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Diffstat (limited to 'deps/node/deps/icu-small/source/i18n/astro.cpp')
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diff --git a/deps/node/deps/icu-small/source/i18n/astro.cpp b/deps/node/deps/icu-small/source/i18n/astro.cpp deleted file mode 100644 index 0bf32ae8..00000000 --- a/deps/node/deps/icu-small/source/i18n/astro.cpp +++ /dev/null @@ -1,1603 +0,0 @@ -// © 2016 and later: Unicode, Inc. and others. -// License & terms of use: http://www.unicode.org/copyright.html -/************************************************************************ - * Copyright (C) 1996-2012, International Business Machines Corporation - * and others. All Rights Reserved. - ************************************************************************ - * 2003-nov-07 srl Port from Java - */ - -#include "astro.h" - -#if !UCONFIG_NO_FORMATTING - -#include "unicode/calendar.h" -#include <math.h> -#include <float.h> -#include "unicode/putil.h" -#include "uhash.h" -#include "umutex.h" -#include "ucln_in.h" -#include "putilimp.h" -#include <stdio.h> // for toString() - -#if defined (PI) -#undef PI -#endif - -#ifdef U_DEBUG_ASTRO -# include "uresimp.h" // for debugging - -static void debug_astro_loc(const char *f, int32_t l) -{ - fprintf(stderr, "%s:%d: ", f, l); -} - -static void debug_astro_msg(const char *pat, ...) -{ - va_list ap; - va_start(ap, pat); - vfprintf(stderr, pat, ap); - fflush(stderr); -} -#include "unicode/datefmt.h" -#include "unicode/ustring.h" -static const char * debug_astro_date(UDate d) { - static char gStrBuf[1024]; - static DateFormat *df = NULL; - if(df == NULL) { - df = DateFormat::createDateTimeInstance(DateFormat::MEDIUM, DateFormat::MEDIUM, Locale::getUS()); - df->adoptTimeZone(TimeZone::getGMT()->clone()); - } - UnicodeString str; - df->format(d,str); - u_austrncpy(gStrBuf,str.getTerminatedBuffer(),sizeof(gStrBuf)-1); - return gStrBuf; -} - -// must use double parens, i.e.: U_DEBUG_ASTRO_MSG(("four is: %d",4)); -#define U_DEBUG_ASTRO_MSG(x) {debug_astro_loc(__FILE__,__LINE__);debug_astro_msg x;} -#else -#define U_DEBUG_ASTRO_MSG(x) -#endif - -static inline UBool isINVALID(double d) { - return(uprv_isNaN(d)); -} - -static UMutex ccLock = U_MUTEX_INITIALIZER; - -U_CDECL_BEGIN -static UBool calendar_astro_cleanup(void) { - return TRUE; -} -U_CDECL_END - -U_NAMESPACE_BEGIN - -/** - * The number of standard hours in one sidereal day. - * Approximately 24.93. - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -#define SIDEREAL_DAY (23.93446960027) - -/** - * The number of sidereal hours in one mean solar day. - * Approximately 24.07. - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -#define SOLAR_DAY (24.065709816) - -/** - * The average number of solar days from one new moon to the next. This is the time - * it takes for the moon to return the same ecliptic longitude as the sun. - * It is longer than the sidereal month because the sun's longitude increases - * during the year due to the revolution of the earth around the sun. - * Approximately 29.53. - * - * @see #SIDEREAL_MONTH - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -const double CalendarAstronomer::SYNODIC_MONTH = 29.530588853; - -/** - * The average number of days it takes - * for the moon to return to the same ecliptic longitude relative to the - * stellar background. This is referred to as the sidereal month. - * It is shorter than the synodic month due to - * the revolution of the earth around the sun. - * Approximately 27.32. - * - * @see #SYNODIC_MONTH - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -#define SIDEREAL_MONTH 27.32166 - -/** - * The average number number of days between successive vernal equinoxes. - * Due to the precession of the earth's - * axis, this is not precisely the same as the sidereal year. - * Approximately 365.24 - * - * @see #SIDEREAL_YEAR - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -#define TROPICAL_YEAR 365.242191 - -/** - * The average number of days it takes - * for the sun to return to the same position against the fixed stellar - * background. This is the duration of one orbit of the earth about the sun - * as it would appear to an outside observer. - * Due to the precession of the earth's - * axis, this is not precisely the same as the tropical year. - * Approximately 365.25. - * - * @see #TROPICAL_YEAR - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -#define SIDEREAL_YEAR 365.25636 - -//------------------------------------------------------------------------- -// Time-related constants -//------------------------------------------------------------------------- - -/** - * The number of milliseconds in one second. - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -#define SECOND_MS U_MILLIS_PER_SECOND - -/** - * The number of milliseconds in one minute. - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -#define MINUTE_MS U_MILLIS_PER_MINUTE - -/** - * The number of milliseconds in one hour. - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -#define HOUR_MS U_MILLIS_PER_HOUR - -/** - * The number of milliseconds in one day. - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -#define DAY_MS U_MILLIS_PER_DAY - -/** - * The start of the julian day numbering scheme used by astronomers, which - * is 1/1/4713 BC (Julian), 12:00 GMT. This is given as the number of milliseconds - * since 1/1/1970 AD (Gregorian), a negative number. - * Note that julian day numbers and - * the Julian calendar are <em>not</em> the same thing. Also note that - * julian days start at <em>noon</em>, not midnight. - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -#define JULIAN_EPOCH_MS -210866760000000.0 - - -/** - * Milliseconds value for 0.0 January 2000 AD. - */ -#define EPOCH_2000_MS 946598400000.0 - -//------------------------------------------------------------------------- -// Assorted private data used for conversions -//------------------------------------------------------------------------- - -// My own copies of these so compilers are more likely to optimize them away -const double CalendarAstronomer::PI = 3.14159265358979323846; - -#define CalendarAstronomer_PI2 (CalendarAstronomer::PI*2.0) -#define RAD_HOUR ( 12 / CalendarAstronomer::PI ) // radians -> hours -#define DEG_RAD ( CalendarAstronomer::PI / 180 ) // degrees -> radians -#define RAD_DEG ( 180 / CalendarAstronomer::PI ) // radians -> degrees - -/*** - * Given 'value', add or subtract 'range' until 0 <= 'value' < range. - * The modulus operator. - */ -inline