1.1 --- /dev/null Thu Jan 01 00:00:00 1970 +0000
1.2 +++ b/intl/icu/source/i18n/astro.cpp Wed Dec 31 06:09:35 2014 +0100
1.3 @@ -0,0 +1,1601 @@
1.4 +/************************************************************************
1.5 + * Copyright (C) 1996-2012, International Business Machines Corporation
1.6 + * and others. All Rights Reserved.
1.7 + ************************************************************************
1.8 + * 2003-nov-07 srl Port from Java
1.9 + */
1.10 +
1.11 +#include "astro.h"
1.12 +
1.13 +#if !UCONFIG_NO_FORMATTING
1.14 +
1.15 +#include "unicode/calendar.h"
1.16 +#include <math.h>
1.17 +#include <float.h>
1.18 +#include "unicode/putil.h"
1.19 +#include "uhash.h"
1.20 +#include "umutex.h"
1.21 +#include "ucln_in.h"
1.22 +#include "putilimp.h"
1.23 +#include <stdio.h> // for toString()
1.24 +
1.25 +#if defined (PI)
1.26 +#undef PI
1.27 +#endif
1.28 +
1.29 +#ifdef U_DEBUG_ASTRO
1.30 +# include "uresimp.h" // for debugging
1.31 +
1.32 +static void debug_astro_loc(const char *f, int32_t l)
1.33 +{
1.34 + fprintf(stderr, "%s:%d: ", f, l);
1.35 +}
1.36 +
1.37 +static void debug_astro_msg(const char *pat, ...)
1.38 +{
1.39 + va_list ap;
1.40 + va_start(ap, pat);
1.41 + vfprintf(stderr, pat, ap);
1.42 + fflush(stderr);
1.43 +}
1.44 +#include "unicode/datefmt.h"
1.45 +#include "unicode/ustring.h"
1.46 +static const char * debug_astro_date(UDate d) {
1.47 + static char gStrBuf[1024];
1.48 + static DateFormat *df = NULL;
1.49 + if(df == NULL) {
1.50 + df = DateFormat::createDateTimeInstance(DateFormat::MEDIUM, DateFormat::MEDIUM, Locale::getUS());
1.51 + df->adoptTimeZone(TimeZone::getGMT()->clone());
1.52 + }
1.53 + UnicodeString str;
1.54 + df->format(d,str);
1.55 + u_austrncpy(gStrBuf,str.getTerminatedBuffer(),sizeof(gStrBuf)-1);
1.56 + return gStrBuf;
1.57 +}
1.58 +
1.59 +// must use double parens, i.e.: U_DEBUG_ASTRO_MSG(("four is: %d",4));
1.60 +#define U_DEBUG_ASTRO_MSG(x) {debug_astro_loc(__FILE__,__LINE__);debug_astro_msg x;}
1.61 +#else
1.62 +#define U_DEBUG_ASTRO_MSG(x)
1.63 +#endif
1.64 +
1.65 +static inline UBool isINVALID(double d) {
1.66 + return(uprv_isNaN(d));
1.67 +}
1.68 +
1.69 +static UMutex ccLock = U_MUTEX_INITIALIZER;
1.70 +
1.71 +U_CDECL_BEGIN
1.72 +static UBool calendar_astro_cleanup(void) {
1.73 + return TRUE;
1.74 +}
1.75 +U_CDECL_END
1.76 +
1.77 +U_NAMESPACE_BEGIN
1.78 +
1.79 +/**
1.80 + * The number of standard hours in one sidereal day.
1.81 + * Approximately 24.93.
1.82 + * @internal
1.83 + * @deprecated ICU 2.4. This class may be removed or modified.
1.84 + */
1.85 +#define SIDEREAL_DAY (23.93446960027)
1.86 +
1.87 +/**
1.88 + * The number of sidereal hours in one mean solar day.
1.89 + * Approximately 24.07.
1.90 + * @internal
1.91 + * @deprecated ICU 2.4. This class may be removed or modified.
1.92 + */
1.93 +#define SOLAR_DAY (24.065709816)
1.94 +
1.95 +/**
1.96 + * The average number of solar days from one new moon to the next. This is the time
1.97 + * it takes for the moon to return the same ecliptic longitude as the sun.
1.98 + * It is longer than the sidereal month because the sun's longitude increases
1.99 + * during the year due to the revolution of the earth around the sun.
1.100 + * Approximately 29.53.
1.101 + *
1.102 + * @see #SIDEREAL_MONTH
1.103 + * @internal
1.104 + * @deprecated ICU 2.4. This class may be removed or modified.
1.105 + */
1.106 +const double CalendarAstronomer::SYNODIC_MONTH = 29.530588853;
1.107 +
1.108 +/**
1.109 + * The average number of days it takes
1.110 + * for the moon to return to the same ecliptic longitude relative to the
1.111 + * stellar background. This is referred to as the sidereal month.
1.112 + * It is shorter than the synodic month due to
1.113 + * the revolution of the earth around the sun.
1.114 + * Approximately 27.32.
1.115 + *
1.116 + * @see #SYNODIC_MONTH
1.117 + * @internal
1.118 + * @deprecated ICU 2.4. This class may be removed or modified.
1.119 + */
1.120 +#define SIDEREAL_MONTH 27.32166
1.121 +
1.122 +/**
1.123 + * The average number number of days between successive vernal equinoxes.
1.124 + * Due to the precession of the earth's
1.125 + * axis, this is not precisely the same as the sidereal year.
1.126 + * Approximately 365.24
1.127 + *
1.128 + * @see #SIDEREAL_YEAR
1.129 + * @internal
1.130 + * @deprecated ICU 2.4. This class may be removed or modified.
1.131 + */
1.132 +#define TROPICAL_YEAR 365.242191
1.133 +
1.134 +/**
1.135 + * The average number of days it takes
1.136 + * for the sun to return to the same position against the fixed stellar
1.137 + * background. This is the duration of one orbit of the earth about the sun
1.138 + * as it would appear to an outside observer.
1.139 + * Due to the precession of the earth's
1.140 + * axis, this is not precisely the same as the tropical year.
1.141 + * Approximately 365.25.
1.142 + *
1.143 + * @see #TROPICAL_YEAR
1.144 + * @internal
1.145 + * @deprecated ICU 2.4. This class may be removed or modified.
1.146 + */
1.147 +#define SIDEREAL_YEAR 365.25636
1.148 +
1.149 +//-------------------------------------------------------------------------
1.150 +// Time-related constants
1.151 +//-------------------------------------------------------------------------
1.152 +
1.153 +/**
1.154 + * The number of milliseconds in one second.
1.155 + * @internal
1.156 + * @deprecated ICU 2.4. This class may be removed or modified.
1.157 + */
1.158 +#define SECOND_MS U_MILLIS_PER_SECOND
1.159 +
1.160 +/**
1.161 + * The number of milliseconds in one minute.
1.162 + * @internal
1.163 + * @deprecated ICU 2.4. This class may be removed or modified.
1.164 + */
1.165 +#define MINUTE_MS U_MILLIS_PER_MINUTE
1.166 +
1.167 +/**
1.168 + * The number of milliseconds in one hour.
1.169 + * @internal
1.170 + * @deprecated ICU 2.4. This class may be removed or modified.
1.171 + */
1.172 +#define HOUR_MS U_MILLIS_PER_HOUR
1.173 +
1.174 +/**
1.175 + * The number of milliseconds in one day.
1.176 + * @internal
1.177 + * @deprecated ICU 2.4. This class may be removed or modified.
1.178 + */
1.179 +#define DAY_MS U_MILLIS_PER_DAY
1.180 +
1.181 +/**
1.182 + * The start of the julian day numbering scheme used by astronomers, which
1.183 + * is 1/1/4713 BC (Julian), 12:00 GMT. This is given as the number of milliseconds
1.184 + * since 1/1/1970 AD (Gregorian), a negative number.
1.185 + * Note that julian day numbers and
1.186 + * the Julian calendar are <em>not</em> the same thing. Also note that
1.187 + * julian days start at <em>noon</em>, not midnight.
1.188 + * @internal
1.189 + * @deprecated ICU 2.4. This class may be removed or modified.
1.190 + */
1.191 +#define JULIAN_EPOCH_MS -210866760000000.0
1.192 +
1.193 +
1.194 +/**
1.195 + * Milliseconds value for 0.0 January 2000 AD.
1.196 + */
1.197 +#define EPOCH_2000_MS 946598400000.0
1.198 +
1.199 +//-------------------------------------------------------------------------
1.200 +// Assorted private data used for conversions
1.201 +//-------------------------------------------------------------------------
1.202 +
1.203 +// My own copies of these so compilers are more likely to optimize them away
1.204 +const double CalendarAstronomer::PI = 3.14159265358979323846;
1.205 +
1.206 +#define CalendarAstronomer_PI2 (CalendarAstronomer::PI*2.0)
1.207 +#define RAD_HOUR ( 12 / CalendarAstronomer::PI ) // radians -> hours
1.208 +#define DEG_RAD ( CalendarAstronomer::PI / 180 ) // degrees -> radians
1.209 +#define RAD_DEG ( 180 / CalendarAstronomer::PI ) // radians -> degrees
1.210 +
1.211 +/***
1.212 + * Given 'value', add or subtract 'range' until 0 <= 'value' < range.
1.213 + * The modulus operator.
1.214 + */
1.215 +inline static double normalize(double value, double range) {
1.216 + return value - range * ClockMath::floorDivide(value, range);
1.217 +}
1.218 +
1.219 +/**
1.220 + * Normalize an angle so that it's in the range 0 - 2pi.
1.221 + * For positive angles this is just (angle % 2pi), but the Java
1.222 + * mod operator doesn't work that way for negative numbers....
