func newQs(JDE float64) *qs {
var q qs
q.t1 = JDE - 2411093
q.t2 = q.t1 / 365.25
q.t3 = (JDE-2433282.423)/365.25 + 1950
q.t4 = JDE - 2411368
q.t5 = q.t4 / 365.25
q.t6 = JDE - 2415020
q.t7 = q.t6 / 36525
q.t8 = q.t6 / 365.25
q.t9 = (JDE - 2442000.5) / 365.25
q.t10 = JDE - 2409786
q.t11 = q.t10 / 36525
q.W0 = 5.095 * d * (q.t3 - 1866.39)
q.W1 = 74.4*d + 32.39*d*q.t2
q.W2 = 134.3*d + 92.62*d*q.t2
q.W3 = 42*d - .5118*d*q.t5
q.W4 = 276.59*d + .5118*d*q.t5
q.W5 = 267.2635*d + 1222.1136*d*q.t7
q.W6 = 175.4762*d + 1221.5515*d*q.t7
q.W7 = 2.4891*d + .002435*d*q.t7
q.W8 = 113.35*d - .2597*d*q.t7
q.s1, q.c1 = math.Sincos(28.0817 * d)
q.s2, q.c2 = math.Sincos(168.8112 * d)
q.e1 = .05589 - .000346*q.t7
q.sW0 = math.Sin(q.W0)
q.s3W0 = math.Sin(3 * q.W0)
q.s5W0 = math.Sin(5 * q.W0)
q.sW1 = math.Sin(q.W1)
q.sW2 = math.Sin(q.W2)
q.sW3, q.cW3 = math.Sincos(q.W3)
q.sW4, q.cW4 = math.Sincos(q.W4)
q.sW7, q.cW7 = math.Sincos(q.W7)
return &q
}
// AberrationRonVondrak uses the Ron-Vondrák expression to compute corrections
// due to aberration for equatorial coordinates of an object.
func AberrationRonVondrak(α, δ, jd float64) (Δα, Δδ float64) {
T := base.J2000Century(jd)
r := &rv{
T: T,
L2: 3.1761467 + 1021.3285546*T,
L3: 1.7534703 + 628.3075849*T,
L4: 6.2034809 + 334.0612431*T,
L5: 0.5995465 + 52.9690965*T,
L6: 0.8740168 + 21.3299095*T,
L7: 5.4812939 + 7.4781599*T,
L8: 5.3118863 + 3.8133036*T,
Lp: 3.8103444 + 8399.6847337*T,
D: 5.1984667 + 7771.3771486*T,
Mp: 2.3555559 + 8328.6914289*T,
F: 1.6279052 + 8433.4661601*T,
}
var Xp, Yp, Zp float64
// sum smaller terms first
for i := 35; i >= 0; i-- {
x, y, z := rvTerm[i](r)
Xp += x
Yp += y
Zp += z
}
sα, cα := math.Sincos(α)
sδ, cδ := math.Sincos(δ)
// (23.4) p. 156
return (Yp*cα - Xp*sα) / (c * cδ), -((Xp*cα+Yp*sα)*sδ - Zp*cδ) / c
}
// EqToEcl converts equatorial coordinates to ecliptic coordinates.
func (ecl *Ecliptic) EqToEcl(eq *Equatorial, ε *Obliquity) *Ecliptic {
sα, cα := math.Sincos(eq.RA)
sδ, cδ := math.Sincos(eq.Dec)
ecl.Lon = math.Atan2(sα*ε.C+(sδ/cδ)*ε.S, cα) // (13.1) p. 93
ecl.Lat = math.Asin(sδ*ε.C - cδ*ε.S*sα) // (13.2) p. 93
return ecl
}
// EqToEcl converts equatorial coordinates to ecliptic coordinates.
//
// α: right ascension coordinate to transform, in radians
// δ: declination coordinate to transform, in radians
// sε: sine of obliquity of the ecliptic
// cε: cosine of obliquity of the ecliptic
//
// Results:
//
// λ: ecliptic longitude in radians
// β: ecliptic latitude in radians
func EqToEcl(α, δ, sε, cε float64) (λ, β float64) {
sα, cα := math.Sincos(α)
sδ, cδ := math.Sincos(δ)
λ = math.Atan2(sα*cε+(sδ/cδ)*sε, cα) // (13.1) p. 93
β = math.Asin(sδ*cε - cδ*sε*sα) // (13.2) p. 93
return
}
// Horizontal computes data for a horizontal sundial.
//
// Argument φ is geographic latitude at which the sundial will be located,
// a is the length of a straight stylus perpendicular to the plane of the
// sundial.
//
// Results consist of a set of lines, a center point, and u, the length of a
// polar stylus. They are in units of a, the stylus length.
func Horizontal(φ, a float64) (lines []Line, center Point, u float64) {
sφ, cφ := math.Sincos(φ)
tφ := sφ / cφ
for i := 0; i < 24; i++ {
l := Line{Hour: i}
H := float64(i-12) * 15 * math.Pi / 180
aH := math.Abs(H)
sH, cH := math.Sincos(H)
for _, d := range m {
tδ := math.Tan(d * math.Pi / 180)
H0 := math.Acos(-tφ * tδ)
if aH > H0 {
continue // sun below horizon
}
Q := cφ*cH + sφ*tδ
x := a * sH / Q
y := a * (sφ*cH - cφ*tδ) / Q
l.Points = append(l.Points, Point{x, y})
}
if len(l.Points) > 0 {
lines = append(lines, l)
}
}
center.Y = -a / tφ
u = a / math.Abs(sφ)
return
}
// Vertical computes data for a vertical sundial.