static double normalize(double value, double range) { - return value - range * ClockMath::floorDivide(value, range); -} - -/** - * Normalize an angle so that it's in the range 0 - 2pi. - * For positive angles this is just (angle % 2pi), but the Java - * mod operator doesn't work that way for negative numbers.... - */ -inline static double norm2PI(double angle) { - return normalize(angle, CalendarAstronomer::PI * 2.0); -} - -/** - * Normalize an angle into the range -PI - PI - */ -inline static double normPI(double angle) { - return normalize(angle + CalendarAstronomer::PI, CalendarAstronomer::PI * 2.0) - CalendarAstronomer::PI; -} - -//------------------------------------------------------------------------- -// Constructors -//------------------------------------------------------------------------- - -/** - * Construct a new <code>CalendarAstronomer</code> object that is initialized to - * the current date and time. - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -CalendarAstronomer::CalendarAstronomer(): - fTime(Calendar::getNow()), fLongitude(0.0), fLatitude(0.0), fGmtOffset(0.0), moonPosition(0,0), moonPositionSet(FALSE) { - clearCache(); -} - -/** - * Construct a new <code>CalendarAstronomer</code> object that is initialized to - * the specified date and time. - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -CalendarAstronomer::CalendarAstronomer(UDate d): fTime(d), fLongitude(0.0), fLatitude(0.0), fGmtOffset(0.0), moonPosition(0,0), moonPositionSet(FALSE) { - clearCache(); -} - -/** - * Construct a new <code>CalendarAstronomer</code> object with the given - * latitude and longitude. The object's time is set to the current - * date and time. - * <p> - * @param longitude The desired longitude, in <em>degrees</em> east of - * the Greenwich meridian. - * - * @param latitude The desired latitude, in <em>degrees</em>. Positive - * values signify North, negative South. - * - * @see java.util.Date#getTime() - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -CalendarAstronomer::CalendarAstronomer(double longitude, double latitude) : - fTime(Calendar::getNow()), moonPosition(0,0), moonPositionSet(FALSE) { - fLongitude = normPI(longitude * (double)DEG_RAD); - fLatitude = normPI(latitude * (double)DEG_RAD); - fGmtOffset = (double)(fLongitude * 24. * (double)HOUR_MS / (double)CalendarAstronomer_PI2); - clearCache(); -} - -CalendarAstronomer::~CalendarAstronomer() -{ -} - -//------------------------------------------------------------------------- -// Time and date getters and setters -//------------------------------------------------------------------------- - -/** - * Set the current date and time of this <code>CalendarAstronomer</code> object. All - * astronomical calculations are performed based on this time setting. - * - * @param aTime the date and time, expressed as the number of milliseconds since - * 1/1/1970 0:00 GMT (Gregorian). - * - * @see #setDate - * @see #getTime - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -void CalendarAstronomer::setTime(UDate aTime) { - fTime = aTime; - U_DEBUG_ASTRO_MSG(("setTime(%.1lf, %sL)\n", aTime, debug_astro_date(aTime+fGmtOffset))); - clearCache(); -} - -/** - * Set the current date and time of this <code>CalendarAstronomer</code> object. All - * astronomical calculations are performed based on this time setting. - * - * @param jdn the desired time, expressed as a "julian day number", - * which is the number of elapsed days since - * 1/1/4713 BC (Julian), 12:00 GMT. Note that julian day - * numbers start at <em>noon</em>. To get the jdn for - * the corresponding midnight, subtract 0.5. - * - * @see #getJulianDay - * @see #JULIAN_EPOCH_MS - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -void CalendarAstronomer::setJulianDay(double jdn) { - fTime = (double)(jdn * DAY_MS) + JULIAN_EPOCH_MS; - clearCache(); - julianDay = jdn; -} - -/** - * Get the current time of this <code>CalendarAstronomer</code> object, - * represented as the number of milliseconds since - * 1/1/1970 AD 0:00 GMT (Gregorian). - * - * @see #setTime - * @see #getDate - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -UDate CalendarAstronomer::getTime() { - return fTime; -} - -/** - * Get the current time of this <code>CalendarAstronomer</code> object, - * expressed as a "julian day number", which is the number of elapsed - * days since 1/1/4713 BC (Julian), 12:00 GMT. - * - * @see #setJulianDay - * @see #JULIAN_EPOCH_MS - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -double CalendarAstronomer::getJulianDay() { - if (isINVALID(julianDay)) { - julianDay = (fTime - (double)JULIAN_EPOCH_MS) / (double)DAY_MS; - } - return julianDay; -} - -/** - * Return this object's time expressed in julian centuries: - * the number of centuries after 1/1/1900 AD, 12:00 GMT - * - * @see #getJulianDay - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -double CalendarAstronomer::getJulianCentury() { - if (isINVALID(julianCentury)) { - julianCentury = (getJulianDay() - 2415020.0) / 36525.0; - } - return julianCentury; -} - -/** - * Returns the current Greenwich sidereal time, measured in hours - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -double CalendarAstronomer::getGreenwichSidereal() { - if (isINVALID(siderealTime)) { - // See page 86 of "Practial Astronomy with your Calculator", - // by Peter Duffet-Smith, for details on the algorithm. - - double UT = normalize(fTime/(double)HOUR_MS, 24.); - - siderealTime = normalize(getSiderealOffset() + UT*1.002737909, 24.); - } - return siderealTime; -} - -double CalendarAstronomer::getSiderealOffset() { - if (isINVALID(siderealT0)) { - double JD = uprv_floor(getJulianDay() - 0.5) + 0.5; - double S = JD - 2451545.0; - double T = S / 36525.0; - siderealT0 = normalize(6.697374558 + 2400.051336*T + 0.000025862*T*T, 24); - } - return siderealT0; -} - -/** - * Returns the current local sidereal time, measured in hours - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -double CalendarAstronomer::getLocalSidereal() { - return normalize(getGreenwichSidereal() + (fGmtOffset/(double)HOUR_MS), 24.); -} - -/** - * Converts local sidereal time to Universal Time. - * - * @param lst The Local Sidereal Time, in hours since sidereal midnight - * on this object's current date. - * - * @return The corresponding Universal Time, in milliseconds since - * 1 Jan 1970, GMT. - */ -double CalendarAstronomer::lstToUT(double lst) { - // Convert to local mean time - double lt = normalize((lst - getSiderealOffset()) * 0.9972695663, 24); - - // Then