1.223 + */
1.224 +inline static double norm2PI(double angle) {
1.225 + return normalize(angle, CalendarAstronomer::PI * 2.0);
1.226 +}
1.227 +
1.228 +/**
1.229 + * Normalize an angle into the range -PI - PI
1.230 + */
1.231 +inline static double normPI(double angle) {
1.232 + return normalize(angle + CalendarAstronomer::PI, CalendarAstronomer::PI * 2.0) - CalendarAstronomer::PI;
1.233 +}
1.234 +
1.235 +//-------------------------------------------------------------------------
1.236 +// Constructors
1.237 +//-------------------------------------------------------------------------
1.238 +
1.239 +/**
1.240 + * Construct a new <code>CalendarAstronomer</code> object that is initialized to
1.241 + * the current date and time.
1.242 + * @internal
1.243 + * @deprecated ICU 2.4. This class may be removed or modified.
1.244 + */
1.245 +CalendarAstronomer::CalendarAstronomer():
1.246 + fTime(Calendar::getNow()), fLongitude(0.0), fLatitude(0.0), fGmtOffset(0.0), moonPosition(0,0), moonPositionSet(FALSE) {
1.247 + clearCache();
1.248 +}
1.249 +
1.250 +/**
1.251 + * Construct a new <code>CalendarAstronomer</code> object that is initialized to
1.252 + * the specified date and time.
1.253 + * @internal
1.254 + * @deprecated ICU 2.4. This class may be removed or modified.
1.255 + */
1.256 +CalendarAstronomer::CalendarAstronomer(UDate d): fTime(d), fLongitude(0.0), fLatitude(0.0), fGmtOffset(0.0), moonPosition(0,0), moonPositionSet(FALSE) {
1.257 + clearCache();
1.258 +}
1.259 +
1.260 +/**
1.261 + * Construct a new <code>CalendarAstronomer</code> object with the given
1.262 + * latitude and longitude. The object's time is set to the current
1.263 + * date and time.
1.264 + * <p>
1.265 + * @param longitude The desired longitude, in <em>degrees</em> east of
1.266 + * the Greenwich meridian.
1.267 + *
1.268 + * @param latitude The desired latitude, in <em>degrees</em>. Positive
1.269 + * values signify North, negative South.
1.270 + *
1.271 + * @see java.util.Date#getTime()
1.272 + * @internal
1.273 + * @deprecated ICU 2.4. This class may be removed or modified.
1.274 + */
1.275 +CalendarAstronomer::CalendarAstronomer(double longitude, double latitude) :
1.276 + fTime(Calendar::getNow()), moonPosition(0,0), moonPositionSet(FALSE) {
1.277 + fLongitude = normPI(longitude * (double)DEG_RAD);
1.278 + fLatitude = normPI(latitude * (double)DEG_RAD);
1.279 + fGmtOffset = (double)(fLongitude * 24. * (double)HOUR_MS / (double)CalendarAstronomer_PI2);
1.280 + clearCache();
1.281 +}
1.282 +
1.283 +CalendarAstronomer::~CalendarAstronomer()
1.284 +{
1.285 +}
1.286 +
1.287 +//-------------------------------------------------------------------------
1.288 +// Time and date getters and setters
1.289 +//-------------------------------------------------------------------------
1.290 +
1.291 +/**
1.292 + * Set the current date and time of this <code>CalendarAstronomer</code> object. All
1.293 + * astronomical calculations are performed based on this time setting.
1.294 + *
1.295 + * @param aTime the date and time, expressed as the number of milliseconds since
1.296 + * 1/1/1970 0:00 GMT (Gregorian).
1.297 + *
1.298 + * @see #setDate
1.299 + * @see #getTime
1.300 + * @internal
1.301 + * @deprecated ICU 2.4. This class may be removed or modified.
1.302 + */
1.303 +void CalendarAstronomer::setTime(UDate aTime) {
1.304 + fTime = aTime;
1.305 + U_DEBUG_ASTRO_MSG(("setTime(%.1lf, %sL)\n", aTime, debug_astro_date(aTime+fGmtOffset)));
1.306 + clearCache();
1.307 +}
1.308 +
1.309 +/**
1.310 + * Set the current date and time of this <code>CalendarAstronomer</code> object. All
1.311 + * astronomical calculations are performed based on this time setting.
1.312 + *
1.313 + * @param jdn the desired time, expressed as a "julian day number",
1.314 + * which is the number of elapsed days since
1.315 + * 1/1/4713 BC (Julian), 12:00 GMT. Note that julian day
1.316 + * numbers start at <em>noon</em>. To get the jdn for
1.317 + * the corresponding midnight, subtract 0.5.
1.318 + *
1.319 + * @see #getJulianDay
1.320 + * @see #JULIAN_EPOCH_MS
1.321 + * @internal
1.322 + * @deprecated ICU 2.4. This class may be removed or modified.
1.323 + */
1.324 +void CalendarAstronomer::setJulianDay(double jdn) {
1.325 + fTime = (double)(jdn * DAY_MS) + JULIAN_EPOCH_MS;
1.326 + clearCache();
1.327 + julianDay = jdn;
1.328 +}
1.329 +
1.330 +/**
1.331 + * Get the current time of this <code>CalendarAstronomer</code> object,
1.332 + * represented as the number of milliseconds since
1.333 + * 1/1/1970 AD 0:00 GMT (Gregorian).
1.334 + *
1.335 + * @see #setTime
1.336 + * @see #getDate
1.337 + * @internal
1.338 + * @deprecated ICU 2.4. This class may be removed or modified.
1.339 + */
1.340 +UDate CalendarAstronomer::getTime() {
1.341 + return fTime;
1.342 +}
1.343 +
1.344 +/**
1.345 + * Get the current time of this <code>CalendarAstronomer</code> object,
1.346 + * expressed as a "julian day number", which is the number of elapsed
1.347 + * days since 1/1/4713 BC (Julian), 12:00 GMT.
1.348 + *
1.349 + * @see #setJulianDay
1.350 + * @see #JULIAN_EPOCH_MS
1.351 + * @internal
1.352 + * @deprecated ICU 2.4. This class may be removed or modified.
1.353 + */
1.354 +double CalendarAstronomer::getJulianDay() {
1.355 + if (isINVALID(julianDay)) {
1.356 + julianDay = (fTime - (double)JULIAN_EPOCH_MS) / (double)DAY_MS;
1.357 + }
1.358 + return julianDay;
1.359 +}
1.360 +
1.361 +/**
1.362 + * Return this object's time expressed in julian centuries:
1.363 + * the number of centuries after 1/1/1900 AD, 12:00 GMT
1.364 + *
1.365 + * @see #getJulianDay
1.366 + * @internal
1.367 + * @deprecated ICU 2.4. This class may be removed or modified.
1.368 + */
1.369 +double CalendarAstronomer::getJulianCentury() {
1.370 + if (isINVALID(julianCentury)) {
1.371 + julianCentury = (getJulianDay() - 2415020.0) / 36525.0;
1.372 + }
1.373 + return julianCentury;
1.374 +}
1.375 +
1.376 +/**
1.377 + * Returns the current Greenwich sidereal time, measured in hours
1.378 + * @internal
1.379 + * @deprecated ICU 2.4. This class may be removed or modified.
1.380 + */
1.381 +double CalendarAstronomer::getGreenwichSidereal() {
1.382 + if (isINVALID(siderealTime)) {
1.383 + // See page 86 of "Practial Astronomy with your Calculator",
1.384 + // by Peter Duffet-Smith, for details on the algorithm.
1.385 +
1.386 + double UT = normalize(fTime/(double)HOUR_MS, 24.);
1.387 +
1.388 + siderealTime = normalize(getSiderealOffset() + UT*1.002737909, 24.);
1.389 + }
1.390 + return siderealTime;
1.391 +}
1.392 +
1.393 +double CalendarAstronomer::getSiderealOffset() {
1.394 + if (isINVALID(siderealT0)) {
1.395 + double JD = uprv_floor(getJulianDay() - 0.5) + 0.5;
1.396 + double S = JD - 2451545.0;
1.397 + double T = S / 36525.0;
1.398 + siderealT0 = normalize(6.697374558 + 2400.051336*T + 0.000025862*T*T, 24);
1.399 + }
1.400 + return siderealT0;
1.401 +}
1.402 +
1.403 +/**
1.404 + * Returns the current local sidereal time, measured in hours
1.405 + * @internal
1.406 + * @deprecated ICU 2.4. This class may be removed or modified.
1.407 + */
1.408 +double CalendarAstronomer::getLocalSidereal() {
1.409 + return normalize(getGreenwichSidereal() + (fGmtOffset/(double)HOUR_MS), 24.);
1.410 +}
1.411 +
1.412 +/**
1.413 + * Converts local sidereal time to Universal Time.
1.414 + *
1.415 + * @param lst The Local Sidereal Time, in hours since sidereal midnight
1.416 + * on this object's current date.
1.417 + *
1.418 + * @return The corresponding Universal Time, in milliseconds since
1.419 + * 1 Jan 1970, GMT.
1.420 + */
1.421 +double CalendarAstronomer::lstToUT(double lst) {
1.422 + // Convert to local mean time
1.423 + double lt = normalize((lst - getSiderealOffset()) * 0.9972695663, 24);
1.424 +
1.425 + // Then find local midnight on this day
1.426 + double base = (DAY_MS * ClockMath::floorDivide(fTime + fGmtOffset,(double)DAY_MS)) - fGmtOffset;
1.427 +
1.428 + //out(" lt =" + lt + " hours");
1.429 + //out(" base=" + new Date(base));
1.430 +
1.431 + return base + (long)(lt * HOUR_MS);
1.432 +}
1.433 +
1.434 +
1.435 +//-------------------------------------------------------------------------
1.436 +// Coordinate transformations, all based on the current time of this object
1.437 +//-------------------------------------------------------------------------
1.438 +
1.439 +/**
1.440 + * Convert from ecliptic to equatorial coordinates.
