841,-2617, 1115,-748,-607, 6074, 354 },
322  { -18549, 30125,20012, -730, 824, 23,1289,-352, -14767, -2062 },
323  { -135245,-14594, 4197,-4030,-5630,-2898,2540,-306, 2939, 1986 },
324  { 89948, 2103, 8963, 2695, 3682, 1648, 866,-154, -1963, -283 }
325  };
326 
327  static const double sl[][10] = {
328  { -342, 136, -23, 62, 66, -52, -33, 17, 0, 0 },
329  { 524, -149, -35, 117, 151, 122, -71, -62, 0, 0 },
330  { -105, -137, 258, 35, -116, -88,-112, -80, 0, 0 },
331  { 854, -205, -936, -240, 140, -341, -97, -232, 536, 0 },
332  { -56980, 8016, 1012, 1448,-3024,-3710, 318, 503, 3767, 577 },
333  { 138606,-13478,-4964, 1441,-1319,-1482, 427, 1236, -9167, -1918 },
334  { 71234,-41116, 5334,-4935,-1848, 66, 434, -1748, 3780, -701 },
335  { -47645, 11647, 2166, 3194, 679, 0,-244, -419, -2531, 48 }
336  };
337 
338 /*--------------------------------------------------------------------*/
339 
340 /* Validate the planet number. */
341  if ((np < 1) || (np > 8)) {
342  jstat = -1;
343 
344  /* Reset the result in case of failure. */
345  for (k = 0; k < 2; k++) {
346  for (i = 0; i < 3; i++) {
347  pv[k][i] = 0.0;
348  }
349  }
350 
351  } else {
352 
353  /* Decrement the planet number to start at zero. */
354  np--;
355 
356  /* Time: Julian millennia since J2000.0. */
357  t = ((date1 - ERFA_DJ00) + date2) / ERFA_DJM;
358 
359  /* OK status unless remote date. */
360  jstat = fabs(t) <= 1.0 ? 0 : 1;
361 
362  /* Compute the mean elements. */
363  da = a[np][0] +
364  (a[np][1] +
365  a[np][2] * t) * t;
366  dl = (3600.0 * dlm[np][0] +
367  (dlm[np][1] +
368  dlm[np][2] * t) * t) * ERFA_DAS2R;
369  de = e[np][0] +
370  ( e[np][1] +
371  e[np][2] * t) * t;
372  dp = eraAnpm((3600.0 * pi[np][0] +
373  (pi[np][1] +
374  pi[np][2] * t) * t) * ERFA_DAS2R);
375  di = (3600.0 * dinc[np][0] +
376  (dinc[np][1] +
377  dinc[np][2] * t) * t) * ERFA_DAS2R;
378  dom = eraAnpm((3600.0 * omega[np][0] +
379  (omega[np][1] +
380  omega[np][2] * t) * t) * ERFA_DAS2R);
381 
382  /* Apply the trigonometric terms. */
383  dmu = 0.35953620 * t;
384  for (k = 0; k < 8; k++) {
385  arga = kp[np][k] * dmu;
386  argl = kq[np][k] * dmu;
387  da += (ca[np][k] * cos(arga) +
388  sa[np][k] * sin(arga)) * 1e-7;
389  dl += (cl[np][k] * cos(argl) +
390  sl[np][k] * sin(argl)) * 1e-7;
391  }
392  arga = kp[np][8] * dmu;
393  da += t * (ca[np][8] * cos(arga) +
394  sa[np][8] * sin(arga)) * 1e-7;
395  for (k = 8; k < 10; k++) {
396  argl = kq[np][k] * dmu;
397  dl += t * (cl[np][k] * cos(argl) +
398  sl[np][k] * sin(argl)) * 1e-7;
399  }
400  dl = fmod(dl, ERFA_D2PI);
401 
402  /* Iterative soln. of Kepler's equation to get eccentric anomaly. */
403  am = dl - dp;
404  ae = am + de * sin(am);
405  k = 0;
406  dae = 1.0;
407  while (k < KMAX && fabs(dae) > 1e-12) {
408  dae = (am - ae + de * sin(ae)) / (1.0 - de * cos(ae));
409  ae += dae;
410  k++;
411  if (k == KMAX-1) jstat = 2;
412  }
413 
414  /* True anomaly. */
415  ae2 = ae / 2.0;
416  at = 2.0 * atan2(sqrt((1.0 + de) / (1.0 - de)) * sin(ae2),
417  cos(ae2));
418 
419  /* Distance (AU) and speed (radians per day). */
420  r = da * (1.0 - de * cos(ae));
421  v = GK * sqrt((1.0 + 1.0 / amas[np]) / (da * da * da));
422 
423  si2 = sin(di / 2.0);
424  xq = si2 * cos(dom);
425  xp = si2 * sin(dom);
426  tl = at + dp;
427  xsw = sin(tl);
428  xcw = cos(tl);
429  xm2 = 2.0 * (xp * xcw - xq * xsw);
430  xf = da / sqrt(1 - de * de);
431  ci2 = cos(di / 2.0);
432  xms = (de * sin(dp) + xsw) * xf;
433  xmc = (de * cos(dp) + xcw) * xf;
434  xpxq2 = 2 * xp * xq;
435 
436  /* Position (J2000.0 ecliptic x,y,z in AU). */
437  x = r * (xcw - xm2 * xp);
438  y = r * (xsw + xm2 * xq);
439  z = r * (-xm2 * ci2);
440 
441  /* Rotate to equatorial. */
442  pv[0][0] = x;
443  pv[0][1] = y * COSEPS - z * SINEPS;
444  pv[0][2] = y * SINEPS + z * COSEPS;
445 
446  /* Velocity (J2000.0 ecliptic xdot,ydot,zdot in AU/d). */
447  x = v * (( -1.0 + 2.0 * xp * xp) * xms + xpxq2 * xmc);
448  y = v * (( 1.0 - 2.0 * xq * xq) * xmc - xpxq2 * xms);
449  z = v * (2.0 * ci2 * (xp * xms + xq * xmc));
450 
451  /* Rotate to equatorial. */
452  pv[1][0] = x;
453  pv[1][1] = y * COSEPS - z * SINEPS;
454  pv[1][2] = y * SINEPS + z * COSEPS;
455 
456  }
457 
458 /* Return the status. */
459  return jstat;
460 
461 }
462 /*----------------------------------------------------------------------
463 **
464 **
465 ** Copyright (C) 2013-2015, NumFOCUS Foundation.