find local midnight on this day - double base = (DAY_MS * ClockMath::floorDivide(fTime + fGmtOffset,(double)DAY_MS)) - fGmtOffset; - - //out(" lt =" + lt + " hours"); - //out(" base=" + new Date(base)); - - return base + (long)(lt * HOUR_MS); -} - - -//------------------------------------------------------------------------- -// Coordinate transformations, all based on the current time of this object -//------------------------------------------------------------------------- - -/** - * Convert from ecliptic to equatorial coordinates. - * - * @param ecliptic A point in the sky in ecliptic coordinates. - * @return The corresponding point in equatorial coordinates. - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -CalendarAstronomer::Equatorial& CalendarAstronomer::eclipticToEquatorial(CalendarAstronomer::Equatorial& result, const CalendarAstronomer::Ecliptic& ecliptic) -{ - return eclipticToEquatorial(result, ecliptic.longitude, ecliptic.latitude); -} - -/** - * Convert from ecliptic to equatorial coordinates. - * - * @param eclipLong The ecliptic longitude - * @param eclipLat The ecliptic latitude - * - * @return The corresponding point in equatorial coordinates. - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -CalendarAstronomer::Equatorial& CalendarAstronomer::eclipticToEquatorial(CalendarAstronomer::Equatorial& result, double eclipLong, double eclipLat) -{ - // See page 42 of "Practial Astronomy with your Calculator", - // by Peter Duffet-Smith, for details on the algorithm. - - double obliq = eclipticObliquity(); - double sinE = ::sin(obliq); - double cosE = cos(obliq); - - double sinL = ::sin(eclipLong); - double cosL = cos(eclipLong); - - double sinB = ::sin(eclipLat); - double cosB = cos(eclipLat); - double tanB = tan(eclipLat); - - result.set(atan2(sinL*cosE - tanB*sinE, cosL), - asin(sinB*cosE + cosB*sinE*sinL) ); - return result; -} - -/** - * Convert from ecliptic longitude to equatorial coordinates. - * - * @param eclipLong The ecliptic longitude - * - * @return The corresponding point in equatorial coordinates. - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -CalendarAstronomer::Equatorial& CalendarAstronomer::eclipticToEquatorial(CalendarAstronomer::Equatorial& result, double eclipLong) -{ - return eclipticToEquatorial(result, eclipLong, 0); // TODO: optimize -} - -/** - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -CalendarAstronomer::Horizon& CalendarAstronomer::eclipticToHorizon(CalendarAstronomer::Horizon& result, double eclipLong) -{ - Equatorial equatorial; - eclipticToEquatorial(equatorial, eclipLong); - - double H = getLocalSidereal()*CalendarAstronomer::PI/12 - equatorial.ascension; // Hour-angle - - double sinH = ::sin(H); - double cosH = cos(H); - double sinD = ::sin(equatorial.declination); - double cosD = cos(equatorial.declination); - double sinL = ::sin(fLatitude); - double cosL = cos(fLatitude); - - double altitude = asin(sinD*sinL + cosD*cosL*cosH); - double azimuth = atan2(-cosD*cosL*sinH, sinD - sinL * ::sin(altitude)); - - result.set(azimuth, altitude); - return result; -} - - -//------------------------------------------------------------------------- -// The Sun -//------------------------------------------------------------------------- - -// -// Parameters of the Sun's orbit as of the epoch Jan 0.0 1990 -// Angles are in radians (after multiplying by CalendarAstronomer::PI/180) -// -#define JD_EPOCH 2447891.5 // Julian day of epoch - -#define SUN_ETA_G (279.403303 * CalendarAstronomer::PI/180) // Ecliptic longitude at epoch -#define SUN_OMEGA_G (282.768422 * CalendarAstronomer::PI/180) // Ecliptic longitude of perigee -#define SUN_E 0.016713 // Eccentricity of orbit -//double sunR0 1.495585e8 // Semi-major axis in KM -//double sunTheta0 (0.533128 * CalendarAstronomer::PI/180) // Angular diameter at R0 - -// The following three methods, which compute the sun parameters -// given above for an arbitrary epoch (whatever time the object is -// set to), make only a small difference as compared to using the -// above constants. E.g., Sunset times might differ by ~12 -// seconds. Furthermore, the eta-g computation is befuddled by -// Duffet-Smith's incorrect coefficients (p.86). I've corrected -// the first-order coefficient but the others may be off too - no -// way of knowing without consulting another source. - -// /** -// * Return the sun's ecliptic longitude at perigee for the current time. -// * See Duffett-Smith, p. 86. -// * @return radians -// */ -// private double getSunOmegaG() { -// double T = getJulianCentury(); -// return (281.2208444 + (1.719175 + 0.000452778*T)*T) * DEG_RAD; -// } - -// /** -// * Return the sun's ecliptic longitude for the current time. -// * See Duffett-Smith, p. 86. -// * @return radians -// */ -// private double getSunEtaG() { -// double T = getJulianCentury(); -// //return (279.6966778 + (36000.76892 + 0.0003025*T)*T) * DEG_RAD; -// // -// // The above line is from Duffett-Smith, and yields manifestly wrong -// // results. The below constant is derived empirically to match the -// // constant he gives for the 1990 EPOCH. -// // -// return (279.6966778 + (-0.3262541582718024 + 0.0003025*T)*T) * DEG_RAD; -// } - -// /** -// * Return the sun's eccentricity of orbit for the current time. -// * See Duffett-Smith, p. 86. -// * @return double -// */ -// private double getSunE() { -// double T = getJulianCentury(); -// return 0.01675104 - (0.0000418 + 0.000000126*T)*T; -// } - -/** - * Find the "true anomaly" (longitude) of an object from - * its mean anomaly and the eccentricity of its orbit. This uses - * an iterative solution to Kepler's equation. - * - * @param meanAnomaly The object's longitude calculated as if it were in - * a regular, circular orbit, measured in radians - * from the point of perigee. - * - * @param eccentricity The eccentricity of the orbit - * - * @return The true anomaly (longitude) measured in radians - */ -static double trueAnomaly(double meanAnomaly, double eccentricity) -{ - // First, solve Kepler's equation iteratively - // Duffett-Smith, p.90 - double delta; - double E = meanAnomaly; - do { - delta = E - eccentricity * ::sin(E) - meanAnomaly; - E = E - delta / (1 - eccentricity * ::cos(E)); - } - while (uprv_fabs(delta) > 1e-5); // epsilon = 1e-5 rad - - return 2.0 * ::atan( ::tan(E/2) * ::sqrt( (1+eccentricity) - /(1-eccentricity) ) ); -} - -/** - * The longitude of the sun at the time specified by this object. - * The longitude is measured in radians along the ecliptic - * from the "first