-í 2FcsúdkZdkZdkZdZdeZ edZ ddZ d„Zd„Zd„Z d„Z  d „Z $d „Z .d „Z ud „Zd „Z©d„Z³d„Z¹d„ZÙed„ZdS(Nf3.1415926535897931f180.0f1.0f360.0csA d|d||dddd|d|dSdS( snA macro to compute the number of days elapsed since 2000 Jan 0.0 (which is equal to 1999 Dec 31, 0h UT)ioii i iii¢% N(sysmsd(sysmsd((s SunRiseSet.pys__daysSince2000Jan0 scsti|tƒSdS(sReturns the sin in degreesN(smathssinsxsDEGRAD(sx((s SunRiseSet.pys__sindscsti|tƒSdS(sReturns the cos in degreesN(smathscossxsDEGRAD(sx((s SunRiseSet.pys__cosdscsti|ƒtSdS(sReturns the arc cos in degreesN(smathsacossxsRADEG(sx((s SunRiseSet.pys__acosdscs! !"ti||ƒtSdS(sReturns the atan2 in degreesN(smathsatan2sysxsRADEG(sysx((s SunRiseSet.pys__atan2d scs-$*+t|||||dddƒSdS(sâ This macro computes times for sunrise/sunset. Sunrise/set is considered to occur when the Sun's upper limb is 35 arc minutes below the horizon (this accounts for the refraction of the Earth's atmosphere). f-35.0f60.0iN(s __sunriset__syearsmonthsdayslonslat(syearsmonthsdayslonslat((s SunRiseSet.pys __sunRiseSet$scsl.JLt|||ƒd|d} Ott| ƒd|ƒ}Rt | ƒ} S| d} T| d} U| d}Xdt|| ƒd}[d |}^|o_||}ndt|ƒt|ƒt| ƒt|ƒt| ƒ} f| d jogd }hd }n:j| d jokd}ld}not| ƒd}r||||fSdS(sC Note: year,month,date = calendar date, 1801-2099 only. Eastern longitude positive, Western longitude negative Northern latitude positive, Southern latitude negative The longitude value IS critical in this function! altit = the altitude which the Sun should cross Set to -35/60 degrees for rise/set, -6 degrees for civil, -12 degrees for nautical and -18 degrees for astronomical twilight. upper_limb: non-zero -> upper limb, zero -> center Set to non-zero (e.g. 1) when computing rise/set times, and to zero when computing start/end of twilight. *rise = where to store the rise time *set = where to store the set time Both times are relative to the specified altitude, and thus this function can be used to compute various twilight times, as well as rise/set times Return value: 0 = sun rises/sets this day, times stored at *trise and *tset. +1 = sun above the specified 'horizon' 24 hours. *trise set to time when the sun is at south, minus 12 hours while *tset is set to the south time plus 12 hours. 'Day' length = 24 hours -1 = sun is below the specified 'horizon' 24 hours 'Day' length = 0 hours, *trise and *tset are both set to the time when the sun is at south. f0.5f360.0f180.0iiif12.0f15.0f0.2666f1.0iÿÿÿÿf0.0f-1.0N(s__daysSince2000Jan0syearsmonthsdayslonsds __revolutions__GMST0ssidtimes __sunRADecsresssRAssdecssrs__rev180stsouthssradiuss upper_limbsaltits__sindslats__cosdscostsrcsts__acosd(syearsmonthsdayslonslatsaltits upper_limbstsouthsrcssdecscostssRAsdsresstssrssidtimessradius((s SunRiseSet.pys __sunriset__.s(!     