1 /*
2 * The MIT License (MIT)
3 *
4 * Copyright (c) 2015-2019 Derick Rethans
5 *
6 * Permission is hereby granted, free of charge, to any person obtaining a copy
7 * of this software and associated documentation files (the "Software"), to deal
8 * in the Software without restriction, including without limitation the rights
9 * to use, copy, modify, merge, publish, distribute, sublicense, and/or sell
10 * copies of the Software, and to permit persons to whom the Software is
11 * furnished to do so, subject to the following conditions:
12 *
13 * The above copyright notice and this permission notice shall be included in
14 * all copies or substantial portions of the Software.
15 *
16 * THE SOFTWARE IS PROVIDED "AS IS", WITHOUT WARRANTY OF ANY KIND, EXPRESS OR
17 * IMPLIED, INCLUDING BUT NOT LIMITED TO THE WARRANTIES OF MERCHANTABILITY,
18 * FITNESS FOR A PARTICULAR PURPOSE AND NONINFRINGEMENT. IN NO EVENT SHALL THE
19 * AUTHORS OR COPYRIGHT HOLDERS BE LIABLE FOR ANY CLAIM, DAMAGES OR OTHER
20 * LIABILITY, WHETHER IN AN ACTION OF CONTRACT, TORT OR OTHERWISE, ARISING FROM,
21 * OUT OF OR IN CONNECTION WITH THE SOFTWARE OR THE USE OR OTHER DEALINGS IN
22 * THE SOFTWARE.
23 */
24 /*
25 | Algorithms are taken from a public domain source by Paul |
26 | Schlyter, who wrote this in December 1992 |
27 */
28
29 #include "timelib.h"
30 #include <stdio.h>
31 #include <math.h>
32
33 #define days_since_2000_Jan_0(y,m,d) \
34 (367L*(y)-((7*((y)+(((m)+9)/12)))/4)+((275*(m))/9)+(d)-730530L)
35
36 #ifndef PI
37 # define PI 3.1415926535897932384
38 #endif
39
40 #define RADEG ( 180.0 / PI )
41 #define DEGRAD ( PI / 180.0 )
42
43 /* The trigonometric functions in degrees */
44
45 #define sind(x) sin((x)*DEGRAD)
46 #define cosd(x) cos((x)*DEGRAD)
47 #define tand(x) tan((x)*DEGRAD)
48
49 #define atand(x) (RADEG*atan(x))
50 #define asind(x) (RADEG*asin(x))
51 #define acosd(x) (RADEG*acos(x))
52 #define atan2d(y,x) (RADEG*atan2(y,x))
53
54
55 /* Following are some macros around the "workhorse" function __daylen__ */
56 /* They mainly fill in the desired values for the reference altitude */
57 /* below the horizon, and also selects whether this altitude should */
58 /* refer to the Sun's center or its upper limb. */
59
60
61 #include "astro.h"
62
63 /******************************************************************/
64 /* This function reduces any angle to within the first revolution */
65 /* by subtracting or adding even multiples of 360.0 until the */
66 /* result is >= 0.0 and < 360.0 */
67 /******************************************************************/
68
69 #define INV360 (1.0 / 360.0)
70
71 /*****************************************/
72 /* Reduce angle to within 0..360 degrees */
73 /*****************************************/
astro_revolution(double x)74 static double astro_revolution(double x)
75 {
76 return (x - 360.0 * floor(x * INV360));
77 }
78
79 /*********************************************/
80 /* Reduce angle to within +180..+180 degrees */
81 /*********************************************/
astro_rev180(double x)82 static double astro_rev180( double x )
83 {
84 return (x - 360.0 * floor(x * INV360 + 0.5));
85 }
86
87 /*******************************************************************/
88 /* This function computes GMST0, the Greenwich Mean Sidereal Time */
89 /* at 0h UT (i.e. the sidereal time at the Greenwhich meridian at */
90 /* 0h UT). GMST is then the sidereal time at Greenwich at any */
91 /* time of the day. I've generalized GMST0 as well, and define it */
92 /* as: GMST0 = GMST - UT -- this allows GMST0 to be computed at */
93 /* other times than 0h UT as well. While this sounds somewhat */
94 /* contradictory, it is very practical: instead of computing */
95 /* GMST like: */
96 /* */
97 /* GMST = (GMST0) + UT * (366.2422/365.2422) */
98 /* */
99 /* where (GMST0) is the GMST last time UT was 0 hours, one simply */
100 /* computes: */
101 /* */
102 /* GMST = GMST0 + UT */
103 /* */
104 /* where GMST0 is the GMST "at 0h UT" but at the current moment! */
