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7322476333c81e529a5781ccad7fcca660d3a1d6
lunar-calendar/aa_full.py
Chen Wei 7322476333 add holiday in AA lunar calendar.
2014-03-12 09:57:46 +08:00

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#!/usr/bin/env python
# -*- coding: utf-8 -*-
''' Implement astronomical algorithms for finding solar terms and moon phases.
Full VSOP87D for calculate Sun's apparent longitude;
Full LEA-406 for calculate Moon's apparent longitude;
Truncated IAU2000B from USNO NOVAS c source is used for nutation.
Reference:
VSOP87: ftp://ftp.imcce.fr/pub/ephem/planets/vsop87
LEA-406: S. M. Kudryavtsev (2007) "Long-term harmonic development of
lunar ephemeris", Astronomy and Astrophysics 471, 1069-1075
'''
__license__ = 'BSD'
__copyright__ = '2014, Chen Wei <weichen302@gmail.com>'
__version__ = '0.0.3'
from numpy import *
import numexpr as ne
from aa_full_table import *
J2000 = 2451545.0
SYNODIC_MONTH = 29.53
MOON_SPEED = 2 * pi / SYNODIC_MONTH
TROPICAL_YEAR = 365.24
SUN_SPEED = 2 * pi / TROPICAL_YEAR
ASEC2RAD = 4.848136811095359935899141e-6
DEG2RAD = 0.017453292519943295
ASEC360 = 1296000.0
PI = pi
TWOPI = 2 * pi
# post import process of LEA-406 tables
# horizontal split the numpy array
F0_V, F1_V, F2_V, F3_V, F4_V = hsplit(M_ARG, 5)
CV = M_PHASE * DEG2RAD
C_V, CT_V, CTT_V = hsplit(CV, 3)
A_V, AT_V, ATT_V = hsplit(M_AMP, 3)
# 77 terms IAU2000B Luni-Solar nutation table from USNO NOVAS c source
#
# Luni-Solar argument multipliers, coefficients, unit 1e-7 arcsec
# L L' F D Om longitude (sin, t*sin, cos), obliquity (cos, t*cos, sin)
IAU2000BNutationTable = array([
[ 0, 0, 0, 0, 1, -172064161, -174666, 33386, 92052331, 9086, 15377 ],
[ 0, 0, 2, -2, 2, -13170906, -1675, -13696, 5730336, -3015, -4587 ],
[ 0, 0, 2, 0, 2, -2276413, -234, 2796, 978459, -485, 1374 ],
[ 0, 0, 0, 0, 2, 2074554, 207, -698, -897492, 470, -291 ],
[ 0, 1, 0, 0, 0, 1475877, -3633, 11817, 73871, -184, -1924 ],
[ 0, 1, 2, -2, 2, -516821, 1226, -524, 224386, -677, -174 ],
[ 1, 0, 0, 0, 0, 711159, 73, -872, -6750, 0, 358 ],
[ 0, 0, 2, 0, 1, -387298, -367, 380, 200728, 18, 318 ],
[ 1, 0, 2, 0, 2, -301461, -36, 816, 129025, -63, 367 ],
[ 0, -1, 2, -2, 2, 215829, -494, 111, -95929, 299, 132 ],
[ 0, 0, 2, -2, 1, 128227, 137, 181, -68982, -9, 39 ],
[ -1, 0, 2, 0, 2, 123457, 11, 19, -53311, 32, -4 ],
[ -1, 0, 0, 2, 0, 156994, 10, -168, -1235, 0, 82 ],
[ 1, 0, 0, 0, 1, 63110, 63, 27, -33228, 0, -9 ],
[ -1, 0, 0, 0, 1, -57976, -63, -189, 31429, 0, -75 ],
[ -1, 0, 2, 2, 2, -59641, -11, 149, 25543, -11, 66 ],
[ 1, 0, 2, 0, 1, -51613, -42, 129, 26366, 0, 78 ],
[ -2, 0, 2, 0, 1, 45893, 50, 31, -24236, -10, 20 ],
[ 0, 0, 0, 2, 0, 63384, 11, -150, -1220, 0, 29 ],