7    c su{~tdd|ƒ}dd|}€dd|}ƒ||tt|ƒd|t|ƒ} „t| ƒ|}…t i d||ƒt| ƒ}†t i ||||ƒ}‡t||ƒ}ˆ||}‰|djoŠ|d}nŒ||fSd S( så Computes the Sun's ecliptic longitude and distance at an instant given in d, number of days since 2000 Jan 0.0. The Sun's ecliptic latitude is not computed, since it's always very near 0. f356.04700000000003f0.98560025849999999f282.94040000000001f4.7093499999999999e-05f0.016709000000000002f1.1510000000000001e-09f1.0f360.0N(s __revolutionsdsMswsesRADEGs__sinds__cosdsEsxsmathssqrtsysrs__atan2dsvslon( sdseslonsMsrswsvsysxsE((s SunRiseSet.pys__sunposus-$ c sÙ“t|ƒ}”|d}•|d}˜|t|ƒ}™|t|ƒ}œdd|}Ÿ|t|ƒ} |t|ƒ}£t ||ƒ}¤t |t i||||ƒƒ} ¦|| |fSdS(siif23.439299999999999f3.5629999999999998e-07N(s__sunpossdsresslonsrs__cosdsxs__sindsysobl_eclszs__atan2dsRAsmathssqrtsdec( sdsresszslonsrsRAsysxsobl_eclsdec((s SunRiseSet.pys __sunRADecs  'cs&©°±|dti|tƒSdS(sÝ This function reduces any angle to within the first revolution by subtracting or adding even multiples of 360.0 until the result is >= 0.0 and < 360.0 Reduce angle to within 0..360 degrees f360.0N(sxsmathsfloorsINV360(sx((s SunRiseSet.pys __revolution©scs*³¶·|dti|tdƒSdS(s3 Reduce angle to within +180..+180 degrees f360.0f0.5N(sxsmathsfloorsINV360(sx((s SunRiseSet.pys__rev180³scs(¹ÑÕtdd|ƒ}Ö|SdS(sË This function computes GMST0, the Greenwich Mean Sidereal Time at 0h UT (i.e. the sidereal time at the Greenwhich meridian at 0h UT). GMST is then the sidereal time at Greenwich at any time of the day. I've generalized GMST0 as well, and define it as: GMST0 = GMST - UT -- this allows GMST0 to be computed at other times than 0h UT as well. While this sounds somewhat contradictory, it is very practical: instead of computing GMST like: GMST = (GMST0) + UT * (366.2422/365.2422) where (GMST0) is the GMST last time UT was 0 hours, one simply computes: GMST = GMST0 + UT where GMST0 is the GMST "at 0h UT" but at the current moment! Defined in this way, GMST0 will increase with about 4 min a day. It also happens that GMST0 (in degrees, 1 hr = 15 degr) is equal to the Sun's mean longitude plus/minus 180 degrees! (if we neglect aberration, which amounts to 20 seconds of arc or 1.33 seconds of time) f818.98753999999997f0.98564735199999998N(s __revolutionsdssidtim0(sdssidtim0((s SunRiseSet.pys__GMST0¹sc sÙÚ|tjoÛtitiƒƒ}nÜt|d|d|d||ƒ}ß|ddjoàtid}nâti d}äg}åxv|Då]k}æt |ƒ} çti|ƒ\}}èt||ƒ| d<ét|dƒ| d<ê|i| ƒq¡Wë|SdS( Niiiiiii<i(sdatesNonestimesgmtimes __sunRiseSetslonslatstimessaltzonestimeDiffstimezonessunRSTstslists localTimesmathsmodfsminshoursintsappend( slonslatsdateshoursminssunRSTstimesststimeDiffs localTime((s SunRiseSet.pyscalcSunRiseSetÙs'  (smathstimesstringsPIsRADEGsDEGRADsINV360s__daysSince2000Jan0s__sinds__cosds__acosds__atan2ds __sunRiseSets __sunriset__s__sunposs __sunRADecs __revolutions__rev180s__GMST0sNonescalcSunRiseSet(s __sunriset__s__cosdsstrings__sindsDEGRADs__daysSince2000Jan0s __revolutions __sunRADecs__GMST0scalcSunRiseSetsRADEGs__atan2ds __sunRiseSets__sunposstimesPIsINV360s__rev180smaths__acosd((s SunRiseSet.pys?s&            G