105 /* Defined in this way, GMST0 will increase with about 4 min a */
106 /* day. It also happens that GMST0 (in degrees, 1 hr = 15 degr) */
107 /* is equal to the Sun's mean longitude plus/minus 180 degrees! */
108 /* (if we neglect aberration, which amounts to 20 seconds of arc */
109 /* or 1.33 seconds of time) */
110 /* */
111 /*******************************************************************/
112
astro_GMST0(double d)113 static double astro_GMST0(double d)
114 {
115 double sidtim0;
116 /* Sidtime at 0h UT = L (Sun's mean longitude) + 180.0 degr */
117 /* L = M + w, as defined in sunpos(). Since I'm too lazy to */
118 /* add these numbers, I'll let the C compiler do it for me. */
119 /* Any decent C compiler will add the constants at compile */
120 /* time, imposing no runtime or code overhead. */
121 sidtim0 = astro_revolution((180.0 + 356.0470 + 282.9404) + (0.9856002585 + 4.70935E-5) * d);
122 return sidtim0;
123 }
124
125 /* This function computes the Sun's position at any instant */
126
127 /******************************************************/
128 /* Computes the Sun's ecliptic longitude and distance */
129 /* at an instant given in d, number of days since */
130 /* 2000 Jan 0.0. The Sun's ecliptic latitude is not */
131 /* computed, since it's always very near 0. */
132 /******************************************************/
astro_sunpos(double d,double * lon,double * r)133 static void astro_sunpos(double d, double *lon, double *r)
134 {
135 double M, /* Mean anomaly of the Sun */
136 w, /* Mean longitude of perihelion */
137 /* Note: Sun's mean longitude = M + w */
138 e, /* Eccentricity of Earth's orbit */
139 E, /* Eccentric anomaly */
140 x, y, /* x, y coordinates in orbit */
141 v; /* True anomaly */
142
143 /* Compute mean elements */
144 M = astro_revolution(356.0470 + 0.9856002585 * d);
145 w = 282.9404 + 4.70935E-5 * d;
146 e = 0.016709 - 1.151E-9 * d;
147
148 /* Compute true longitude and radius vector */
149 E = M + e * RADEG * sind(M) * (1.0 + e * cosd(M));
150 x = cosd(E) - e;
151 y = sqrt(1.0 - e*e) * sind(E);
152 *r = sqrt(x*x + y*y); /* Solar distance */
153 v = atan2d(y, x); /* True anomaly */
154 *lon = v + w; /* True solar longitude */
155 if (*lon >= 360.0) {
156 *lon -= 360.0; /* Make it 0..360 degrees */
157 }
158 }
159
astro_sun_RA_dec(double d,double * RA,double * dec,double * r)160 static void astro_sun_RA_dec(double d, double *RA, double *dec, double *r)
161 {
162 double lon, obl_ecl, x, y, z;
163
164 /* Compute Sun's ecliptical coordinates */
165 astro_sunpos(d, &lon, r);
166
167 /* Compute ecliptic rectangular coordinates (z=0) */
168 x = *r * cosd(lon);
169 y = *r * sind(lon);
170
171 /* Compute obliquity of ecliptic (inclination of Earth's axis) */
172 obl_ecl = 23.4393 - 3.563E-7 * d;
173
174 /* Convert to equatorial rectangular coordinates - x is unchanged */
175 z = y * sind(obl_ecl);
176 y = y * cosd(obl_ecl);
177
178 /* Convert to spherical coordinates */
179 *RA = atan2d(y, x);
180 *dec = atan2d(z, sqrt(x*x + y*y));
181 }
182
183 /**
184 * Note: timestamp = unixtimestamp (NEEDS to be 00:00:00 UT)
185 * Eastern longitude positive, Western longitude negative
186 * Northern latitude positive, Southern latitude negative
187 * The longitude value IS critical in this function!
188 * altit = the altitude which the Sun should cross
189 * Set to -35/60 degrees for rise/set, -6 degrees
190 * for civil, -12 degrees for nautical and -18
191 * degrees for astronomical twilight.
192 * upper_limb: non-zero -> upper limb, zero -> center
193 * Set to non-zero (e.g. 1) when computing rise/set
194 * times, and to zero when computing start/end of
195 * twilight.
196 * *rise = where to store the rise time
197 * *set = where to store the set time
198 * Both times are relative to the specified altitude,
199 * and thus this function can be used to compute
200 * various twilight times, as well as rise/set times
201 * Return value: 0 = sun rises/sets this day, times stored at
202 * *trise and *tset.
203 * +1 = sun above the specified "horizon" 24 hours.