[ 0, 0, 2, 2, 2, -38571, -1, 158, 16452, -11, 68 ],
[ 0, -2, 2, -2, 2, 32481, 0, 0, -13870, 0, 0 ],
[ -2, 0, 0, 2, 0, -47722, 0, -18, 477, 0, -25 ],
[ 2, 0, 2, 0, 2, -31046, -1, 131, 13238, -11, 59 ],
[ 1, 0, 2, -2, 2, 28593, 0, -1, -12338, 10, -3 ],
[ -1, 0, 2, 0, 1, 20441, 21, 10, -10758, 0, -3 ],
[ 2, 0, 0, 0, 0, 29243, 0, -74, -609, 0, 13 ],
[ 0, 0, 2, 0, 0, 25887, 0, -66, -550, 0, 11 ],
[ 0, 1, 0, 0, 1, -14053, -25, 79, 8551, -2, -45 ],
[ -1, 0, 0, 2, 1, 15164, 10, 11, -8001, 0, -1 ],
[ 0, 2, 2, -2, 2, -15794, 72, -16, 6850, -42, -5 ],
[ 0, 0, -2, 2, 0, 21783, 0, 13, -167, 0, 13 ],
[ 1, 0, 0, -2, 1, -12873, -10, -37, 6953, 0, -14 ],
[ 0, -1, 0, 0, 1, -12654, 11, 63, 6415, 0, 26 ],
[ -1, 0, 2, 2, 1, -10204, 0, 25, 5222, 0, 15 ],
[ 0, 2, 0, 0, 0, 16707, -85, -10, 168, -1, 10 ],
[ 1, 0, 2, 2, 2, -7691, 0, 44, 3268, 0, 19 ],
[ -2, 0, 2, 0, 0, -11024, 0, -14, 104, 0, 2 ],
[ 0, 1, 2, 0, 2, 7566, -21, -11, -3250, 0, -5 ],
[ 0, 0, 2, 2, 1, -6637, -11, 25, 3353, 0, 14 ],
[ 0, -1, 2, 0, 2, -7141, 21, 8, 3070, 0, 4 ],
[ 0, 0, 0, 2, 1, -6302, -11, 2, 3272, 0, 4 ],
[ 1, 0, 2, -2, 1, 5800, 10, 2, -3045, 0, -1 ],
[ 2, 0, 2, -2, 2, 6443, 0, -7, -2768, 0, -4 ],
[ -2, 0, 0, 2, 1, -5774, -11, -15, 3041, 0, -5 ],
[ 2, 0, 2, 0, 1, -5350, 0, 21, 2695, 0, 12 ],
[ 0, -1, 2, -2, 1, -4752, -11, -3, 2719, 0, -3 ],
[ 0, 0, 0, -2, 1, -4940, -11, -21, 2720, 0, -9 ],
[ -1, -1, 0, 2, 0, 7350, 0, -8, -51, 0, 4 ],
[ 2, 0, 0, -2, 1, 4065, 0, 6, -2206, 0, 1 ],
[ 1, 0, 0, 2, 0, 6579, 0, -24, -199, 0, 2 ],
[ 0, 1, 2, -2, 1, 3579, 0, 5, -1900, 0, 1 ],
[ 1, -1, 0, 0, 0, 4725, 0, -6, -41, 0, 3 ],
[ -2, 0, 2, 0, 2, -3075, 0, -2, 1313, 0, -1 ],
[ 3, 0, 2, 0, 2, -2904, 0, 15, 1233, 0, 7 ],
[ 0, -1, 0, 2, 0, 4348, 0, -10, -81, 0, 2 ],
[ 1, -1, 2, 0, 2, -2878, 0, 8, 1232, 0, 4 ],
[ 0, 0, 0, 1, 0, -4230, 0, 5, -20, 0, -2 ],
[ -1, -1, 2, 2, 2, -2819, 0, 7, 1207, 0, 3 ],
[ -1, 0, 2, 0, 0, -4056, 0, 5, 40, 0, -2 ],
[ 0, -1, 2, 2, 2, -2647, 0, 11, 1129, 0, 5 ],
[ -2, 0, 0, 0, 1, -2294, 0, -10, 1266, 0, -4 ],
[ 1, 1, 2, 0, 2, 2481, 0, -7, -1062, 0, -3 ],
[ 2, 0, 0, 0, 1, 2179, 0, -2, -1129, 0, -2 ],
[ -1, 1, 0, 1, 0, 3276, 0, 1, -9, 0, 0 ],
[ 1, 1, 0, 0, 0, -3389, 0, 5, 35, 0, -2 ],
[ 1, 0, 2, 0, 0, 3339, 0, -13, -107, 0, 1 ],
[ -1, 0, 2, -2, 1, -1987, 0, -6, 1073, 0, -2 ],
[ 1, 0, 0, 0, 2, -1981, 0, 0, 854, 0, 0 ],
[ -1, 0, 0, 1, 0, 4026, 0, -353, -553, 0, -139 ],
[ 0, 0, 2, 1, 2, 1660, 0, -5, -710, 0, -2 ],
[ -1, 0, 2, 4, 2, -1521, 0, 9, 647, 0, 4 ],
[ -1, 1, 0, 1, 1, 1314, 0, 0, -700, 0, 0 ],
[ 0, -2, 2, -2, 1, -1283, 0, 0, 672, 0, 0 ],
[ 1, 0, 2, 2, 1, -1331, 0, 8, 663, 0, 4 ],
[ -2, 0, 2, 2, 2, 1383, 0, -2, -594, 0, -2 ],
[ -1, 0, 0, 0, 2, 1405, 0, 4, -610, 0, 2 ],