1.441 + *
1.442 + * @param ecliptic A point in the sky in ecliptic coordinates.
1.443 + * @return The corresponding point in equatorial coordinates.
1.444 + * @internal
1.445 + * @deprecated ICU 2.4. This class may be removed or modified.
1.446 + */
1.447 +CalendarAstronomer::Equatorial& CalendarAstronomer::eclipticToEquatorial(CalendarAstronomer::Equatorial& result, const CalendarAstronomer::Ecliptic& ecliptic)
1.448 +{
1.449 + return eclipticToEquatorial(result, ecliptic.longitude, ecliptic.latitude);
1.450 +}
1.451 +
1.452 +/**
1.453 + * Convert from ecliptic to equatorial coordinates.
1.454 + *
1.455 + * @param eclipLong The ecliptic longitude
1.456 + * @param eclipLat The ecliptic latitude
1.457 + *
1.458 + * @return The corresponding point in equatorial coordinates.
1.459 + * @internal
1.460 + * @deprecated ICU 2.4. This class may be removed or modified.
1.461 + */
1.462 +CalendarAstronomer::Equatorial& CalendarAstronomer::eclipticToEquatorial(CalendarAstronomer::Equatorial& result, double eclipLong, double eclipLat)
1.463 +{
1.464 + // See page 42 of "Practial Astronomy with your Calculator",
1.465 + // by Peter Duffet-Smith, for details on the algorithm.
1.466 +
1.467 + double obliq = eclipticObliquity();
1.468 + double sinE = ::sin(obliq);
1.469 + double cosE = cos(obliq);
1.470 +
1.471 + double sinL = ::sin(eclipLong);
1.472 + double cosL = cos(eclipLong);
1.473 +
1.474 + double sinB = ::sin(eclipLat);
1.475 + double cosB = cos(eclipLat);
1.476 + double tanB = tan(eclipLat);
1.477 +
1.478 + result.set(atan2(sinL*cosE - tanB*sinE, cosL),
1.479 + asin(sinB*cosE + cosB*sinE*sinL) );
1.480 + return result;
1.481 +}
1.482 +
1.483 +/**
1.484 + * Convert from ecliptic longitude to equatorial coordinates.
1.485 + *
1.486 + * @param eclipLong The ecliptic longitude
1.487 + *
1.488 + * @return The corresponding point in equatorial coordinates.
1.489 + * @internal
1.490 + * @deprecated ICU 2.4. This class may be removed or modified.
1.491 + */
1.492 +CalendarAstronomer::Equatorial& CalendarAstronomer::eclipticToEquatorial(CalendarAstronomer::Equatorial& result, double eclipLong)
1.493 +{
1.494 + return eclipticToEquatorial(result, eclipLong, 0); // TODO: optimize
1.495 +}
1.496 +
1.497 +/**
1.498 + * @internal
1.499 + * @deprecated ICU 2.4. This class may be removed or modified.
1.500 + */
1.501 +CalendarAstronomer::Horizon& CalendarAstronomer::eclipticToHorizon(CalendarAstronomer::Horizon& result, double eclipLong)
1.502 +{
1.503 + Equatorial equatorial;
1.504 + eclipticToEquatorial(equatorial, eclipLong);
1.505 +
1.506 + double H = getLocalSidereal()*CalendarAstronomer::PI/12 - equatorial.ascension; // Hour-angle
1.507 +
1.508 + double sinH = ::sin(H);
1.509 + double cosH = cos(H);
1.510 + double sinD = ::sin(equatorial.declination);
1.511 + double cosD = cos(equatorial.declination);
1.512 + double sinL = ::sin(fLatitude);
1.513 + double cosL = cos(fLatitude);
1.514 +
1.515 + double altitude = asin(sinD*sinL + cosD*cosL*cosH);
1.516 + double azimuth = atan2(-cosD*cosL*sinH, sinD - sinL * ::sin(altitude));
1.517 +
1.518 + result.set(azimuth, altitude);
1.519 + return result;
1.520 +}
1.521 +
1.522 +
1.523 +//-------------------------------------------------------------------------
1.524 +// The Sun
1.525 +//-------------------------------------------------------------------------
1.526 +
1.527 +//
1.528 +// Parameters of the Sun's orbit as of the epoch Jan 0.0 1990
1.529 +// Angles are in radians (after multiplying by CalendarAstronomer::PI/180)
1.530 +//
1.531 +#define JD_EPOCH 2447891.5 // Julian day of epoch
1.532 +
1.533 +#define SUN_ETA_G (279.403303 * CalendarAstronomer::PI/180) // Ecliptic longitude at epoch
1.534 +#define SUN_OMEGA_G (282.768422 * CalendarAstronomer::PI/180) // Ecliptic longitude of perigee
1.535 +#define SUN_E 0.016713 // Eccentricity of orbit
1.536 +//double sunR0 1.495585e8 // Semi-major axis in KM
1.537 +//double sunTheta0 (0.533128 * CalendarAstronomer::PI/180) // Angular diameter at R0
1.538 +
1.539 +// The following three methods, which compute the sun parameters
1.540 +// given above for an arbitrary epoch (whatever time the object is
1.541 +// set to), make only a small difference as compared to using the
1.542 +// above constants. E.g., Sunset times might differ by ~12
1.543 +// seconds. Furthermore, the eta-g computation is befuddled by
1.544 +// Duffet-Smith's incorrect coefficients (p.86). I've corrected
1.545 +// the first-order coefficient but the others may be off too - no
1.546 +// way of knowing without consulting another source.
1.547 +
1.548 +// /**
1.549 +// * Return the sun's ecliptic longitude at perigee for the current time.
1.550 +// * See Duffett-Smith, p. 86.
1.551 +// * @return radians
1.552 +// */
1.553 +// private double getSunOmegaG() {
1.554 +// double T = getJulianCentury();
1.555 +// return (281.2208444 + (1.719175 + 0.000452778*T)*T) * DEG_RAD;
1.556 +// }
1.557 +
1.558 +// /**
1.559 +// * Return the sun's ecliptic longitude for the current time.
1.560 +// * See Duffett-Smith, p. 86.
1.561 +// * @return radians
1.562 +// */
1.563 +// private double getSunEtaG() {
1.564 +// double T = getJulianCentury();
1.565 +// //return (279.6966778 + (36000.76892 + 0.0003025*T)*T) * DEG_RAD;
1.566 +// //
1.567 +// // The above line is from Duffett-Smith, and yields manifestly wrong
1.568 +// // results. The below constant is derived empirically to match the
1.569 +// // constant he gives for the 1990 EPOCH.
1.570 +// //
1.571 +// return (279.6966778 + (-0.3262541582718024 + 0.0003025*T)*T) * DEG_RAD;
1.572 +// }
1.573 +
1.574 +// /**
1.575 +// * Return the sun's eccentricity of orbit for the current time.
1.576 +// * See Duffett-Smith, p. 86.
1.577 +// * @return double
1.578 +// */
1.579 +// private double getSunE() {
1.580 +// double T = getJulianCentury();
1.581 +// return 0.01675104 - (0.0000418 + 0.000000126*T)*T;
1.582 +// }
1.583 +
1.584 +/**
1.585 + * Find the "true anomaly" (longitude) of an object from
1.586 + * its mean anomaly and the eccentricity of its orbit. This uses
1.587 + * an iterative solution to Kepler's equation.
1.588 + *
1.589 + * @param meanAnomaly The object's longitude calculated as if it were in
1.590 + * a regular, circular orbit, measured in radians
1.591 + * from the point of perigee.
1.592 + *
1.593 + * @param eccentricity The eccentricity of the orbit
1.594 + *
1.595 + * @return The true anomaly (longitude) measured in radians
1.596 + */
1.597 +static double trueAnomaly(double meanAnomaly, double eccentricity)
1.598 +{
1.599 + // First, solve Kepler's equation iteratively
1.600 + // Duffett-Smith, p.90
1.601 + double delta;
1.602 + double E = meanAnomaly;
1.603 + do {
1.604 + delta = E - eccentricity * ::sin(E) - meanAnomaly;
1.605 + E = E - delta / (1 - eccentricity * ::cos(E));
1.606 + }
1.607 + while (uprv_fabs(delta) > 1e-5); // epsilon = 1e-5 rad
1.608 +
1.609 + return 2.0 * ::atan( ::tan(E/2) * ::sqrt( (1+eccentricity)
1.610 + /(1-eccentricity) ) );
1.611 +}
1.612 +
1.613 +/**
1.614 + * The longitude of the sun at the time specified by this object.
1.615 + * The longitude is measured in radians along the ecliptic
1.616 + * from the "first point of Aries," the point at which the ecliptic
1.617 + * crosses the earth's equatorial plane at the vernal equinox.
1.618 + * <p>
1.619 + * Currently, this method uses an approximation of the two-body Kepler's
1.620 + * equation for the earth and the sun. It does not take into account the
1.621 + * perturbations caused by the other planets, the moon, etc.
1.622 + * @internal
1.623 + * @deprecated ICU 2.4. This class may be removed or modified.
1.624 + */
1.625 +double CalendarAstronomer::getSunLongitude()
1.626 +{
1.627 + // See page 86 of "Practial Astronomy with your Calculator",
1.628 + // by Peter Duffet-Smith, for details on the algorithm.
1.629 +
1.630 + if (isINVALID(sunLongitude)) {
1.631 + getSunLongitude(getJulianDay(), sunLongitude, meanAnomalySun);
1.632 + }
1.633 + return sunLongitude;
1.634 +}
1.635 +
1.636 +/**
1.637 + * TODO Make this public when the entire class is package-private.
1.638 + */
1.639 +/*public*/ void CalendarAstronomer::getSunLongitude(double jDay, double &longitude, double &meanAnomaly)
1.640 +{
1.641 + // See page 86 of "Practial Astronomy with your Calculator",
1.642 + // by Peter Duffet-Smith, for details on the algorithm.