point of Aries," the point at which the ecliptic - * crosses the earth's equatorial plane at the vernal equinox. - * <p> - * Currently, this method uses an approximation of the two-body Kepler's - * equation for the earth and the sun. It does not take into account the - * perturbations caused by the other planets, the moon, etc. - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -double CalendarAstronomer::getSunLongitude() -{ - // See page 86 of "Practial Astronomy with your Calculator", - // by Peter Duffet-Smith, for details on the algorithm. - - if (isINVALID(sunLongitude)) { - getSunLongitude(getJulianDay(), sunLongitude, meanAnomalySun); - } - return sunLongitude; -} - -/** - * TODO Make this public when the entire class is package-private. - */ -/*public*/ void CalendarAstronomer::getSunLongitude(double jDay, double &longitude, double &meanAnomaly) -{ - // See page 86 of "Practial Astronomy with your Calculator", - // by Peter Duffet-Smith, for details on the algorithm. - - double day = jDay - JD_EPOCH; // Days since epoch - - // Find the angular distance the sun in a fictitious - // circular orbit has travelled since the epoch. - double epochAngle = norm2PI(CalendarAstronomer_PI2/TROPICAL_YEAR*day); - - // The epoch wasn't at the sun's perigee; find the angular distance - // since perigee, which is called the "mean anomaly" - meanAnomaly = norm2PI(epochAngle + SUN_ETA_G - SUN_OMEGA_G); - - // Now find the "true anomaly", e.g. the real solar longitude - // by solving Kepler's equation for an elliptical orbit - // NOTE: The 3rd ed. of the book lists omega_g and eta_g in different - // equations; omega_g is to be correct. - longitude = norm2PI(trueAnomaly(meanAnomaly, SUN_E) + SUN_OMEGA_G); -} - -/** - * The position of the sun at this object's current date and time, - * in equatorial coordinates. - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -CalendarAstronomer::Equatorial& CalendarAstronomer::getSunPosition(CalendarAstronomer::Equatorial& result) { - return eclipticToEquatorial(result, getSunLongitude(), 0); -} - - -/** - * Constant representing the vernal equinox. - * For use with {@link #getSunTime getSunTime}. - * Note: In this case, "vernal" refers to the northern hemisphere's seasons. - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -/*double CalendarAstronomer::VERNAL_EQUINOX() { - return 0; -}*/ - -/** - * Constant representing the summer solstice. - * For use with {@link #getSunTime getSunTime}. - * Note: In this case, "summer" refers to the northern hemisphere's seasons. - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -double CalendarAstronomer::SUMMER_SOLSTICE() { - return (CalendarAstronomer::PI/2); -} - -/** - * Constant representing the autumnal equinox. - * For use with {@link #getSunTime getSunTime}. - * Note: In this case, "autumn" refers to the northern hemisphere's seasons. - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -/*double CalendarAstronomer::AUTUMN_EQUINOX() { - return (CalendarAstronomer::PI); -}*/ - -/** - * Constant representing the winter solstice. - * For use with {@link #getSunTime getSunTime}. - * Note: In this case, "winter" refers to the northern hemisphere's seasons. - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -double CalendarAstronomer::WINTER_SOLSTICE() { - return ((CalendarAstronomer::PI*3)/2); -} - -CalendarAstronomer::AngleFunc::~AngleFunc() {} - -/** - * Find the next time at which the sun's ecliptic longitude will have - * the desired value. - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -class SunTimeAngleFunc : public CalendarAstronomer::AngleFunc { -public: - virtual ~SunTimeAngleFunc(); - virtual double eval(CalendarAstronomer& a) { return a.getSunLongitude(); } -}; - -SunTimeAngleFunc::~SunTimeAngleFunc() {} - -UDate CalendarAstronomer::getSunTime(double desired, UBool next) -{ - SunTimeAngleFunc func; - return timeOfAngle( func, - desired, - TROPICAL_YEAR, - MINUTE_MS, - next); -} - -CalendarAstronomer::CoordFunc::~CoordFunc() {} - -class RiseSetCoordFunc : public CalendarAstronomer::CoordFunc { -public: - virtual ~RiseSetCoordFunc(); - virtual void eval(CalendarAstronomer::Equatorial& result, CalendarAstronomer&a) { a.getSunPosition(result); } -}; - -RiseSetCoordFunc::~RiseSetCoordFunc() {} - -UDate CalendarAstronomer::getSunRiseSet(UBool rise) -{ - UDate t0 = fTime; - - // Make a rough guess: 6am or 6pm local time on the current day - double noon = ClockMath::floorDivide(fTime + fGmtOffset, (double)DAY_MS)*DAY_MS - fGmtOffset + (12*HOUR_MS); - - U_DEBUG_ASTRO_MSG(("Noon=%.2lf, %sL, gmtoff %.2lf\n", noon, debug_astro_date(noon+fGmtOffset), fGmtOffset)); - setTime(noon + ((rise ? -6 : 6) * HOUR_MS)); - U_DEBUG_ASTRO_MSG(("added %.2lf ms as a guess,\n", ((rise ? -6. : 6.) * HOUR_MS))); - - RiseSetCoordFunc func; - double t = riseOrSet(func, - rise, - .533 * DEG_RAD, // Angular Diameter - 34. /60.0 * DEG_RAD, // Refraction correction - MINUTE_MS / 12.); // Desired accuracy - - setTime(t0); - return t; -} - -// Commented out - currently unused. ICU 2.6, Alan -// //------------------------------------------------------------------------- -// // Alternate Sun Rise/Set -// // See Duffett-Smith p.93 -// //------------------------------------------------------------------------- -// -// // This yields worse results (as compared to USNO data) than getSunRiseSet(). -// /** -// * TODO Make this when the entire class is package-private. -// */ -// /*public*/ long getSunRiseSet2(boolean rise) { -// // 1. Calculate coordinates of the sun's center for midnight -// double jd = uprv_floor(getJulianDay() - 0.5) + 0.5; -// double[] sl = getSunLongitude(jd);// double lambda1 = sl[0]; -// Equatorial pos1 = eclipticToEquatorial(lambda1, 0); -// -// // 2. Add ... to lambda to get position 24 hours later -// double lambda2 = lambda1 + 0.985647*DEG_RAD; -// Equatorial pos2 = eclipticToEquatorial(lambda2, 0); -// -// // 3. Calculate LSTs of rising and setting for these two positions -// double tanL = ::tan(fLatitude); -// double H = ::acos(-tanL * ::tan(pos1.declination)); -// double lst1r = (CalendarAstronomer_PI2 + pos1.ascension - H) * 24 / CalendarAstronomer_PI2; -// double lst1s = (pos1.ascension + H) * 24 / CalendarAstronomer_PI2; -// H = ::acos(-tanL * ::tan(pos2.declination)); -// double lst2r = (CalendarAstronomer_PI2-H + pos2.ascension ) * 24 / CalendarAstronomer_PI2; -// double lst2s = (H + pos2.ascension ) * 24 / CalendarAstronomer_PI2; -// if (lst1r > 24) lst1r -= 24; -// if (lst1s > 24) lst1s -= 24; -// if (lst2r > 24) lst2r -= 24; -// if (lst2s > 24) lst2s -= 24; -// -// // 4. Convert LSTs to GSTs. If GST1 > GST2, add 24 to GST2. -// double gst1r = lstToGst(lst1r); -// double gst1s = lstToGst(lst1s); -// double gst2r = lstToGst(lst2r); -// double gst2s = lstToGst(lst2s); -// if (gst1r > gst2r) gst2r += 24; -// if (gst1s > gst2s) gst2s += 24; -// -// // 5. Calculate GST at 0h UT of this date -// double t00 = utToGst(0); -// -// // 6. Calculate GST at 0h on the observer's longitude -// double offset = ::round(fLongitude*12/PI); // p.95 step 6; he _rounds_ to nearest 15 deg. -// double t00p = t00 - offset*1.002737909; -// if (t00p < 0) t00p += 24; // do NOT normalize -// -// // 7. Adjust -// if (gst1r < t00p) { -// gst1r += 24; -// gst2r += 24; -// } -// if (gst1s < t00p) { -// gst1s += 24; -// gst2s += 24; -// } -// -// // 8. -// double gstr = (24.07*gst1r-t00*(gst2r-gst1r))/(24.07+gst1r-gst2r); -// double gsts = (24.07*gst1s-t00*(gst2s-gst1s))/(24.07+gst1s-gst2s); -// -// // 9. Correct for parallax, refraction, and sun's diameter -// double dec = (pos1.declination + pos2.declination) / 2; -// double psi = ::acos(sin(fLatitude) / cos(dec)); -// double x = 0.830725 * DEG_RAD; // parallax+refraction+diameter -// double y = ::asin(sin(x) / ::sin(psi)) * RAD_DEG; -// double delta_t = 240 * y / cos(dec) / 3600; // hours -// -// // 10. Add correction to GSTs, subtract from GSTr -// gstr -= delta_t; -// gsts += delta_t; -// -// // 11. Convert GST to UT and then to local civil time -// double ut = gstToUt(rise ? gstr : gsts); -// //System.out.println((rise?"rise=":"set=") + ut + ", delta_t=" + delta_t); -// long midnight = DAY_MS * (time / DAY_MS); // Find UT midnight on this day -// return midnight + (long) (ut * 3600000); -// } - -// Commented out - currently unused. ICU 2.6, Alan -// /** -// * Convert local sidereal time to Greenwich sidereal time. -// * Section 15. Duffett-Smith p.21 -// * @param lst in hours (0..24) -// * @return GST in hours (0..24) -// */ -// double lstToGst(double lst) { -// double delta = fLongitude * 24 / CalendarAstronomer_PI2; -// return normalize(lst - delta, 24); -// } - -// Commented out - currently unused. ICU 2.6, Alan -// /** -// * Convert UT to GST on this date. -// * Section 12. Duffett-Smith p.17 -// * @param ut in hours -// * @return GST in hours -// */ -// double utToGst(double ut) { -// return normalize(getT0() + ut*1.002737909, 24); -// } - -// Commented out - currently unused. ICU 2.6, Alan -// /** -// * Convert GST to UT on this date. -// * Section 13. Duffett-Smith p.18 -// * @param gst in hours -// * @return UT in hours -// */ -// double gstToUt(double gst) { -// return normalize(gst - getT0(), 24) * 0.9972695663; -// } - -// Commented out - currently unused. ICU 2.6, Alan -// double getT0() { -// // Common computation for UT <=> GST -// -// // Find JD for 0h UT -// double jd = uprv_floor(getJulianDay() - 0.5) + 0.5; -// -// double s = jd - 2451545.0; -// double t = s / 36525.0; -// double t0 = 6.697374558 + (2400.051336 + 0.000025862*t)*t; -// return t0; -// } - -// Commented out - currently unused. ICU 2.6, Alan -// //------------------------------------------------------------------------- -// // Alternate Sun Rise/Set -// // See sci.astro FAQ -// // http://www.faqs.org/faqs/astronomy/faq/part3/section-5.html -// //------------------------------------------------------------------------- -// -// // Note: This method appears to produce inferior accuracy as -// // compared to getSunRiseSet(). -// -// /** -// * TODO Make this when the entire class is package-private. -// */ -// /*public*/ long getSunRiseSet3(boolean rise) { -// -// // Compute day number for 0.0 Jan 2000 epoch -// double d = (double)(time - EPOCH_2000_MS) / DAY_MS; -// -// // Now compute the Local Sidereal Time, LST: -// // -// double LST = 98.9818 + 0.985647352 * d + /*UT*15 + long*/ -// fLongitude*RAD_DEG; -// // -// // (east long. positive). Note that LST is here expressed in degrees, -// // where 15 degrees corresponds to one hour. Since LST really is an angle, -// // it's convenient to use one unit---degrees---throughout. -// -// // COMPUTING THE SUN'S POSITION -// // ---------------------------- -// // -// // To be able to compute the Sun's rise/set times, you need to be able to -// // compute the Sun's position at any time. First compute the "day -// // number" d as outlined above, for the desired moment. Next compute: -// // -// double oblecl = 23.4393 - 3.563E-7 * d; -// // -// double w = 282.9404 + 4.70935E-5 * d; -// double M = 356.0470 + 0.9856002585 * d; -// double e = 0.016709 - 1.151E-9 * d; -// // -// // This is the obliquity of the ecliptic, plus some of the elements of -// // the Sun's apparent orbit (i.e., really the Earth's orbit): w = -// // argument of perihelion, M = mean anomaly, e = eccentricity. -// // Semi-major axis is here assumed to be exactly 1.0 (while not strictly -// // true, this is still an accurate approximation). Next compute E, the -// // eccentric anomaly: -// // -// double E = M + e*(180/PI) * ::sin(M*DEG_RAD) * ( 1.0 + e*cos(M*DEG_RAD) ); -// // -// // where E and M are in degrees. This is it---no further iterations are -// // needed because we know e has a sufficiently small value. Next compute -// // the true anomaly, v, and the distance, r: -// // -// /* r * cos(v) = */ double A = cos(E*DEG_RAD) - e; -// /* r * ::sin(v) = */ double B = ::sqrt(1 - e*e) * ::sin(E*DEG_RAD); -// // -// // and -// // -// // r = sqrt( A*A + B*B ) -// double v = ::atan2( B, A )*RAD_DEG; -// // -// // The Sun's true longitude, slon, can now be computed: -// // -// double slon = v + w; -// // -// // Since the Sun is always at the ecliptic (or at least very very close to -// // it), we can use simplified formulae to convert slon (the Sun's ecliptic -// // longitude) to sRA and sDec (the Sun's RA and Dec): -// // -// // ::sin(slon) * cos(oblecl) -// // tan(sRA) = ------------------------- -// // cos(slon) -// // -// // ::sin(sDec) = ::sin(oblecl) * ::sin(slon) -// // -// // As was the case when computing az, the Azimuth, if possible use an -// // atan2() function to compute sRA. -// -// double sRA = ::atan2(sin(slon*DEG_RAD) * cos(oblecl*DEG_RAD), cos(slon*DEG_RAD))*RAD_DEG; -// -// double sin_sDec = ::sin(oblecl*DEG_RAD) * ::sin(slon*DEG_RAD); -// double sDec = ::asin(sin_sDec)*RAD_DEG; -// -// // COMPUTING RISE AND SET TIMES -// // ---------------------------- -// // -// // To compute when an object rises or sets, you must compute when it -// // passes the meridian and the HA of