[ 1, 1, 2, -2, 2, 1290, 0, 0, -556, 0, 0 ]
])
def vsopLx(vsopterms, t):
''' helper function for calculate VSOP87 '''
lx = vsopterms[:, 0] * cos(vsopterms[:, 1] + vsopterms[:, 2] * t)
return sum(lx)
def vsop(jde, FK5=True):
''' Calculate ecliptical longitude of earth in heliocentric coordinates,
use VSOP87D table, heliocentric spherical, coordinates referred to the mean
equinox of the date,
In A&A, Meeus said while the complete VSOP87 yields an accuracy of 0.01",
the abridge VSOP87 has an accuracy of 1" for -2000 - +6000.
The VSOP87D table used here is a truncated version, done by the
vsoptrunc-sph.c from Celestia.
Arg:
jde: in JDTT
Return:
earth longitude in radians, referred to mean dynamical ecliptic and
equinox of the date
'''
t = (jde - J2000) / 365250.0
L0 = vsopLx(earth_L0, t)
L1 = vsopLx(earth_L1, t)
L2 = vsopLx(earth_L2, t)
L3 = vsopLx(earth_L3, t)
L4 = vsopLx(earth_L4, t)
L5 = vsopLx(earth_L5, t)
lon = (L0 + t * (L1 + t * (L2 + t * (L3 + t * (L4 + t * L5)))))
if FK5:
#b0 = vsopLx(earth_B0, t)
#b1 = vsopLx(earth_B1, t)
#b2 = vsopLx(earth_B2, t)
#b3 = vsopLx(earth_B3, t)
#b4 = vsopLx(earth_B4, t)
#lat = b0 + t * (b1 + t * (b2 + t * (b3 + t * b4 )))
#lp = lon - 1.397 * t - 0.00031 * t * t
#deltalon = (-0.09033 + 0.03916 * (cos(lp) + sin(lp))
# * tan(lat)) * ASEC2RAD
#print 'FK5 convertion: %s' % fmtdeg(math.degrees(deltalon))
# appears -0.09033 is good enough
#deltal = math.radians(-0.09033 / 3600.0)
deltalon = -4.379321981462438e-07
lon += deltalon
return lon
def rootbysecand(f, angle, x0, x1, precision=0.000000001):
''' solve the equation when function f(jd, angle) reaches zero by
Secand method
'''
fx0, fx1 = f(x0, angle), f(x1, angle)
while abs(fx1) > precision and abs(x0 - x1) > precision and fx0 != fx1:
x2 = x1 - fx1 * (x1 - x0) / (fx1 - fx0)
fx0 = fx1
fx1 = f(x2, angle)
x0 = x1
x1 = x2
return x1
def normrad(r):
''' covernt radian to 0 - 2pi '''
alpha = fmod(r, TWOPI)
if alpha < 0:
alpha += TWOPI
return alpha
def npitopi(r):
''' convert an angle in radians into (-pi, +pi] '''
r = fmod(r, TWOPI)
if r > PI:
r -= TWOPI
elif r <= -1.0 * PI:
r += TWOPI
return r
def fmtdeg(fdegree):
'''convert decimal degree to d m s format string'''
if abs(fdegree) > 360:
fdegree = math.fmod(fdegree, 360.0)
degree = math.fabs(fdegree)
tmp, deg = math.modf(degree)
minutes = tmp * 60
secs = math.modf(minutes)[0] * 60
sign =''
if fdegree < 0:
sign = '-'
res = '''%s%d%s%d'%.6f"''' % (sign, int(deg), u'\N{DEGREE SIGN}',
math.floor(minutes), secs)
return res
def f_solarangle(jd, r_angle):
''' Calculate the difference between target angle and solar geocentric
longitude at a given JDTT
and normalize the angle between Sun's Longitude on a given