1.643 +
1.644 + double day = jDay - JD_EPOCH; // Days since epoch
1.645 +
1.646 + // Find the angular distance the sun in a fictitious
1.647 + // circular orbit has travelled since the epoch.
1.648 + double epochAngle = norm2PI(CalendarAstronomer_PI2/TROPICAL_YEAR*day);
1.649 +
1.650 + // The epoch wasn't at the sun's perigee; find the angular distance
1.651 + // since perigee, which is called the "mean anomaly"
1.652 + meanAnomaly = norm2PI(epochAngle + SUN_ETA_G - SUN_OMEGA_G);
1.653 +
1.654 + // Now find the "true anomaly", e.g. the real solar longitude
1.655 + // by solving Kepler's equation for an elliptical orbit
1.656 + // NOTE: The 3rd ed. of the book lists omega_g and eta_g in different
1.657 + // equations; omega_g is to be correct.
1.658 + longitude = norm2PI(trueAnomaly(meanAnomaly, SUN_E) + SUN_OMEGA_G);
1.659 +}
1.660 +
1.661 +/**
1.662 + * The position of the sun at this object's current date and time,
1.663 + * in equatorial coordinates.
1.664 + * @internal
1.665 + * @deprecated ICU 2.4. This class may be removed or modified.
1.666 + */
1.667 +CalendarAstronomer::Equatorial& CalendarAstronomer::getSunPosition(CalendarAstronomer::Equatorial& result) {
1.668 + return eclipticToEquatorial(result, getSunLongitude(), 0);
1.669 +}
1.670 +
1.671 +
1.672 +/**
1.673 + * Constant representing the vernal equinox.
1.674 + * For use with {@link #getSunTime getSunTime}.
1.675 + * Note: In this case, "vernal" refers to the northern hemisphere's seasons.
1.676 + * @internal
1.677 + * @deprecated ICU 2.4. This class may be removed or modified.
1.678 + */
1.679 +/*double CalendarAstronomer::VERNAL_EQUINOX() {
1.680 + return 0;
1.681 +}*/
1.682 +
1.683 +/**
1.684 + * Constant representing the summer solstice.
1.685 + * For use with {@link #getSunTime getSunTime}.
1.686 + * Note: In this case, "summer" refers to the northern hemisphere's seasons.
1.687 + * @internal
1.688 + * @deprecated ICU 2.4. This class may be removed or modified.
1.689 + */
1.690 +double CalendarAstronomer::SUMMER_SOLSTICE() {
1.691 + return (CalendarAstronomer::PI/2);
1.692 +}
1.693 +
1.694 +/**
1.695 + * Constant representing the autumnal equinox.
1.696 + * For use with {@link #getSunTime getSunTime}.
1.697 + * Note: In this case, "autumn" refers to the northern hemisphere's seasons.
1.698 + * @internal
1.699 + * @deprecated ICU 2.4. This class may be removed or modified.
1.700 + */
1.701 +/*double CalendarAstronomer::AUTUMN_EQUINOX() {
1.702 + return (CalendarAstronomer::PI);
1.703 +}*/
1.704 +
1.705 +/**
1.706 + * Constant representing the winter solstice.
1.707 + * For use with {@link #getSunTime getSunTime}.
1.708 + * Note: In this case, "winter" refers to the northern hemisphere's seasons.
1.709 + * @internal
1.710 + * @deprecated ICU 2.4. This class may be removed or modified.
1.711 + */
1.712 +double CalendarAstronomer::WINTER_SOLSTICE() {
1.713 + return ((CalendarAstronomer::PI*3)/2);
1.714 +}
1.715 +
1.716 +CalendarAstronomer::AngleFunc::~AngleFunc() {}
1.717 +
1.718 +/**
1.719 + * Find the next time at which the sun's ecliptic longitude will have
1.720 + * the desired value.
1.721 + * @internal
1.722 + * @deprecated ICU 2.4. This class may be removed or modified.
1.723 + */
1.724 +class SunTimeAngleFunc : public CalendarAstronomer::AngleFunc {
1.725 +public:
1.726 + virtual ~SunTimeAngleFunc();
1.727 + virtual double eval(CalendarAstronomer& a) { return a.getSunLongitude(); }
1.728 +};
1.729 +
1.730 +SunTimeAngleFunc::~SunTimeAngleFunc() {}
1.731 +
1.732 +UDate CalendarAstronomer::getSunTime(double desired, UBool next)
1.733 +{
1.734 + SunTimeAngleFunc func;
1.735 + return timeOfAngle( func,
1.736 + desired,
1.737 + TROPICAL_YEAR,
1.738 + MINUTE_MS,
1.739 + next);
1.740 +}
1.741 +
1.742 +CalendarAstronomer::CoordFunc::~CoordFunc() {}
1.743 +
1.744 +class RiseSetCoordFunc : public CalendarAstronomer::CoordFunc {
1.745 +public:
1.746 + virtual ~RiseSetCoordFunc();
1.747 + virtual void eval(CalendarAstronomer::Equatorial& result, CalendarAstronomer&a) { a.getSunPosition(result); }
1.748 +};
1.749 +
1.750 +RiseSetCoordFunc::~RiseSetCoordFunc() {}
1.751 +
1.752 +UDate CalendarAstronomer::getSunRiseSet(UBool rise)
1.753 +{
1.754 + UDate t0 = fTime;
1.755 +
1.756 + // Make a rough guess: 6am or 6pm local time on the current day
1.757 + double noon = ClockMath::floorDivide(fTime + fGmtOffset, (double)DAY_MS)*DAY_MS - fGmtOffset + (12*HOUR_MS);
1.758 +
1.759 + U_DEBUG_ASTRO_MSG(("Noon=%.2lf, %sL, gmtoff %.2lf\n", noon, debug_astro_date(noon+fGmtOffset), fGmtOffset));
1.760 + setTime(noon + ((rise ? -6 : 6) * HOUR_MS));
1.761 + U_DEBUG_ASTRO_MSG(("added %.2lf ms as a guess,\n", ((rise ? -6. : 6.) * HOUR_MS)));
1.762 +
1.763 + RiseSetCoordFunc func;
1.764 + double t = riseOrSet(func,
1.765 + rise,
1.766 + .533 * DEG_RAD, // Angular Diameter
1.767 + 34. /60.0 * DEG_RAD, // Refraction correction
1.768 + MINUTE_MS / 12.); // Desired accuracy
1.769 +
1.770 + setTime(t0);
1.771 + return t;
1.772 +}
1.773 +
1.774 +// Commented out - currently unused. ICU 2.6, Alan
1.775 +// //-------------------------------------------------------------------------
1.776 +// // Alternate Sun Rise/Set
1.777 +// // See Duffett-Smith p.93
1.778 +// //-------------------------------------------------------------------------
1.779 +//
1.780 +// // This yields worse results (as compared to USNO data) than getSunRiseSet().
1.781 +// /**
1.782 +// * TODO Make this when the entire class is package-private.
1.783 +// */
1.784 +// /*public*/ long getSunRiseSet2(boolean rise) {
1.785 +// // 1. Calculate coordinates of the sun's center for midnight
1.786 +// double jd = uprv_floor(getJulianDay() - 0.5) + 0.5;
1.787 +// double[] sl = getSunLongitude(jd);// double lambda1 = sl[0];
1.788 +// Equatorial pos1 = eclipticToEquatorial(lambda1, 0);
1.789 +//
1.790 +// // 2. Add ... to lambda to get position 24 hours later
1.791 +// double lambda2 = lambda1 + 0.985647*DEG_RAD;
1.792 +// Equatorial pos2 = eclipticToEquatorial(lambda2, 0);
1.793 +//
1.794 +// // 3. Calculate LSTs of rising and setting for these two positions
1.795 +// double tanL = ::tan(fLatitude);
1.796 +// double H = ::acos(-tanL * ::tan(pos1.declination));
1.797 +// double lst1r = (CalendarAstronomer_PI2 + pos1.ascension - H) * 24 / CalendarAstronomer_PI2;
1.798 +// double lst1s = (pos1.ascension + H) * 24 / CalendarAstronomer_PI2;
1.799 +// H = ::acos(-tanL * ::tan(pos2.declination));
1.800 +// double lst2r = (CalendarAstronomer_PI2-H + pos2.ascension ) * 24 / CalendarAstronomer_PI2;
1.801 +// double lst2s = (H + pos2.ascension ) * 24 / CalendarAstronomer_PI2;
1.802 +// if (lst1r > 24) lst1r -= 24;
1.803 +// if (lst1s > 24) lst1s -= 24;
1.804 +// if (lst2r > 24) lst2r -= 24;
1.805 +// if (lst2s > 24) lst2s -= 24;
1.806 +//
1.807 +// // 4. Convert LSTs to GSTs. If GST1 > GST2, add 24 to GST2.
1.808 +// double gst1r = lstToGst(lst1r);
1.809 +// double gst1s = lstToGst(lst1s);
1.810 +// double gst2r = lstToGst(lst2r);
1.811 +// double gst2s = lstToGst(lst2s);
1.812 +// if (gst1r > gst2r) gst2r += 24;
1.813 +// if (gst1s > gst2s) gst2s += 24;
1.814 +//
1.815 +// // 5. Calculate GST at 0h UT of this date
1.816 +// double t00 = utToGst(0);
1.817 +//
1.818 +// // 6. Calculate GST at 0h on the observer's longitude
1.819 +// double offset = ::round(fLongitude*12/PI); // p.95 step 6; he _rounds_ to nearest 15 deg.
1.820 +// double t00p = t00 - offset*1.002737909;
1.821 +// if (t00p < 0) t00p += 24; // do NOT normalize
1.822 +//
1.823 +// // 7. Adjust
1.824 +// if (gst1r < t00p) {
1.825 +// gst1r += 24;
1.826 +// gst2r += 24;
1.827 +// }
1.828 +// if (gst1s < t00p) {
1.829 +// gst1s += 24;
1.830 +// gst2s += 24;
1.831 +// }
1.832 +//
1.833 +// // 8.