204 * *trise set to time when the sun is at south,
205 * minus 12 hours while *tset is set to the south
206 * time plus 12 hours. "Day" length = 24 hours
207 * -1 = sun is below the specified "horizon" 24 hours
208 * "Day" length = 0 hours, *trise and *tset are
209 * both set to the time when the sun is at south.
210 *
211 */
timelib_astro_rise_set_altitude(timelib_time * t_loc,double lon,double lat,double altit,int upper_limb,double * h_rise,double * h_set,timelib_sll * ts_rise,timelib_sll * ts_set,timelib_sll * ts_transit)212 int timelib_astro_rise_set_altitude(timelib_time *t_loc, double lon, double lat, double altit, int upper_limb, double *h_rise, double *h_set, timelib_sll *ts_rise, timelib_sll *ts_set, timelib_sll *ts_transit)
213 {
214 double d, /* Days since 2000 Jan 0.0 (negative before) */
215 sr, /* Solar distance, astronomical units */
216 sRA, /* Sun's Right Ascension */
217 sdec, /* Sun's declination */
218 sradius, /* Sun's apparent radius */
219 t, /* Diurnal arc */
220 tsouth, /* Time when Sun is at south */
221 sidtime; /* Local sidereal time */
222 timelib_time *t_utc;
223 timelib_sll timestamp, old_sse;
224
225 int rc = 0; /* Return cde from function - usually 0 */
226
227 /* Normalize time */
228 old_sse = t_loc->sse;
229 t_loc->h = 12;
230 t_loc->i = t_loc->s = 0;
231 timelib_update_ts(t_loc, NULL);
232
233 /* Calculate TS belonging to UTC 00:00 of the current day, for input into
234 * the algorithm */
235 t_utc = timelib_time_ctor();
236 t_utc->y = t_loc->y;
237 t_utc->m = t_loc->m;
238 t_utc->d = t_loc->d;
239 t_utc->h = t_utc->i = t_utc->s = 0;
240 timelib_update_ts(t_utc, NULL);
241
242 /* Compute d of 12h local mean solar time */
243 timestamp = t_utc->sse;
244 d = timelib_ts_to_j2000(timestamp) + 2 - lon/360.0;
245
246 /* Compute local sidereal time of this moment */
247 sidtime = astro_revolution(astro_GMST0(d) + 180.0 + lon);
248
249 /* Compute Sun's RA + Decl at this moment */
250 astro_sun_RA_dec( d, &sRA, &sdec, &sr );
251
252 /* Compute time when Sun is at south - in hours UT */
253 tsouth = 12.0 - astro_rev180(sidtime - sRA) / 15.0;
254
255 /* Compute the Sun's apparent radius, degrees */
256 sradius = 0.2666 / sr;
257
258 /* Do correction to upper limb, if necessary */
259 if (upper_limb) {
260 altit -= sradius;
261 }
262
263 /* Compute the diurnal arc that the Sun traverses to reach */
264 /* the specified altitude altit: */
265 {
266 double cost;
267 cost = (sind(altit) - sind(lat) * sind(sdec)) / (cosd(lat) * cosd(sdec));
268 *ts_transit = t_utc->sse + (tsouth * 3600);
269 if (cost >= 1.0) {
270 rc = -1;
271 t = 0.0; /* Sun always below altit */
272
273 *ts_rise = *ts_set = t_utc->sse + (tsouth * 3600);
274 } else if (cost <= -1.0) {
275 rc = +1;
276 t = 12.0; /* Sun always above altit */
277
278 *ts_rise = t_loc->sse - (12 * 3600);
279 *ts_set = t_loc->sse + (12 * 3600);
280 } else {
281 t = acosd(cost) / 15.0; /* The diurnal arc, hours */
282
283 /* Store rise and set times - as Unix Timestamp */
284 *ts_rise = ((tsouth - t) * 3600) + t_utc->sse;
285 *ts_set = ((tsouth + t) * 3600) + t_utc->sse;
286
287 *h_rise = (tsouth - t);
288 *h_set = (tsouth + t);
289 }
290 }
291
292 /* Kill temporary time and restore original sse */
293 timelib_time_dtor(t_utc);
294 t_loc->sse = old_sse;
295
296 return rc;
297 }
298
timelib_ts_to_julianday(timelib_sll ts)299 double timelib_ts_to_julianday(timelib_sll ts)
300 {
301 double tmp;
302
303 tmp = (double) ts;
304 tmp /= (double) 86400;
305 tmp += (double) 2440587.5;
306
307 return tmp;
308 }
309
timelib_ts_to_j2000(timelib_sll ts)310 double timelib_ts_to_j2000(timelib_sll ts)
311 {
312 return timelib_ts_to_julianday(ts) - 2451545;
313 }
314