day and the angle we are looking for to (-pi, pi), therefore f(x) is
continuous from -pi to pi, '''
return npitopi(apparentsun(jd) - r_angle)
def f_msangle(jd, angle):
''' Calculate difference between target angle and current sun-moon angle
Arg:
jd: time in JDTT
Return:
angle in radians, convert to -pi to +pi range
'''
return npitopi(apparentmoon(jd, ignorenutation=True)
- apparentsun(jd, ignorenutation=True)
- angle)
def solarterm(year, angle):
''' calculate Solar Term by secand method
The Sun's moving speed on ecliptical longitude is 0.04 argsecond / second,
The accuracy of nutation by IAU2000B is 0.001"
Args:
year: the year in integer
angle: degree of the solar term, in integer
Return:
time in JDTT
'''
# mean error when compare apparentsun to NASA(1900-2100) is 0.05"
# 0.000000005 radians = 0.001"
ERROR = 0.000000005
r = normrad(math.radians(angle))
# negative angle means we want search backward from Vernal Equinox,
# initialize x0 to the day which apparent Sun longitude close to the angle
# we searching for
est_vejd = g2jd(year, 3, 20.5)
x0 = est_vejd + angle * 360.0 / 365.24 # estimate
#x0 -= solarangle(x0, r) / SUN_SPEED # further closing
x1 = x0 + 0.5
return rootbysecand(f_solarangle, r, x0, x1, precision=ERROR)
def newmoon(jd):
''' search newmoon near a given date.
Angle between Sun-Moon has been converted to [-pi, pi] range so the
function f_msangle is continuous in that range. Use Secand method to find
root.
Test shows newmoon can be found in 5 iterations, if the start is close
enough, it may use only 3 iterations.
Arg:
jd: in JDTT
Return:
JDTT of newmoon
'''
# 0.0000001 radians is about 0.02 arcsecond, mean error of apparentmoon
# when compared to JPL Horizon is about 0.7 arcsecond
ERROR = 0.0000001
# initilize x0 to the day close to newmoon
x0 = jd - f_msangle(jd, 0) / MOON_SPEED
x1 = x0 + 0.5
return rootbysecand(f_msangle, 0, x0, x1, precision=ERROR)
def findnewmoons(start, count=15):
''' search new moon from specified start time
Arg:
start: the start time in JD, doesn't matter if it is in TT or UT
count: the number of newmoons to search after start time
Return:
a list of JDTT when newmoon occure
'''
nm = 0
newmoons = []
nmcount = 0
count += 1
while nmcount < count:
b = newmoon(start)
if b != nm:
if nm > 0 and abs(nm - b) > (SYNODIC_MONTH + 1):
print 'last newmoon %s, found %s' % (fmtjde2ut(nm),
fmtjde2ut(b))
newmoons.append(b)
nm = b
nmcount += 1
start = nm + SYNODIC_MONTH
else:
start += 1
return newmoons
def apparentmoon(jde, ignorenutation=False):
''' calculate the apparent position of the Moon, it is an alias to the
lea406 function'''
return lea406(jde, ignorenutation)
def apparentsun(jde, ignorenutation=False):
''' calculate the apprent place of the Sun.