1.834 +// double gstr = (24.07*gst1r-t00*(gst2r-gst1r))/(24.07+gst1r-gst2r);
1.835 +// double gsts = (24.07*gst1s-t00*(gst2s-gst1s))/(24.07+gst1s-gst2s);
1.836 +//
1.837 +// // 9. Correct for parallax, refraction, and sun's diameter
1.838 +// double dec = (pos1.declination + pos2.declination) / 2;
1.839 +// double psi = ::acos(sin(fLatitude) / cos(dec));
1.840 +// double x = 0.830725 * DEG_RAD; // parallax+refraction+diameter
1.841 +// double y = ::asin(sin(x) / ::sin(psi)) * RAD_DEG;
1.842 +// double delta_t = 240 * y / cos(dec) / 3600; // hours
1.843 +//
1.844 +// // 10. Add correction to GSTs, subtract from GSTr
1.845 +// gstr -= delta_t;
1.846 +// gsts += delta_t;
1.847 +//
1.848 +// // 11. Convert GST to UT and then to local civil time
1.849 +// double ut = gstToUt(rise ? gstr : gsts);
1.850 +// //System.out.println((rise?"rise=":"set=") + ut + ", delta_t=" + delta_t);
1.851 +// long midnight = DAY_MS * (time / DAY_MS); // Find UT midnight on this day
1.852 +// return midnight + (long) (ut * 3600000);
1.853 +// }
1.854 +
1.855 +// Commented out - currently unused. ICU 2.6, Alan
1.856 +// /**
1.857 +// * Convert local sidereal time to Greenwich sidereal time.
1.858 +// * Section 15. Duffett-Smith p.21
1.859 +// * @param lst in hours (0..24)
1.860 +// * @return GST in hours (0..24)
1.861 +// */
1.862 +// double lstToGst(double lst) {
1.863 +// double delta = fLongitude * 24 / CalendarAstronomer_PI2;
1.864 +// return normalize(lst - delta, 24);
1.865 +// }
1.866 +
1.867 +// Commented out - currently unused. ICU 2.6, Alan
1.868 +// /**
1.869 +// * Convert UT to GST on this date.
1.870 +// * Section 12. Duffett-Smith p.17
1.871 +// * @param ut in hours
1.872 +// * @return GST in hours
1.873 +// */
1.874 +// double utToGst(double ut) {
1.875 +// return normalize(getT0() + ut*1.002737909, 24);
1.876 +// }
1.877 +
1.878 +// Commented out - currently unused. ICU 2.6, Alan
1.879 +// /**
1.880 +// * Convert GST to UT on this date.
1.881 +// * Section 13. Duffett-Smith p.18
1.882 +// * @param gst in hours
1.883 +// * @return UT in hours
1.884 +// */
1.885 +// double gstToUt(double gst) {
1.886 +// return normalize(gst - getT0(), 24) * 0.9972695663;
1.887 +// }
1.888 +
1.889 +// Commented out - currently unused. ICU 2.6, Alan
1.890 +// double getT0() {
1.891 +// // Common computation for UT <=> GST
1.892 +//
1.893 +// // Find JD for 0h UT
1.894 +// double jd = uprv_floor(getJulianDay() - 0.5) + 0.5;
1.895 +//
1.896 +// double s = jd - 2451545.0;
1.897 +// double t = s / 36525.0;
1.898 +// double t0 = 6.697374558 + (2400.051336 + 0.000025862*t)*t;
1.899 +// return t0;
1.900 +// }
1.901 +
1.902 +// Commented out - currently unused. ICU 2.6, Alan
1.903 +// //-------------------------------------------------------------------------
1.904 +// // Alternate Sun Rise/Set
1.905 +// // See sci.astro FAQ
1.906 +// // http://www.faqs.org/faqs/astronomy/faq/part3/section-5.html
1.907 +// //-------------------------------------------------------------------------
1.908 +//
1.909 +// // Note: This method appears to produce inferior accuracy as
1.910 +// // compared to getSunRiseSet().
1.911 +//
1.912 +// /**
1.913 +// * TODO Make this when the entire class is package-private.
1.914 +// */
1.915 +// /*public*/ long getSunRiseSet3(boolean rise) {
1.916 +//
1.917 +// // Compute day number for 0.0 Jan 2000 epoch
1.918 +// double d = (double)(time - EPOCH_2000_MS) / DAY_MS;
1.919 +//
1.920 +// // Now compute the Local Sidereal Time, LST:
1.921 +// //
1.922 +// double LST = 98.9818 + 0.985647352 * d + /*UT*15 + long*/
1.923 +// fLongitude*RAD_DEG;
1.924 +// //
1.925 +// // (east long. positive). Note that LST is here expressed in degrees,
1.926 +// // where 15 degrees corresponds to one hour. Since LST really is an angle,
1.927 +// // it's convenient to use one unit---degrees---throughout.
1.928 +//
1.929 +// // COMPUTING THE SUN'S POSITION
1.930 +// // ----------------------------
1.931 +// //
1.932 +// // To be able to compute the Sun's rise/set times, you need to be able to
1.933 +// // compute the Sun's position at any time. First compute the "day
1.934 +// // number" d as outlined above, for the desired moment. Next compute:
1.935 +// //
1.936 +// double oblecl = 23.4393 - 3.563E-7 * d;
1.937 +// //
1.938 +// double w = 282.9404 + 4.70935E-5 * d;
1.939 +// double M = 356.0470 + 0.9856002585 * d;
1.940 +// double e = 0.016709 - 1.151E-9 * d;
1.941 +// //
1.942 +// // This is the obliquity of the ecliptic, plus some of the elements of
1.943 +// // the Sun's apparent orbit (i.e., really the Earth's orbit): w =
1.944 +// // argument of perihelion, M = mean anomaly, e = eccentricity.
1.945 +// // Semi-major axis is here assumed to be exactly 1.0 (while not strictly
1.946 +// // true, this is still an accurate approximation). Next compute E, the
1.947 +// // eccentric anomaly:
1.948 +// //
1.949 +// double E = M + e*(180/PI) * ::sin(M*DEG_RAD) * ( 1.0 + e*cos(M*DEG_RAD) );
1.950 +// //
1.951 +// // where E and M are in degrees. This is it---no further iterations are
1.952 +// // needed because we know e has a sufficiently small value. Next compute
1.953 +// // the true anomaly, v, and the distance, r:
1.954 +// //
1.955 +// /* r * cos(v) = */ double A = cos(E*DEG_RAD) - e;
1.956 +// /* r * ::sin(v) = */ double B = ::sqrt(1 - e*e) * ::sin(E*DEG_RAD);
1.957 +// //
1.958 +// // and
1.959 +// //
1.960 +// // r = sqrt( A*A + B*B )
1.961 +// double v = ::atan2( B, A )*RAD_DEG;
1.962 +// //
1.963 +// // The Sun's true longitude, slon, can now be computed:
1.964 +// //
1.965 +// double slon = v + w;
1.966 +// //
1.967 +// // Since the Sun is always at the ecliptic (or at least very very close to
1.968 +// // it), we can use simplified formulae to convert slon (the Sun's ecliptic
1.969 +// // longitude) to sRA and sDec (the Sun's RA and Dec):
1.970 +// //
1.971 +// // ::sin(slon) * cos(oblecl)
1.972 +// // tan(sRA) = -------------------------
1.973 +// // cos(slon)
1.974 +// //
1.975 +// // ::sin(sDec) = ::sin(oblecl) * ::sin(slon)
1.976 +// //
1.977 +// // As was the case when computing az, the Azimuth, if possible use an
1.978 +// // atan2() function to compute sRA.
1.979 +//
1.980 +// double sRA = ::atan2(sin(slon*DEG_RAD) * cos(oblecl*DEG_RAD), cos(slon*DEG_RAD))*RAD_DEG;
1.981 +//
1.982 +// double sin_sDec = ::sin(oblecl*DEG_RAD) * ::sin(slon*DEG_RAD);
1.983 +// double sDec = ::asin(sin_sDec)*RAD_DEG;
1.984 +//
1.985 +// // COMPUTING RISE AND SET TIMES
1.986 +// // ----------------------------
1.987 +// //
1.988 +// // To compute when an object rises or sets, you must compute when it
1.989 +// // passes the meridian and the HA of rise/set. Then the rise time is
1.990 +// // the meridian time minus HA for rise/set, and the set time is the
1.991 +// // meridian time plus the HA for rise/set.
1.992 +// //
1.993 +// // To find the meridian time, compute the Local Sidereal Time at 0h local
1.994 +// // time (or 0h UT if you prefer to work in UT) as outlined above---name
1.995 +// // that quantity LST0. The Meridian Time, MT, will now be:
1.996 +// //
1.997 +// // MT = RA - LST0
1.998 +// double MT = normalize(sRA - LST, 360);
1.999 +// //
1.1000 +// // where "RA" is the object's Right Ascension (in degrees!). If negative,
1.1001 +// // add 360 deg to MT. If the object is the Sun, leave the time as it is,
1.1002 +// // but if it's stellar, multiply MT by 365.2422/366.2422, to convert from
1.1003 +// // sidereal to solar time. Now, compute HA for rise/set, name that
1.1004 +// // quantity HA0:
1.1005 +// //
1.1006 +// // ::sin(h0) - ::sin(lat) * ::sin(Dec)
1.1007 +// // cos(HA0) = ---------------------------------
1.1008 +// // cos(lat) * cos(Dec)
1.1009 +// //
1.1010 +// // where h0 is the altitude selected to represent rise/set. For a purely
1.1011 +// // mathematical horizon, set h0 = 0 and simplify to:
1.1012 +// //
1.1013 +// // cos(HA0) = - tan(lat) * tan(Dec)
1.1014 +// //
1.1015 +// // If you want to account for refraction on the atmosphere, set h0 = -35/60
1.1016 +// // degrees (-35 arc minutes), and if you want to compute the rise/set times
1.1017 +// // for the Sun's upper limb, set h0 = -50/60 (-50 arc minutes).