466 ** All rights reserved.
467 **
468 ** This library is derived, with permission, from the International
469 ** Astronomical Union's "Standards of Fundamental Astronomy" library,
470 ** available from http://www.iausofa.org.
471 **
472 ** The ERFA version is intended to retain identical functionality to
473 ** the SOFA library, but made distinct through different function and
474 ** file names, as set out in the SOFA license conditions. The SOFA
475 ** original has a role as a reference standard for the IAU and IERS,
476 ** and consequently redistribution is permitted only in its unaltered
477 ** state. The ERFA version is not subject to this restriction and
478 ** therefore can be included in distributions which do not support the
479 ** concept of "read only" software.
480 **
481 ** Although the intent is to replicate the SOFA API (other than
482 ** replacement of prefix names) and results (with the exception of
483 ** bugs; any that are discovered will be fixed), SOFA is not
484 ** responsible for any errors found in this version of the library.
485 **
486 ** If you wish to acknowledge the SOFA heritage, please acknowledge
487 ** that you are using a library derived from SOFA, rather than SOFA
488 ** itself.
489 **
490 **
491 ** TERMS AND CONDITIONS
492 **
493 ** Redistribution and use in source and binary forms, with or without
494 ** modification, are permitted provided that the following conditions
495 ** are met:
496 **
497 ** 1 Redistributions of source code must retain the above copyright
498 ** notice, this list of conditions and the following disclaimer.
499 **
500 ** 2 Redistributions in binary form must reproduce the above copyright
501 ** notice, this list of conditions and the following disclaimer in
502 ** the documentation and/or other materials provided with the
503 ** distribution.
504 **
505 ** 3 Neither the name of the Standards Of Fundamental Astronomy Board,
506 ** the International Astronomical Union nor the names of its
507 ** contributors may be used to endorse or promote products derived
508 ** from this software without specific prior written permission.
509 **
510 ** THIS SOFTWARE IS PROVIDED BY THE COPYRIGHT HOLDERS AND CONTRIBUTORS
511 ** "AS IS" AND ANY EXPRESS OR IMPLIED WARRANTIES, INCLUDING, BUT NOT
512 ** LIMITED TO, THE IMPLIED WARRANTIES OF MERCHANTABILITY AND FITNESS
513 ** FOR A PARTICULAR PURPOSE ARE DISCLAIMED. IN NO EVENT SHALL THE
514 ** COPYRIGHT HOLDER OR CONTRIBUTORS BE LIABLE FOR ANY DIRECT, INDIRECT,
515 ** INCIDENTAL, SPECIAL, EXEMPLARY, OR CONSEQUENTIAL DAMAGES (INCLUDING,
516 ** BUT NOT LIMITED TO, PROCUREMENT OF SUBSTITUTE GOODS OR SERVICES;
517 ** LOSS OF USE, DATA, OR PROFITS; OR BUSINESS INTERRUPTION) HOWEVER
518 ** CAUSED AND ON ANY THEORY OF LIABILITY, WHETHER IN CONTRACT, STRICT
519 ** LIABILITY, OR TORT (INCLUDING NEGLIGENCE OR OTHERWISE) ARISING IN
520 ** ANY WAY OUT OF THE USE OF THIS SOFTWARE, EVEN IF ADVISED OF THE
521 ** POSSIBILITY OF SUCH DAMAGE.
522 **
523 */
ERFA_DJ00
#define ERFA_DJ00
Definition: erfam.h:87
i
int i
Definition: db_dim_client.c:21
eraPlan94
int eraPlan94(double date1, double date2, int np, double pv[2][3])
Definition: plan94.c:3
ERFA_DAS2R
#define ERFA_DAS2R
Definition: erfam.h:60
ERFA_DJM
#define ERFA_DJM
Definition: erfam.h:84
ERFA_D2PI
#define ERFA_D2PI
Definition: erfam.h:48
eraAnpm
double eraAnpm(double a)
Definition: anpm.c:3
t
TT t
Definition: test_client.c:26