Arg:
jde as jde
Return:
geocentric longitude in radians, 0 - 2pi
'''
heliolong = vsop(jde)
geolong = heliolong + PI
# compensate nutation
if not ignorenutation:
geolong += nutation(jde)
labbr = lightabbr_high(jde)
geolong += labbr
return normrad(geolong)
# the higher accuracy light abberation table from A & A.
# the first item of row is the power of time, the 3rd and 4th item are the arg
# of sin, they have been converted into radians.
LIGHTABBR_TABLE = [
[ 0, 118.568, 1.527664004990, 6283.075850600876 ],
[ 0, 2.476, 1.484508993906, 12566.151699456424 ],
[ 0, 1.376, 0.486077687339, 77713.771468687730 ],
[ 0, 0.119, 1.276490181677, 7860.419392621536 ],
[ 0, 0.114, 5.885711004647, 5753.384884566103 ],
[ 0, 0.086, 3.884055717388, 11506.769769132206 ],
[ 0, 0.078, 2.841633387025, 161000.685738008644 ],
[ 0, 0.054, 1.441333038870, 18849.227550057301 ],
[ 0, 0.052, 2.993569534399, 3930.209696310768 ],
[ 0, 0.034, 0.529208263814, 71430.695618086858 ],
[ 0, 0.033, 2.091087703461, 5884.926847413107 ],
[ 0, 0.023, 4.320419446313, 5223.693920276658 ],
[ 0, 0.023, 5.674983441420, 5507.553238331428 ],
[ 0, 0.021, 2.707426294193, 11790.629088932305 ],
[ 1, 7.311, 5.819826570714, 6283.075850600876 ],
[ 1, 0.305, 5.776715192860, 12566.151699456424 ],
[ 1, 0.010, 5.733703298774, 18849.227550057301 ],
[ 2, 0.309, 4.214128894867, 6283.075850600876 ],
[ 2, 0.021, 3.578766215288, 12566.151699456424 ],
[ 2, 0.004, 5.198655163283, 77713.771468687730 ],
[ 3, 0.010, 2.700139544566, 6283.075850600876 ],
]
def lightabbr_high(jd):
'''compute light abberation based on A & A p156
the error will be less than 0.001"
'''
t = (jd - J2000) / 365250.0
# variation of the Sun's longitude
var_lon = 3548.330
for r in LIGHTABBR_TABLE:
var_lon += t ** r[0] * r[1] * sin(r[2] + r[3] * t)
t = (jd - J2000) / 36525.0
t2 = t * t
t3 = t * t2
# mean anomaly of the Sun
M = 357.52910 + 35999.0503 * t - 0.0001559 * t2 - 0.00000048 * t3
# the eccentricity of Earth's orbit
e = 0.016708617 - 0.000042037 * t - 0.0000001236 * t2
# Sun's equation of center
C = ((1.9146 - 0.004817 * t - 0.000014 * t2) * sin(math.radians(M))
+ (0.019993 - 0.000101 * t) * sin(math.radians(2 * M))
+ 0.00029 * sin(math.radians(3 * M)))
# true anomaly
v = M + C
# Sun's distance from the Earth, in AU
R = (1.000001018 * (1 - e * e)) / (1 + e * cos(math.radians(v)))
res = -0.005775518 * R * var_lon * ASEC2RAD
return res
def g2jd(y, m, d):
''' convert a Gregorian date to JD
from AA, p61
'''
if m <= 2:
y -= 1
m += 12
a = int(y / 100)
julian = False
if y < 1582:
julian = True
elif y == 1582:
if m < 10:
julian = True
if m == 10 and d <= 5:
julian = True
if m == 10 and d > 5 and d < 15:
return 2299160.5
if julian:
b = 0
else:
b = 2 - a + int(a / 4)
# 30.6001 is a hack Meeus suggested
return int(365.25 * (y + 4716)) + int(30.6001 * (m + 1)) + d + b - 1524.5