1.1018 +// //
1.1019 +// double h0 = -50/60 * DEG_RAD;
1.1020 +//
1.1021 +// double HA0 = ::acos(
1.1022 +// (sin(h0) - ::sin(fLatitude) * sin_sDec) /
1.1023 +// (cos(fLatitude) * cos(sDec*DEG_RAD)))*RAD_DEG;
1.1024 +//
1.1025 +// // When HA0 has been computed, leave it as it is for the Sun but multiply
1.1026 +// // by 365.2422/366.2422 for stellar objects, to convert from sidereal to
1.1027 +// // solar time. Finally compute:
1.1028 +// //
1.1029 +// // Rise time = MT - HA0
1.1030 +// // Set time = MT + HA0
1.1031 +// //
1.1032 +// // convert the times from degrees to hours by dividing by 15.
1.1033 +// //
1.1034 +// // If you'd like to check that your calculations are accurate or just
1.1035 +// // need a quick result, check the USNO's Sun or Moon Rise/Set Table,
1.1036 +// // <URL:http://aa.usno.navy.mil/AA/data/docs/RS_OneYear.html>.
1.1037 +//
1.1038 +// double result = MT + (rise ? -HA0 : HA0); // in degrees
1.1039 +//
1.1040 +// // Find UT midnight on this day
1.1041 +// long midnight = DAY_MS * (time / DAY_MS);
1.1042 +//
1.1043 +// return midnight + (long) (result * 3600000 / 15);
1.1044 +// }
1.1045 +
1.1046 +//-------------------------------------------------------------------------
1.1047 +// The Moon
1.1048 +//-------------------------------------------------------------------------
1.1049 +
1.1050 +#define moonL0 (318.351648 * CalendarAstronomer::PI/180 ) // Mean long. at epoch
1.1051 +#define moonP0 ( 36.340410 * CalendarAstronomer::PI/180 ) // Mean long. of perigee
1.1052 +#define moonN0 ( 318.510107 * CalendarAstronomer::PI/180 ) // Mean long. of node
1.1053 +#define moonI ( 5.145366 * CalendarAstronomer::PI/180 ) // Inclination of orbit
1.1054 +#define moonE ( 0.054900 ) // Eccentricity of orbit
1.1055 +
1.1056 +// These aren't used right now
1.1057 +#define moonA ( 3.84401e5 ) // semi-major axis (km)
1.1058 +#define moonT0 ( 0.5181 * CalendarAstronomer::PI/180 ) // Angular size at distance A
1.1059 +#define moonPi ( 0.9507 * CalendarAstronomer::PI/180 ) // Parallax at distance A
1.1060 +
1.1061 +/**
1.1062 + * The position of the moon at the time set on this
1.1063 + * object, in equatorial coordinates.
1.1064 + * @internal
1.1065 + * @deprecated ICU 2.4. This class may be removed or modified.
1.1066 + */
1.1067 +const CalendarAstronomer::Equatorial& CalendarAstronomer::getMoonPosition()
1.1068 +{
1.1069 + //
1.1070 + // See page 142 of "Practial Astronomy with your Calculator",
1.1071 + // by Peter Duffet-Smith, for details on the algorithm.
1.1072 + //
1.1073 + if (moonPositionSet == FALSE) {
1.1074 + // Calculate the solar longitude. Has the side effect of
1.1075 + // filling in "meanAnomalySun" as well.
1.1076 + getSunLongitude();
1.1077 +
1.1078 + //
1.1079 + // Find the # of days since the epoch of our orbital parameters.
1.1080 + // TODO: Convert the time of day portion into ephemeris time
1.1081 + //
1.1082 + double day = getJulianDay() - JD_EPOCH; // Days since epoch
1.1083 +
1.1084 + // Calculate the mean longitude and anomaly of the moon, based on
1.1085 + // a circular orbit. Similar to the corresponding solar calculation.
1.1086 + double meanLongitude = norm2PI(13.1763966*PI/180*day + moonL0);
1.1087 + meanAnomalyMoon = norm2PI(meanLongitude - 0.1114041*PI/180 * day - moonP0);
1.1088 +
1.1089 + //
1.1090 + // Calculate the following corrections:
1.1091 + // Evection: the sun's gravity affects the moon's eccentricity
1.1092 + // Annual Eqn: variation in the effect due to earth-sun distance
1.1093 + // A3: correction factor (for ???)
1.1094 + //
1.1095 + double evection = 1.2739*PI/180 * ::sin(2 * (meanLongitude - sunLongitude)
1.1096 + - meanAnomalyMoon);
1.1097 + double annual = 0.1858*PI/180 * ::sin(meanAnomalySun);
1.1098 + double a3 = 0.3700*PI/180 * ::sin(meanAnomalySun);
1.1099 +
1.1100 + meanAnomalyMoon += evection - annual - a3;
1.1101 +
1.1102 + //
1.1103 + // More correction factors:
1.1104 + // center equation of the center correction
1.1105 + // a4 yet another error correction (???)
1.1106 + //
1.1107 + // TODO: Skip the equation of the center correction and solve Kepler's eqn?
1.1108 + //
1.1109 + double center = 6.2886*PI/180 * ::sin(meanAnomalyMoon);
1.1110 + double a4 = 0.2140*PI/180 * ::sin(2 * meanAnomalyMoon);
1.1111 +
1.1112 + // Now find the moon's corrected longitude
1.1113 + moonLongitude = meanLongitude + evection + center - annual + a4;
1.1114 +
1.1115 + //
1.1116 + // And finally, find the variation, caused by the fact that the sun's
1.1117 + // gravitational pull on the moon varies depending on which side of
1.1118 + // the earth the moon is on
1.1119 + //
1.1120 + double variation = 0.6583*CalendarAstronomer::PI/180 * ::sin(2*(moonLongitude - sunLongitude));
1.1121 +
1.1122 + moonLongitude += variation;
1.1123 +
1.1124 + //
1.1125 + // What we've calculated so far is the moon's longitude in the plane
1.1126 + // of its own orbit. Now map to the ecliptic to get the latitude
1.1127 + // and longitude. First we need to find the longitude of the ascending
1.1128 + // node, the position on the ecliptic where it is crossed by the moon's
1.1129 + // orbit as it crosses from the southern to the northern hemisphere.
1.1130 + //
1.1131 + double nodeLongitude = norm2PI(moonN0 - 0.0529539*PI/180 * day);
1.1132 +
1.1133 + nodeLongitude -= 0.16*PI/180 * ::sin(meanAnomalySun);
1.1134 +
1.1135 + double y = ::sin(moonLongitude - nodeLongitude);
1.1136 + double x = cos(moonLongitude - nodeLongitude);
1.1137 +
1.1138 + moonEclipLong = ::atan2(y*cos(moonI), x) + nodeLongitude;
1.1139 + double moonEclipLat = ::asin(y * ::sin(moonI));
1.1140 +
1.1141 + eclipticToEquatorial(moonPosition, moonEclipLong, moonEclipLat);
1.1142 + moonPositionSet = TRUE;
1.1143 + }
1.1144 + return moonPosition;
1.1145 +}
1.1146 +
1.1147 +/**
1.1148 + * The "age" of the moon at the time specified in this object.
1.1149 + * This is really the angle between the
1.1150 + * current ecliptic longitudes of the sun and the moon,
1.1151 + * measured in radians.
1.1152 + *
1.1153 + * @see #getMoonPhase
1.1154 + * @internal
1.1155 + * @deprecated ICU 2.4. This class may be removed or modified.
1.1156 + */
1.1157 +double CalendarAstronomer::getMoonAge() {
1.1158 + // See page 147 of "Practial Astronomy with your Calculator",
1.1159 + // by Peter Duffet-Smith, for details on the algorithm.
1.1160 + //
1.1161 + // Force the moon's position to be calculated. We're going to use
1.1162 + // some the intermediate results cached during that calculation.
1.1163 + //
1.1164 + getMoonPosition();
1.1165 +
1.1166 + return norm2PI(moonEclipLong - sunLongitude);
1.1167 +}
1.1168 +
1.1169 +/**
1.1170 + * Calculate the phase of the moon at the time set in this object.
1.1171 + * The returned phase is a <code>double</code> in the range
1.1172 + * <code>0 <= phase < 1</code>, interpreted as follows:
1.1173 + * <ul>
1.1174 + * <li>0.00: New moon
1.1175 + * <li>0.25: First quarter
1.1176 + * <li>0.50: Full moon
1.1177 + * <li>0.75: Last quarter
1.1178 + * </ul>
1.1179 + *
1.1180 + * @see #getMoonAge
1.1181 + * @internal
1.1182 + * @deprecated ICU 2.4. This class may be removed or modified.
1.1183 + */
1.1184 +double CalendarAstronomer::getMoonPhase() {
1.1185 + // See page 147 of "Practial Astronomy with your Calculator",
1.1186 + // by Peter Duffet-Smith, for details on the algorithm.
1.1187 + return 0.5 * (1 - cos(getMoonAge()));
1.1188 +}
1.1189 +
1.1190 +/**
1.1191 + * Constant representing a new moon.
1.1192 + * For use with {@link #getMoonTime getMoonTime}
1.1193 + * @internal
1.1194 + * @deprecated ICU 2.4. This class may be removed or modified.
1.1195 + */
1.1196 +const CalendarAstronomer::MoonAge CalendarAstronomer::NEW_MOON() {
1.1197 + return CalendarAstronomer::MoonAge(0);
1.1198 +}
1.1199 +
1.1200 +/**
1.1201 + * Constant representing the moon's first quarter.