rise/set. Then the rise time is -// // the meridian time minus HA for rise/set, and the set time is the -// // meridian time plus the HA for rise/set. -// // -// // To find the meridian time, compute the Local Sidereal Time at 0h local -// // time (or 0h UT if you prefer to work in UT) as outlined above---name -// // that quantity LST0. The Meridian Time, MT, will now be: -// // -// // MT = RA - LST0 -// double MT = normalize(sRA - LST, 360); -// // -// // where "RA" is the object's Right Ascension (in degrees!). If negative, -// // add 360 deg to MT. If the object is the Sun, leave the time as it is, -// // but if it's stellar, multiply MT by 365.2422/366.2422, to convert from -// // sidereal to solar time. Now, compute HA for rise/set, name that -// // quantity HA0: -// // -// // ::sin(h0) - ::sin(lat) * ::sin(Dec) -// // cos(HA0) = --------------------------------- -// // cos(lat) * cos(Dec) -// // -// // where h0 is the altitude selected to represent rise/set. For a purely -// // mathematical horizon, set h0 = 0 and simplify to: -// // -// // cos(HA0) = - tan(lat) * tan(Dec) -// // -// // If you want to account for refraction on the atmosphere, set h0 = -35/60 -// // degrees (-35 arc minutes), and if you want to compute the rise/set times -// // for the Sun's upper limb, set h0 = -50/60 (-50 arc minutes). -// // -// double h0 = -50/60 * DEG_RAD; -// -// double HA0 = ::acos( -// (sin(h0) - ::sin(fLatitude) * sin_sDec) / -// (cos(fLatitude) * cos(sDec*DEG_RAD)))*RAD_DEG; -// -// // When HA0 has been computed, leave it as it is for the Sun but multiply -// // by 365.2422/366.2422 for stellar objects, to convert from sidereal to -// // solar time. Finally compute: -// // -// // Rise time = MT - HA0 -// // Set time = MT + HA0 -// // -// // convert the times from degrees to hours by dividing by 15. -// // -// // If you'd like to check that your calculations are accurate or just -// // need a quick result, check the USNO's Sun or Moon Rise/Set Table, -// // <URL:http://aa.usno.navy.mil/AA/data/docs/RS_OneYear.html>. -// -// double result = MT + (rise ? -HA0 : HA0); // in degrees -// -// // Find UT midnight on this day -// long midnight = DAY_MS * (time / DAY_MS); -// -// return midnight + (long) (result * 3600000 / 15); -// } - -//------------------------------------------------------------------------- -// The Moon -//------------------------------------------------------------------------- - -#define moonL0 (318.351648 * CalendarAstronomer::PI/180 ) // Mean long. at epoch -#define moonP0 ( 36.340410 * CalendarAstronomer::PI/180 ) // Mean long. of perigee -#define moonN0 ( 318.510107 * CalendarAstronomer::PI/180 ) // Mean long. of node -#define moonI ( 5.145366 * CalendarAstronomer::PI/180 ) // Inclination of orbit -#define moonE ( 0.054900 ) // Eccentricity of orbit - -// These aren't used right now -#define moonA ( 3.84401e5 ) // semi-major axis (km) -#define moonT0 ( 0.5181 * CalendarAstronomer::PI/180 ) // Angular size at distance A -#define moonPi ( 0.9507 * CalendarAstronomer::PI/180 ) // Parallax at distance A - -/** - * The position of the moon at the time set on this - * object, in equatorial coordinates. - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -const CalendarAstronomer::Equatorial& CalendarAstronomer::getMoonPosition() -{ - // - // See page 142 of "Practial Astronomy with your Calculator", - // by Peter Duffet-Smith, for details on the algorithm. - // - if (moonPositionSet == FALSE) { - // Calculate the solar longitude. Has the side effect of - // filling in "meanAnomalySun" as well. - getSunLongitude(); - - // - // Find the # of days since the epoch of our orbital parameters. - // TODO: Convert the time of day portion into ephemeris time - // - double day = getJulianDay() - JD_EPOCH; // Days since epoch - - // Calculate the mean longitude and anomaly of the moon, based on - // a circular orbit. Similar to the corresponding solar calculation. - double meanLongitude = norm2PI(13.1763966*PI/180*day + moonL0); - meanAnomalyMoon = norm2PI(meanLongitude - 0.1114041*PI/180 * day - moonP0); - - // - // Calculate the following corrections: - // Evection: the sun's gravity affects the moon's eccentricity - // Annual Eqn: variation in the effect due to earth-sun distance - // A3: correction factor (for ???) - // - double evection = 1.2739*PI/180 * ::sin(2 * (meanLongitude - sunLongitude) - - meanAnomalyMoon); - double annual = 0.1858*PI/180 * ::sin(meanAnomalySun); - double a3 = 0.3700*PI/180 * ::sin(meanAnomalySun); - - meanAnomalyMoon += evection - annual - a3; - - // - // More correction factors: - // center equation of the center correction - // a4 yet another error correction (???) - // - // TODO: Skip the equation of the center correction and solve Kepler's eqn? - // - double center = 6.2886*PI/180 * ::sin(meanAnomalyMoon); - double a4 = 0.2140*PI/180 * ::sin(2 * meanAnomalyMoon); - - // Now find the moon's corrected longitude - moonLongitude = meanLongitude + evection + center - annual + a4; - - // - // And finally, find the variation, caused by the fact that the sun's - // gravitational pull on the moon varies depending on which side of - // the earth the moon is on - // - double variation = 0.6583*CalendarAstronomer::PI/180 * ::sin(2*(moonLongitude - sunLongitude)); - - moonLongitude += variation; - - // - // What we've calculated so far is the moon's longitude in the plane - // of its own orbit. Now map to the ecliptic to get the latitude - // and longitude. First we need to find the longitude of the ascending - // node, the position on the ecliptic where it is crossed by the moon's - // orbit as it crosses from the southern to the northern hemisphere. - // - double nodeLongitude = norm2PI(moonN0 - 0.0529539*PI/180 * day); - - nodeLongitude -= 0.16*PI/180 * ::sin(meanAnomalySun); - - double y = ::sin(moonLongitude - nodeLongitude); - double x = cos(moonLongitude - nodeLongitude); - - moonEclipLong = ::atan2(y*cos(moonI), x) + nodeLongitude; - double moonEclipLat = ::asin(y * ::sin(moonI)); - - eclipticToEquatorial(moonPosition, moonEclipLong, moonEclipLat); - moonPositionSet = TRUE; - } - return moonPosition; -} - -/** - * The "age" of the moon at the time specified in this object. - * This is really the angle between the - * current ecliptic longitudes of the sun and the moon, - * measured in radians. - * - * @see #getMoonPhase - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -double CalendarAstronomer::getMoonAge() { - // See page 147 of "Practial Astronomy with your Calculator", - // by