def td2jde(y, m, d):
''' convert Terrestrial (Dynamic) Time to JDE '''
return g2jd(y, m ,d)
def ut2jde(y, m, d):
''' convert UT to JDE, compensate the delta T '''
jd = g2jd(y, m, d)
deltat = deltaT(y, m) / 86400.0
return jd + deltat
def ut2jdut(y, m, d):
''' convert UT to JD, ignore delta T '''
return g2jd(y, m, d)
def jdut2ut(jd):
return jd2g(jd)
def jde2ut(jde, showtime=False):
g = jd2g(jde, showtime)
deltat = deltaT(g[0], g[1]) / 86400.0 # in day
return jd2g(jde - deltat, showtime)
def jde2td(jde):
return jd2g(jde)
def jd2g(jd):
''' convert JD to Gregorian date '''
jd += 0.5
z = int(jd)
f = fmod(jd, 1.0) # decimal part
if z < 2299161:
a = z
else:
alpha = int((z - 1867216.25) / 36524.25)
a = z + 1 + alpha - int(alpha / 4)
b = a + 1524
c = int((b - 122.1) / 365.25)
d = int(365.25 * c)
e = int((b - d) / 30.6001)
res_d = b - d - int(30.6001 * e) + f
if e < 14:
res_m = e - 1
else:
res_m = e - 13
if res_m > 2:
res_y = c - 4716
else:
res_y = c - 4715
return (res_y, res_m, res_d)
def jdptime(isodt, fmt, tz=0, ut=False):
'''
Args:
isodt: datetime string in ISO format
tz: a integer as timezone, e.g. -8 for UTC-8, 2 for UTC2
fmt: like strftime but currently only support three format
%y-%m-%d %H:%M:%S
%y-%m-%d %H:%M
%y-%m-%d
ut: convert to UTC(adjust delta T)
Return:
Julian Day
'''
if fmt == '%y-%m-%d':
isodate = isodt
isot = '00:00:00'
elif fmt == '%y-%m-%d %H:%M':
isodate, isot = isodt.split()
isot += ':00'
else:
isodate, isot = isodt.split()
y, m, d = [int(x) for x in isodate.split('-')]
#if isot:
H, M, S = [int(x) for x in isot.split(':')]
d += (H * 3600 + M * 60 + S) / 86400.0
return g2jd(y, m, d)
def jdftime(jde, fmt='%y-%m-%d %H:%M:%S', tz=0, ut=False):
''' format a Julian Day to ISO format datetime
Args:
jde: time in JDTT
tz: a integer as timezone, e.g. -8 for UTC-8, 2 for UTC2
fmt: like strftime but currently only support three format
%y-%m-%d %H:%M:%S
%y-%m-%d %H:%M
%y-%m-%d
ut: convert to UTC(adjust delta T)
Return:
time string in ISO format, e.g. 1984-01-01 23:59:59
'''
g = jd2g(jde)
deltat = deltaT(g[0], g[1]) if ut else 0
# convert JDE to seconds, then adjust deltat
utsec = jde * 86400.0 + tz * 3600 - deltat
jdut = utsec / 86400.0
# get time in seconds directly to minimize round error
secs = (utsec + 43200) % 86400
if fmt == '%y-%m-%d %H:%M':
secs = int(round(secs / 60.0) * 60.0)
else:
secs = int(secs)
if 86400 == secs:
jdut = int(jdut) + 0.5
secs = 0
y, m, d = jd2g(jdut)
d = int(d)
# use integer math hereafter
H = secs / 3600
ms = secs % 3600
M = ms / 60
S = ms % 60
# padding zero
d = '0%d' % d if d < 10 else str(d)
m = '0%d' % m if m < 10 else str(m)
H = '0%d' % H if H < 10 else str(H)
M = '0%d' % M if M < 10 else str(M)
S = '0%d' % S if S < 10 else str(S)
if fmt == '%y-%m-%d':
isodt = '%d-%s-%s' % (y, m, d)
elif fmt == '%y-%m-%d %H:%M':