1.1202 + * For use with {@link #getMoonTime getMoonTime}
1.1203 + * @internal
1.1204 + * @deprecated ICU 2.4. This class may be removed or modified.
1.1205 + */
1.1206 +/*const CalendarAstronomer::MoonAge CalendarAstronomer::FIRST_QUARTER() {
1.1207 + return CalendarAstronomer::MoonAge(CalendarAstronomer::PI/2);
1.1208 +}*/
1.1209 +
1.1210 +/**
1.1211 + * Constant representing a full moon.
1.1212 + * For use with {@link #getMoonTime getMoonTime}
1.1213 + * @internal
1.1214 + * @deprecated ICU 2.4. This class may be removed or modified.
1.1215 + */
1.1216 +const CalendarAstronomer::MoonAge CalendarAstronomer::FULL_MOON() {
1.1217 + return CalendarAstronomer::MoonAge(CalendarAstronomer::PI);
1.1218 +}
1.1219 +/**
1.1220 + * Constant representing the moon's last quarter.
1.1221 + * For use with {@link #getMoonTime getMoonTime}
1.1222 + * @internal
1.1223 + * @deprecated ICU 2.4. This class may be removed or modified.
1.1224 + */
1.1225 +
1.1226 +class MoonTimeAngleFunc : public CalendarAstronomer::AngleFunc {
1.1227 +public:
1.1228 + virtual ~MoonTimeAngleFunc();
1.1229 + virtual double eval(CalendarAstronomer&a) { return a.getMoonAge(); }
1.1230 +};
1.1231 +
1.1232 +MoonTimeAngleFunc::~MoonTimeAngleFunc() {}
1.1233 +
1.1234 +/*const CalendarAstronomer::MoonAge CalendarAstronomer::LAST_QUARTER() {
1.1235 + return CalendarAstronomer::MoonAge((CalendarAstronomer::PI*3)/2);
1.1236 +}*/
1.1237 +
1.1238 +/**
1.1239 + * Find the next or previous time at which the Moon's ecliptic
1.1240 + * longitude will have the desired value.
1.1241 + * <p>
1.1242 + * @param desired The desired longitude.
1.1243 + * @param next <tt>true</tt> if the next occurrance of the phase
1.1244 + * is desired, <tt>false</tt> for the previous occurrance.
1.1245 + * @internal
1.1246 + * @deprecated ICU 2.4. This class may be removed or modified.
1.1247 + */
1.1248 +UDate CalendarAstronomer::getMoonTime(double desired, UBool next)
1.1249 +{
1.1250 + MoonTimeAngleFunc func;
1.1251 + return timeOfAngle( func,
1.1252 + desired,
1.1253 + SYNODIC_MONTH,
1.1254 + MINUTE_MS,
1.1255 + next);
1.1256 +}
1.1257 +
1.1258 +/**
1.1259 + * Find the next or previous time at which the moon will be in the
1.1260 + * desired phase.
1.1261 + * <p>
1.1262 + * @param desired The desired phase of the moon.
1.1263 + * @param next <tt>true</tt> if the next occurrance of the phase
1.1264 + * is desired, <tt>false</tt> for the previous occurrance.
1.1265 + * @internal
1.1266 + * @deprecated ICU 2.4. This class may be removed or modified.
1.1267 + */
1.1268 +UDate CalendarAstronomer::getMoonTime(const CalendarAstronomer::MoonAge& desired, UBool next) {
1.1269 + return getMoonTime(desired.value, next);
1.1270 +}
1.1271 +
1.1272 +class MoonRiseSetCoordFunc : public CalendarAstronomer::CoordFunc {
1.1273 +public:
1.1274 + virtual ~MoonRiseSetCoordFunc();
1.1275 + virtual void eval(CalendarAstronomer::Equatorial& result, CalendarAstronomer&a) { result = a.getMoonPosition(); }
1.1276 +};
1.1277 +
1.1278 +MoonRiseSetCoordFunc::~MoonRiseSetCoordFunc() {}
1.1279 +
1.1280 +/**
1.1281 + * Returns the time (GMT) of sunrise or sunset on the local date to which
1.1282 + * this calendar is currently set.
1.1283 + * @internal
1.1284 + * @deprecated ICU 2.4. This class may be removed or modified.
1.1285 + */
1.1286 +UDate CalendarAstronomer::getMoonRiseSet(UBool rise)
1.1287 +{
1.1288 + MoonRiseSetCoordFunc func;
1.1289 + return riseOrSet(func,
1.1290 + rise,
1.1291 + .533 * DEG_RAD, // Angular Diameter
1.1292 + 34 /60.0 * DEG_RAD, // Refraction correction
1.1293 + MINUTE_MS); // Desired accuracy
1.1294 +}
1.1295 +
1.1296 +//-------------------------------------------------------------------------
1.1297 +// Interpolation methods for finding the time at which a given event occurs
1.1298 +//-------------------------------------------------------------------------
1.1299 +
1.1300 +UDate CalendarAstronomer::timeOfAngle(AngleFunc& func, double desired,
1.1301 + double periodDays, double epsilon, UBool next)
1.1302 +{
1.1303 + // Find the value of the function at the current time
1.1304 + double lastAngle = func.eval(*this);
1.1305 +
1.1306 + // Find out how far we are from the desired angle
1.1307 + double deltaAngle = norm2PI(desired - lastAngle) ;
1.1308 +
1.1309 + // Using the average period, estimate the next (or previous) time at
1.1310 + // which the desired angle occurs.
1.1311 + double deltaT = (deltaAngle + (next ? 0.0 : - CalendarAstronomer_PI2 )) * (periodDays*DAY_MS) / CalendarAstronomer_PI2;
1.1312 +
1.1313 + double lastDeltaT = deltaT; // Liu
1.1314 + UDate startTime = fTime; // Liu
1.1315 +
1.1316 + setTime(fTime + uprv_ceil(deltaT));
1.1317 +
1.1318 + // Now iterate until we get the error below epsilon. Throughout
1.1319 + // this loop we use normPI to get values in the range -Pi to Pi,
1.1320 + // since we're using them as correction factors rather than absolute angles.
1.1321 + do {
1.1322 + // Evaluate the function at the time we've estimated
1.1323 + double angle = func.eval(*this);
1.1324 +
1.1325 + // Find the # of milliseconds per radian at this point on the curve
1.1326 + double factor = uprv_fabs(deltaT / normPI(angle-lastAngle));
1.1327 +
1.1328 + // Correct the time estimate based on how far off the angle is
1.1329 + deltaT = normPI(desired - angle) * factor;
1.1330 +
1.1331 + // HACK:
1.1332 + //
1.1333 + // If abs(deltaT) begins to diverge we need to quit this loop.
1.1334 + // This only appears to happen when attempting to locate, for
1.1335 + // example, a new moon on the day of the new moon. E.g.:
1.1336 + //
1.1337 + // This result is correct:
1.1338 + // newMoon(7508(Mon Jul 23 00:00:00 CST 1990,false))=
1.1339 + // Sun Jul 22 10:57:41 CST 1990
1.1340 + //
1.1341 + // But attempting to make the same call a day earlier causes deltaT
1.1342 + // to diverge:
1.1343 + // CalendarAstronomer.timeOfAngle() diverging: 1.348508727575625E9 ->
1.1344 + // 1.3649828540224032E9
1.1345 + // newMoon(7507(Sun Jul 22 00:00:00 CST 1990,false))=
1.1346 + // Sun Jul 08 13:56:15 CST 1990
1.1347 + //
1.1348 + // As a temporary solution, we catch this specific condition and
1.1349 + // adjust our start time by one eighth period days (either forward
1.1350 + // or backward) and try again.
1.1351 + // Liu 11/9/00
1.1352 + if (uprv_fabs(deltaT) > uprv_fabs(lastDeltaT)) {
1.1353 + double delta = uprv_ceil (periodDays * DAY_MS / 8.0);
1.1354 + setTime(startTime + (next ? delta : -delta));
1.1355 + return timeOfAngle(func, desired, periodDays, epsilon, next);
1.1356 + }
1.1357 +
1.1358 + lastDeltaT = deltaT;
1.1359 + lastAngle = angle;
1.1360 +
1.1361 + setTime(fTime + uprv_ceil(deltaT));
1.1362 + }
1.1363 + while (uprv_fabs(deltaT) > epsilon);
1.1364 +
1.1365 + return fTime;
1.1366 +}
1.1367 +
1.1368 +UDate CalendarAstronomer::riseOrSet(CoordFunc& func, UBool rise,
1.1369 + double diameter, double refraction,
1.1370 + double epsilon)
1.1371 +{
1.1372 + Equatorial pos;
1.1373 + double tanL = ::tan(fLatitude);
1.1374 + double deltaT = 0;
1.1375 + int32_t count = 0;
1.1376 +
1.1377 + //
1.1378 + // Calculate the object's position at the current time, then use that
1.1379 + // position to calculate the time of rising or setting. The position
1.1380 + // will be different at that time, so iterate until the error is allowable.
1.1381 + //
1.1382 + U_DEBUG_ASTRO_MSG(("setup rise=%s, dia=%.3lf, ref=%.3lf, eps=%.3lf\n",
1.1383 + rise?"T":"F", diameter, refraction, epsilon));
1.1384 + do {
1.1385 + // See "Practical Astronomy With Your Calculator, section 33.
1.1386 + func.eval(pos, *this);
1.1387 + double angle = ::acos(-tanL * ::tan(pos.declination));
1.1388 + double lst = ((rise ? CalendarAstronomer_PI2-angle : angle) + pos.ascension ) * 24 / CalendarAstronomer_PI2;
1.1389 +
1.1390 + // Convert from LST to Universal Time.