Peter Duffet-Smith, for details on the algorithm. - // - // Force the moon's position to be calculated. We're going to use - // some the intermediate results cached during that calculation. - // - getMoonPosition(); - - return norm2PI(moonEclipLong - sunLongitude); -} - -/** - * Calculate the phase of the moon at the time set in this object. - * The returned phase is a <code>double</code> in the range - * <code>0 <= phase < 1</code>, interpreted as follows: - * <ul> - * <li>0.00: New moon - * <li>0.25: First quarter - * <li>0.50: Full moon - * <li>0.75: Last quarter - * </ul> - * - * @see #getMoonAge - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -double CalendarAstronomer::getMoonPhase() { - // See page 147 of "Practial Astronomy with your Calculator", - // by Peter Duffet-Smith, for details on the algorithm. - return 0.5 * (1 - cos(getMoonAge())); -} - -/** - * Constant representing a new moon. - * For use with {@link #getMoonTime getMoonTime} - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -const CalendarAstronomer::MoonAge CalendarAstronomer::NEW_MOON() { - return CalendarAstronomer::MoonAge(0); -} - -/** - * Constant representing the moon's first quarter. - * For use with {@link #getMoonTime getMoonTime} - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -/*const CalendarAstronomer::MoonAge CalendarAstronomer::FIRST_QUARTER() { - return CalendarAstronomer::MoonAge(CalendarAstronomer::PI/2); -}*/ - -/** - * Constant representing a full moon. - * For use with {@link #getMoonTime getMoonTime} - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -const CalendarAstronomer::MoonAge CalendarAstronomer::FULL_MOON() { - return CalendarAstronomer::MoonAge(CalendarAstronomer::PI); -} -/** - * Constant representing the moon's last quarter. - * For use with {@link #getMoonTime getMoonTime} - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ - -class MoonTimeAngleFunc : public CalendarAstronomer::AngleFunc { -public: - virtual ~MoonTimeAngleFunc(); - virtual double eval(CalendarAstronomer&a) { return a.getMoonAge(); } -}; - -MoonTimeAngleFunc::~MoonTimeAngleFunc() {} - -/*const CalendarAstronomer::MoonAge CalendarAstronomer::LAST_QUARTER() { - return CalendarAstronomer::MoonAge((CalendarAstronomer::PI*3)/2); -}*/ - -/** - * Find the next or previous time at which the Moon's ecliptic - * longitude will have the desired value. - * <p> - * @param desired The desired longitude. - * @param next <tt>true</tt> if the next occurrance of the phase - * is desired, <tt>false</tt> for the previous occurrance. - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -UDate CalendarAstronomer::getMoonTime(double desired, UBool next) -{ - MoonTimeAngleFunc func; - return timeOfAngle( func, - desired, - SYNODIC_MONTH, - MINUTE_MS, - next); -} - -/** - * Find the next or previous time at which the moon will be in the - * desired phase. - * <p> - * @param desired The desired phase of the moon. - * @param next <tt>true</tt> if the next occurrance of the phase - * is desired, <tt>false</tt> for the previous occurrance. - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -UDate CalendarAstronomer::getMoonTime(const CalendarAstronomer::MoonAge& desired, UBool next) { - return getMoonTime(desired.value, next); -} - -class MoonRiseSetCoordFunc : public CalendarAstronomer::CoordFunc { -public: - virtual ~MoonRiseSetCoordFunc(); - virtual void eval(CalendarAstronomer::Equatorial& result, CalendarAstronomer&a) { result = a.getMoonPosition(); } -}; - -MoonRiseSetCoordFunc::~MoonRiseSetCoordFunc() {} - -/** - * Returns the time (GMT) of sunrise or sunset on the local date to which - * this calendar is currently set. - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -UDate CalendarAstronomer::getMoonRiseSet(UBool rise) -{ - MoonRiseSetCoordFunc func; - return riseOrSet(func, - rise, - .533 * DEG_RAD, // Angular Diameter - 34 /60.0 * DEG_RAD, // Refraction correction - MINUTE_MS); // Desired accuracy -} - -//------------------------------------------------------------------------- -// Interpolation methods for finding the time at which a given event occurs -//------------------------------------------------------------------------- - -UDate CalendarAstronomer::timeOfAngle(AngleFunc& func, double desired, - double periodDays, double epsilon, UBool next) -{ - // Find the value of the function at the current time - double lastAngle = func.eval(*this); - - // Find out how far we are from the desired angle - double deltaAngle = norm2PI(desired - lastAngle) ; - - // Using the average period, estimate the next (or previous) time at - // which the desired angle occurs. - double deltaT = (deltaAngle + (next ? 0.0 : - CalendarAstronomer_PI2 )) * (periodDays*DAY_MS) / CalendarAstronomer_PI2; - - double lastDeltaT = deltaT; // Liu - UDate startTime = fTime; // Liu - - setTime(fTime + uprv_ceil(deltaT)); - - // Now iterate until we get the error below epsilon. Throughout - // this loop we use normPI to get values in the range -Pi to Pi, - // since we're using them as correction factors rather than absolute angles. - do { - // Evaluate the function at the time we've estimated - double angle = func.eval(*this); - - // Find the # of milliseconds per radian at this point on the curve - double factor = uprv_fabs(deltaT / normPI(angle-lastAngle)); - - // Correct the time estimate based on how far off the angle is - deltaT = normPI(desired - angle) * factor; - - // HACK: - // - // If abs(deltaT) begins to diverge we need to quit this loop. - // This only appears to happen when attempting to locate, for - // example, a new moon on the day of the new moon. E.g.: - // - // This result is correct: - // newMoon(7508(Mon Jul 23 00:00:00 CST 1990,false))= - // Sun Jul 22 10:57:41 CST 1990 - // - // But attempting to make the same call a day earlier causes deltaT - // to diverge: - // CalendarAstronomer.timeOfAngle() diverging: 1.348508727575625E9 -> - // 1.3649828540224032E9 - // newMoon(7507(Sun Jul 22 00:00:00 CST 1990,false))= - // Sun Jul 08 13:56:15 CST 1990 - // - // As a temporary solution, we catch this specific condition and - // adjust our start time by one eighth period days (either forward - // or backward) and try again. - // Liu 11/9/00 - if (uprv_fabs(deltaT) > uprv_fabs(lastDeltaT)) { - double delta = uprv_ceil (periodDays * DAY_MS / 8.0); - setTime(startTime + (next ? delta : -delta)); - return timeOfAngle(func, desired, periodDays, epsilon, next); - } - - lastDeltaT = deltaT; - lastAngle = angle; - - setTime(fTime + uprv_ceil(deltaT)); - } - while (uprv_fabs(deltaT) > epsilon); - - return fTime; -} - -UDate CalendarAstronomer::riseOrSet(CoordFunc& func, UBool rise, - double diameter, double refraction, - double epsilon) -{ - Equatorial pos; - double tanL = ::tan(fLatitude); - double deltaT = 0; - int32_t count = 0; - - // - // Calculate the object's position at the current time, then use that - // position to calculate the time of rising or setting. The position - // will be different at that time, so iterate until the error is allowable. - // - U_DEBUG_ASTRO_MSG(("setup rise=%s, dia=%.3lf, ref=%.3lf, eps=%.3lf\n", - rise?"T":"F", diameter, refraction, epsilon)); - do { - // See "Practical Astronomy With Your Calculator, section 33. - func.eval(pos, *this); - double angle = ::acos(-tanL * ::tan(pos.declination)); - double lst = ((rise ? CalendarAstronomer_PI2-angle : angle) + pos.ascension ) * 24 / CalendarAstronomer_PI2; - - // Convert from LST to Universal Time. - UDate newTime = lstToUT( lst ); - - deltaT = newTime - fTime; - setTime(newTime); - U_DEBUG_ASTRO_MSG(("%d] dT=%.3lf, angle=%.3lf, lst=%.3lf, A=%.3lf/D=%.3lf\n", - count, deltaT, angle, lst, pos.ascension, pos.declination)); - } - while (++ count < 5 && uprv_fabs(deltaT) > epsilon); - - // Calculate the correction due to refraction and the object's angular diameter - double cosD = ::cos(pos.declination); - double psi = ::acos(sin(fLatitude) / cosD); - double x = diameter / 2 + refraction; - double y = ::asin(sin(x) / ::sin(psi)); - long delta = (long)((240 * y * RAD_DEG / cosD)*SECOND_MS); - - return fTime + (rise ? -delta : delta); -} - /** - * Return the obliquity of the ecliptic (the angle between the ecliptic - * and the earth's equator) at the current time. This varies due to - * the precession of the earth's axis. - * - * @return the obliquity of the ecliptic relative to the equator, - * measured in radians. - */ -double CalendarAstronomer::eclipticObliquity() { - if (isINVALID(eclipObliquity)) { - const double epoch = 2451545.0; // 2000 AD, January 1.5 - - double T = (getJulianDay() - epoch) / 36525; - - eclipObliquity = 23.439292 - - 46.815/3600 * T - - 0.0006/3600 * T*T - + 0.00181/3600 * T*T*T; - - eclipObliquity *= DEG_RAD; - } - return eclipObliquity; -} - - -//------------------------------------------------------------------------- -// Private data -//------------------------------------------------------------------------- -void CalendarAstronomer::clearCache() { - const double INVALID = uprv_getNaN(); - - julianDay = INVALID; - julianCentury = INVALID; - sunLongitude = INVALID; - meanAnomalySun = INVALID; - moonLongitude = INVALID; - moonEclipLong = INVALID; - meanAnomalyMoon = INVALID; - eclipObliquity = INVALID; - siderealTime = INVALID; - siderealT0 = INVALID; - moonPositionSet = FALSE; -} - -//private static void out(String s) { -// System.out.println(s); -//} - -//private static String deg(double rad) { -// return Double.toString(rad * RAD_DEG); -//} - -//private static String hours(long ms) { -// return Double.toString((double)ms / HOUR_MS) + " hours"; -//} - -/** - * @internal - * @deprecated ICU 2.4. This class may be removed or modified. - */ -/*UDate CalendarAstronomer::local(UDate localMillis) { - // TODO - srl ? - TimeZone *tz = TimeZone::createDefault(); - int32_t rawOffset; - int32_t dstOffset; - UErrorCode status = U_ZERO_ERROR; - tz->getOffset(localMillis, TRUE, rawOffset, dstOffset, status); - delete tz; - return localMillis - rawOffset; -}*/ - -// Debugging functions -UnicodeString CalendarAstronomer::Ecliptic::toString() const -{ -#ifdef U_DEBUG_ASTRO - char tmp[800]; - sprintf(tmp, "[%.5f,%.5f]", longitude*RAD_DEG, latitude*RAD_DEG); - return UnicodeString(tmp, ""); -#else - return UnicodeString(); -#endif -} - -UnicodeString CalendarAstronomer::Equatorial::toString() const -{ -#ifdef U_DEBUG_ASTRO - char tmp[400]; - sprintf(tmp, "%f,%f", - (ascension*RAD_DEG), (declination*RAD_DEG)); - return UnicodeString(tmp, ""); -#else - return UnicodeString(); -#endif -} - -UnicodeString CalendarAstronomer::Horizon::toString() const -{ -#ifdef U_DEBUG_ASTRO - char tmp[800]; - sprintf(tmp, "[%.5f,%.5f]", altitude*RAD_DEG, azimuth*RAD_DEG); - return UnicodeString(tmp, ""); -#else - return UnicodeString(); -#endif -} - - -// static private String radToHms(double angle) { -// int hrs = (int) (angle*RAD_HOUR); -// int min = (int)((angle*RAD_HOUR - hrs) * 60); -// int sec = (int)((angle*RAD_HOUR - hrs - min/60.0) * 3600); - -// return Integer.toString(hrs) + "h" + min + "m" + sec + "s"; -// } - -// static private String radToDms(double angle) { -// int deg = (int) (angle*RAD_DEG); -// int min = (int)((angle*RAD_DEG - deg) * 60); -// int sec = (int)((angle*RAD_DEG - deg - min/60.0) * 3600); - -// return Integer.toString(deg) + "\u00b0" + min + "'" + sec + "\""; -// } - -// =============== Calendar Cache ================ - -void CalendarCache::createCache(CalendarCache** cache, UErrorCode& status) { - ucln_i18n_registerCleanup(UCLN_I18N_ASTRO_CALENDAR, calendar_astro_cleanup); - if(cache == NULL) { - status = U_MEMORY_ALLOCATION_ERROR; - } else { - *cache = new CalendarCache(32, status); - if(U_FAILURE(status)) { - delete *cache; - *cache = NULL; - } - } -} - -int32_t CalendarCache::get(CalendarCache** cache, int32_t key, UErrorCode &status) { - int32_t res; - - if(U_FAILURE(status)) { - return 0; - } - umtx_lock(&ccLock); - - if(*cache == NULL) { - createCache(cache, status); - if(U_FAILURE(status)) { - umtx_unlock(&ccLock); - return 0; - } - } - - res = uhash_igeti((*cache)->fTable, key); - U_DEBUG_ASTRO_MSG(("%p: GET: [%d] == %d\n", (*cache)->fTable, key, res)); - - umtx_unlock(&ccLock); - return res; -} - -void CalendarCache::put(CalendarCache** cache, int32_t key, int32_t value, UErrorCode &status) { - if(U_FAILURE(status)) { - return; - } - umtx_lock(&ccLock); - - if(*cache == NULL) { - createCache(cache, status); - if(U_FAILURE(status)) { - umtx_unlock(&ccLock); - return; - } - } - - uhash_iputi((*cache)->fTable, key, value, &status); - U_DEBUG_ASTRO_MSG(("%p: PUT: [%d] := %d\n", (*cache)->fTable, key, value)); - - umtx_unlock(&ccLock); -} - -CalendarCache::CalendarCache(int32_t size, UErrorCode &status) { - fTable = uhash_openSize(uhash_hashLong, uhash_compareLong, NULL, size, &status); - U_DEBUG_ASTRO_MSG(("%p: Opening.\n", fTable)); -} - -CalendarCache::~CalendarCache() { - if(fTable != NULL) { - U_DEBUG_ASTRO_MSG(("%p: Closing.\n", fTable)); - uhash_close(fTable); - } -} - -U_NAMESPACE_END - -#endif // !UCONFIG_NO_FORMATTING |