isodt = '%d-%s-%s %s:%s' % (y, m, d, H, M)
else:
isodt = '%d-%s-%s %s:%s:%s' % (y, m, d, H, M, S)
return isodt
def deltaT(year, m ,d=0):
''' Polynomial Expressions for Delta T (ΔT) from nasa. Valid for -1999 to
+3000. http://eclipse.gsfc.nasa.gov/LEcat5/deltatpoly.html
Arg:
year: Gregorian year in integer
m: Gregorian month in integer
d: doesn't matter
Result:
ΔT in seconds
verfify against historical records from NASA
year history computed diff
-500 17190 17195.37 5.4
-400 15530 15523.84 6.2
-300 14080 14071.97 8.0
-200 12790 12786.59 3.4
-100 11640 11632.52 7.5
0 10580 10578.95 1.0
100 9600 9592.45 7.6
200 8640 8636.34 3.7
300 7680 7676.67 3.3
400 6700 6694.67 5.3
500 5710 5705.50 4.5
600 4740 4734.89 5.1
700 3810 3809.04 1.0
800 2960 2951.97 8.0
900 2200 2197.11 2.9
1000 1570 1571.65 1.7
1100 1090 1086.99 3.0
1200 740 735.10 4.9
1300 490 490.98 1.0
1400 320 321.09 1.1
1500 200 197.85 2.2
1600 120 119.55 0.5
1700 9 8.90 0.1
1750 13 13.44 0.4
1800 14 13.57 0.4
1850 7 7.16 0.2
1900 -3 -2.12 0.9
1950 29 29.26 0.3
1955 31 31.23 0.1
1960 33 33.31 0.1
1965 36 36.13 0.4
1970 40 40.66 0.5
1975 46 45.94 0.4
1980 50 50.93 0.4
1985 54 54.60 0.3
1990 57 57.20 0.3
1995 61 61.17 0.4
2000 64 64.00 0.2
2005 65 64.85 0.1
Also, JPL uses "last known leap-second is used over any future interval".
It causes the large error when compare apparent sun/moon position with JPL
Horizon
'''
y = year + (m - 0.5) / 12
if year < -500:
u = (year - 1820) / 100.0
return -20 + 32 * u ** 2
elif year < 500:
u = y / 100.0
return 10583.6 + u * (-1014.41 +
u * (33.78311 +
u * (-5.952053 +
u * (-0.1798452 +
u * (0.022174192 +
u * 0.0090316521)))))
elif year < 1600:
u = (y -1000) / 100.0
return 1574.2 + u * (-556.01 +
u * (71.23472 +
u * (0.319781 +
u * (-0.8503463 +
u * (-0.005050998 +
u * 0.0083572073)))))
elif year < 1700:
u = y -1600
return 120 + u * (-0.9808 +
u * (- 0.01532 +
u / 7129))
elif year < 1800:
u = y - 1700
return 8.83 + u * (0.1603 +
u * (-0.0059285 +
u * (0.00013336 +
u / -1174000)))
elif year < 1860:
u = y - 1800
return 13.72 + u * (-0.332447 +
u * (0.0068612 +
u * (0.0041116 +
u * (-0.00037436 +
u * (0.0000121272 +
u * (-0.0000001699 +
u * 0.000000000875))))))
elif year < 1900:
u = y - 1860
return 7.62 + u * (0.5737 +
u * (-0.251754 +
u * (0.01680668 +
u * (-0.0004473624 +
u / 233174))))
elif year < 1920:
u = y - 1900
return -2.79 + u * (1.494119 +
u * (-0.0598939 +
u * (0.0061966 +
u * -0.000197)))
elif year < 1941:
u = y - 1920
return 21.20 + u * (0.84493 +
u * (-0.076100 +
u * 0.0020936))
elif year < 1961:
u = y - 1950
return 29.07 + u * (0.407 +
u * (-1.0 / 233 +
u / 2547))
elif year < 1986:
u = y - 1975
return 45.45 + u * (1.067 +
u * (-1.0 / 260 +
u / -718))
elif year < 2005:
u = y -2000
return 63.86 + u * (0.3345 +
u * (-0.060374 +
u * (0.0017275 +
u * (0.000651814 +
u * 0.00002373599))))
'''
else:
# JPL uses "last known leap-second is used over any future interval" .
# It causes the large error when compare apparent sun/moon position
# with JPL Horizon
return 67.182963
'''
elif year < 2050:
u = y -2000
return 62.92 + u * (0.32217 + u * 0.005589)
elif year < 2150:
u = (y - 1820.0) / 100.0
return -20 + 32 * u ** 2 - 0.5628 * (2150 - y)
else:
u = (y - 1820.0) / 100.0
return -20 + 32 * u ** 2
def nutation(jde):
'''
Calculate nutation angles using the IAU 2000B model.
The table is from NOVAS(USNO) c source flle.
"...the 77-term, IAU-approved truncated nutation series, IAU 2000B, which
is accurate to about 0.001 arcsecond in the interval 1995-2050"
Arg:
jde as JDE
Return:
nutation of longitude in radians
'''
t = (jde - J2000) / 36525.0
#Mean anomaly of the Moon, in arcsec
L = 485868.249036 + t * 1717915923.2178
#Mean anomaly of the Sun.
Lp = 1287104.79305 + t * 129596581.0481
#Mean argument of the latitude of the Moon.
F = 335779.526232 + t * 1739527262.8478
#Mean elongation of the Moon from the Sun.
D = 1072260.70369 + t * 1602961601.2090
#Mean longitude of the ascending node of the Moon.
Om = 450160.398036 - t * 6962890.5431
m1, m2, m3, m4, m5, AA, BB, CC, EE, DD, FF = hsplit(IAU2000BNutationTable,
11)
args = (m1 * L + m2 * Lp + m3 * F + m4 * D + m5 * Om) * ASEC2RAD
lon = sum((AA + BB * t) * sin(args) + CC * cos(args))
# unit of longitude is 1.0e-7 arcsec, convert it to arcsec
lon *= 1.0e-7
# Constant account for the missing long-period planetary terms in the
# truncated nutation model, in arcsec
deplan = 0.000388
lon += deplan
lon *= ASEC2RAD # Convert from arcsec to radians
lon = fmod(lon, TWOPI)
return lon
#------------------------------------------------------------------------------
# LEA-406 Moon Solution
#
# Reference:
# Long-term harmonic development of lunar ephemeris.
# Kudryavtsev S.M. <Astron. Astrophys. 471, 1069 (2007)>
#
# the tables M_AMP, M_PHASE, M_ARG are imported from aa_full_table
#------------------------------------------------------------------------------
FRM = [785939.924268, 1732564372.3047, -5.279, .006665, -5.522e-5 ]
def lea406(jd, ignorenutation=False):
''' compute moon ecliptic longitude using lea406
numpy is used
'''
t = (jd - J2000) / 36525.0
t2 = t * t
t3 = t2 * t
t4 = t3 * t
tm = t / 10.0
tm2 = tm * tm
V = FRM[0] + (((FRM[4] * t + FRM[3]) * t + FRM[2]) * t + FRM[1]) * t
# numpy array operation
ARGS = ne.evaluate('''( F0_V
+ F1_V * t
+ F2_V * t2
+ F3_V * t3
+ F4_V * t4) * ASEC2RAD''')
P = ne.evaluate('''( A_V * sin(ARGS + C_V)
+ AT_V * sin(ARGS + CT_V) * tm
+ ATT_V * sin(ARGS + CTT_V) * tm2)''')
V += sum(P)
V = V * ASEC2RAD
if not ignorenutation:
V += nutation(jd)
return normrad(V)
def main():
#jd = 2444239.5
jd = g2jd(1900, 1, 1)
for i in xrange(1):
l = normrad(lea406(jd))
#d = fmtdeg(math.degrees(npitopi(e -l )))
print jd, l, fmtdeg(math.degrees(l))
jd += 2000
#print fmtdeg(math.degrees(e) % 360.0)
#angle = -105
#while angle < 360:
# a = solarterm(2014, angle)
# print 'search %d %s' % (angle,jdftime(a, tz=8, ut=True))
# angle += 15
if __name__ == "__main__":
main()
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