1.1391 + UDate newTime = lstToUT( lst );
1.1392 +
1.1393 + deltaT = newTime - fTime;
1.1394 + setTime(newTime);
1.1395 + U_DEBUG_ASTRO_MSG(("%d] dT=%.3lf, angle=%.3lf, lst=%.3lf, A=%.3lf/D=%.3lf\n",
1.1396 + count, deltaT, angle, lst, pos.ascension, pos.declination));
1.1397 + }
1.1398 + while (++ count < 5 && uprv_fabs(deltaT) > epsilon);
1.1399 +
1.1400 + // Calculate the correction due to refraction and the object's angular diameter
1.1401 + double cosD = ::cos(pos.declination);
1.1402 + double psi = ::acos(sin(fLatitude) / cosD);
1.1403 + double x = diameter / 2 + refraction;
1.1404 + double y = ::asin(sin(x) / ::sin(psi));
1.1405 + long delta = (long)((240 * y * RAD_DEG / cosD)*SECOND_MS);
1.1406 +
1.1407 + return fTime + (rise ? -delta : delta);
1.1408 +}
1.1409 + /**
1.1410 + * Return the obliquity of the ecliptic (the angle between the ecliptic
1.1411 + * and the earth's equator) at the current time. This varies due to
1.1412 + * the precession of the earth's axis.
1.1413 + *
1.1414 + * @return the obliquity of the ecliptic relative to the equator,
1.1415 + * measured in radians.
1.1416 + */
1.1417 +double CalendarAstronomer::eclipticObliquity() {
1.1418 + if (isINVALID(eclipObliquity)) {
1.1419 + const double epoch = 2451545.0; // 2000 AD, January 1.5
1.1420 +
1.1421 + double T = (getJulianDay() - epoch) / 36525;
1.1422 +
1.1423 + eclipObliquity = 23.439292
1.1424 + - 46.815/3600 * T
1.1425 + - 0.0006/3600 * T*T
1.1426 + + 0.00181/3600 * T*T*T;
1.1427 +
1.1428 + eclipObliquity *= DEG_RAD;
1.1429 + }
1.1430 + return eclipObliquity;
1.1431 +}
1.1432 +
1.1433 +
1.1434 +//-------------------------------------------------------------------------
1.1435 +// Private data
1.1436 +//-------------------------------------------------------------------------
1.1437 +void CalendarAstronomer::clearCache() {
1.1438 + const double INVALID = uprv_getNaN();
1.1439 +
1.1440 + julianDay = INVALID;
1.1441 + julianCentury = INVALID;
1.1442 + sunLongitude = INVALID;
1.1443 + meanAnomalySun = INVALID;
1.1444 + moonLongitude = INVALID;
1.1445 + moonEclipLong = INVALID;
1.1446 + meanAnomalyMoon = INVALID;
1.1447 + eclipObliquity = INVALID;
1.1448 + siderealTime = INVALID;
1.1449 + siderealT0 = INVALID;
1.1450 + moonPositionSet = FALSE;
1.1451 +}
1.1452 +
1.1453 +//private static void out(String s) {
1.1454 +// System.out.println(s);
1.1455 +//}
1.1456 +
1.1457 +//private static String deg(double rad) {
1.1458 +// return Double.toString(rad * RAD_DEG);
1.1459 +//}
1.1460 +
1.1461 +//private static String hours(long ms) {
1.1462 +// return Double.toString((double)ms / HOUR_MS) + " hours";
1.1463 +//}
1.1464 +
1.1465 +/**
1.1466 + * @internal
1.1467 + * @deprecated ICU 2.4. This class may be removed or modified.
1.1468 + */
1.1469 +/*UDate CalendarAstronomer::local(UDate localMillis) {
1.1470 + // TODO - srl ?
1.1471 + TimeZone *tz = TimeZone::createDefault();
1.1472 + int32_t rawOffset;
1.1473 + int32_t dstOffset;
1.1474 + UErrorCode status = U_ZERO_ERROR;
1.1475 + tz->getOffset(localMillis, TRUE, rawOffset, dstOffset, status);
1.1476 + delete tz;
1.1477 + return localMillis - rawOffset;
1.1478 +}*/
1.1479 +
1.1480 +// Debugging functions
1.1481 +UnicodeString CalendarAstronomer::Ecliptic::toString() const
1.1482 +{
1.1483 +#ifdef U_DEBUG_ASTRO
1.1484 + char tmp[800];
1.1485 + sprintf(tmp, "[%.5f,%.5f]", longitude*RAD_DEG, latitude*RAD_DEG);
1.1486 + return UnicodeString(tmp, "");
1.1487 +#else
1.1488 + return UnicodeString();
1.1489 +#endif
1.1490 +}
1.1491 +
1.1492 +UnicodeString CalendarAstronomer::Equatorial::toString() const
1.1493 +{
1.1494 +#ifdef U_DEBUG_ASTRO
1.1495 + char tmp[400];
1.1496 + sprintf(tmp, "%f,%f",
1.1497 + (ascension*RAD_DEG), (declination*RAD_DEG));
1.1498 + return UnicodeString(tmp, "");
1.1499 +#else
1.1500 + return UnicodeString();
1.1501 +#endif
1.1502 +}
1.1503 +
1.1504 +UnicodeString CalendarAstronomer::Horizon::toString() const
1.1505 +{
1.1506 +#ifdef U_DEBUG_ASTRO
1.1507 + char tmp[800];
1.1508 + sprintf(tmp, "[%.5f,%.5f]", altitude*RAD_DEG, azimuth*RAD_DEG);
1.1509 + return UnicodeString(tmp, "");
1.1510 +#else
1.1511 + return UnicodeString();
1.1512 +#endif
1.1513 +}
1.1514 +
1.1515 +
1.1516 +// static private String radToHms(double angle) {
1.1517 +// int hrs = (int) (angle*RAD_HOUR);
1.1518 +// int min = (int)((angle*RAD_HOUR - hrs) * 60);
1.1519 +// int sec = (int)((angle*RAD_HOUR - hrs - min/60.0) * 3600);
1.1520 +
1.1521 +// return Integer.toString(hrs) + "h" + min + "m" + sec + "s";
1.1522 +// }
1.1523 +
1.1524 +// static private String radToDms(double angle) {
1.1525 +// int deg = (int) (angle*RAD_DEG);
1.1526 +// int min = (int)((angle*RAD_DEG - deg) * 60);
1.1527 +// int sec = (int)((angle*RAD_DEG - deg - min/60.0) * 3600);
1.1528 +
1.1529 +// return Integer.toString(deg) + "\u00b0" + min + "'" + sec + "\"";
1.1530 +// }
1.1531 +
1.1532 +// =============== Calendar Cache ================
1.1533 +
1.1534 +void CalendarCache::createCache(CalendarCache** cache, UErrorCode& status) {
1.1535 + ucln_i18n_registerCleanup(UCLN_I18N_ASTRO_CALENDAR, calendar_astro_cleanup);
1.1536 + if(cache == NULL) {
1.1537 + status = U_MEMORY_ALLOCATION_ERROR;
1.1538 + } else {
1.1539 + *cache = new CalendarCache(32, status);
1.1540 + if(U_FAILURE(status)) {
1.1541 + delete *cache;
1.1542 + *cache = NULL;
1.1543 + }
1.1544 + }
1.1545 +}
1.1546 +
1.1547 +int32_t CalendarCache::get(CalendarCache** cache, int32_t key, UErrorCode &status) {
1.1548 + int32_t res;
1.1549 +
1.1550 + if(U_FAILURE(status)) {
1.1551 + return 0;
1.1552 + }
1.1553 + umtx_lock(&ccLock);
1.1554 +
1.1555 + if(*cache == NULL) {
1.1556 + createCache(cache, status);
1.1557 + if(U_FAILURE(status)) {
1.1558 + umtx_unlock(&ccLock);
1.1559 + return 0;
1.1560 + }
1.1561 + }
1.1562 +
1.1563 + res = uhash_igeti((*cache)->fTable, key);
1.1564 + U_DEBUG_ASTRO_MSG(("%p: GET: [%d] == %d\n", (*cache)->fTable, key, res));
1.1565 +
1.1566 + umtx_unlock(&ccLock);
1.1567 + return res;
1.1568 +}
1.1569 +
1.1570 +void CalendarCache::put(CalendarCache** cache, int32_t key, int32_t value, UErrorCode &status) {
1.1571 + if(U_FAILURE(status)) {
1.1572 + return;
1.1573 + }
1.1574 + umtx_lock(&ccLock);
1.1575 +
1.1576 + if(*cache == NULL) {
1.1577 + createCache(cache, status);
1.1578 + if(U_FAILURE(status)) {
1.1579 + umtx_unlock(&ccLock);
1.1580 + return;
1.1581 + }
1.1582 + }
1.1583 +
1.1584 + uhash_iputi((*cache)->fTable, key, value, &status);
1.1585 + U_DEBUG_ASTRO_MSG(("%p: PUT: [%d] := %d\n", (*cache)->fTable, key, value));
1.1586 +
1.1587 + umtx_unlock(&ccLock);
1.1588 +}
1.1589 +
1.1590 +CalendarCache::CalendarCache(int32_t size, UErrorCode &status) {
1.1591 + fTable = uhash_openSize(uhash_hashLong, uhash_compareLong, NULL, size, &status);
1.1592 + U_DEBUG_ASTRO_MSG(("%p: Opening.\n", fTable));
1.1593 +}
1.1594 +
1.1595 +CalendarCache::~CalendarCache() {
1.1596 + if(fTable != NULL) {
1.1597 + U_DEBUG_ASTRO_MSG(("%p: Closing.\n", fTable));
1.1598 + uhash_close(fTable);
1.1599 + }
1.1600 +}
1.1601 +
1.1602 +U_NAMESPACE_END
1.1603 +
1.1604 +#endif // !UCONFIG_NO_FORMATTING