//
// Argument φ is geographic latitude at which the sundial will be located.
// D is gnomonic declination, the azimuth of the perpendicular to the plane
// of the sundial, measured from the southern meridian towards the west.
// Argument a is the length of a straight stylus perpendicular to the plane
// of the sundial.
//
// Results consist of a set of lines, a center point, and u, the length of a
// polar stylus. They are in units of a, the stylus length.
func Vertical(φ, D, a float64) (lines []Line, center Point, u float64) {
sφ, cφ := math.Sincos(φ)
tφ := sφ / cφ
sD, cD := math.Sincos(D)
for i := 0; i < 24; i++ {
l := Line{Hour: i}
H := float64(i-12) * 15 * math.Pi / 180
aH := math.Abs(H)
sH, cH := math.Sincos(H)
for _, d := range m {
tδ := math.Tan(d * math.Pi / 180)
H0 := math.Acos(-tφ * tδ)
if aH > H0 {
continue // sun below horizon
}
Q := sD*sH + sφ*cD*cH - cφ*cD*tδ
if Q < 0 {
continue // sun below plane of sundial
}
x := a * (cD*sH - sφ*sD*cH + cφ*sD*tδ) / Q
y := -a * (cφ*cH + sφ*tδ) / Q
l.Points = append(l.Points, Point{x, y})
}
if len(l.Points) > 0 {
lines = append(lines, l)
}
}
center.X = -a * sD / cD
center.Y = a * tφ / cD
u = a / math.Abs(cφ*cD)
return
}
// ParallaxConstants computes parallax constants ρ sin φ′ and ρ cos φ′.
//
// Arguments are geographic latitude φ in radians and height h
// in meters above the ellipsoid.
func (e Ellipsoid) ParallaxConstants(φ, h float64) (s, c float64) {
boa := 1 - e.Fl
su, cu := math.Sincos(math.Atan(boa * math.Tan(φ)))
s, c = math.Sincos(φ)
hoa := h * 1e-3 / e.Er
return su*boa + hoa*s, cu + hoa*c
}
// Andoyer computes approximate geodesic distance between two
// points p1 and p2 on the spheroid s.
// Computations use Andoyer-Lambert first order (in flattening) approximation.
//
// Reference: P.D. Thomas, Mathematical Models for Navigation Systems, TR-182,
// US Naval Oceanographic Office (1965).
func Andoyer(s *Spheroid, p1, p2 LL) float64 {
a, f := s.A(), s.F()
lat1, lon1 := p1.LatLon()
lat2, lon2 := p2.LatLon()
F, G := (lat1+lat2)/2.0, (lat1-lat2)/2.0
L := math.Remainder(lon1-lon2, 360.0) / 2.0
sinF, cosF := math.Sincos((math.Pi / 180.0) * F)
sinG, cosG := math.Sincos((math.Pi / 180.0) * G)
sinL, cosL := math.Sincos((math.Pi / 180.0) * L)
S2 := sq(sinG*cosL) + sq(cosF*sinL)
C2 := sq(cosG*cosL) + sq(sinF*sinL)
S, C := math.Sqrt(S2), math.Sqrt(C2)
omega := math.Atan2(S, C)
R := (S * C) / omega
D := 2.0 * omega * a
H1 := (3.0*R - 1.0) / (2.0 * C2)
H2 := (3.0*R + 1.0) / (2.0 * S2)
dist := D * (1.0 + f*(H1*sq(sinF*cosG)-H2*sq(cosF*sinG)))
if finite(dist) {
return dist
}
// Antipodal points.
if finite(R) {
return 2.0 * s.Quad()
}
// Identical points.
return 0.0
}
// TrueEquatorial returns the true geometric position of the Sun as equatorial coordinates.
func TrueEquatorial(jde float64) (α, δ float64) {
s, _ := True(base.J2000Century(jde))
ε := nutation.MeanObliquity(jde)
ss, cs := math.Sincos(s)
sε, cε := math.Sincos(ε)
// (25.6, 25.7) p. 165
return math.Atan2(cε*ss, cs), sε * ss
}
// Angle returns the angle between great circles defined by three points.
//
// Coordinates may be right ascensions and declinations or longitudes and
// latitudes. If r1, d1, r2, d2 defines one line and r2, d2, r3, d3 defines
// another, the result is the angle between the two lines.
//
// Algorithm by Meeus.
func Angle(r1, d1, r2, d2, r3, d3 float64) float64 {
sd2, cd2 := math.Sincos(d2)
sr21, cr21 := math.Sincos(r2 - r1)
sr32, cr32 := math.Sincos(r3 - r2)
C1 := math.Atan2(sr21, cd2*math.Tan(d1)-sd2*cr21)
C2 := math.Atan2(sr32, cd2*math.Tan(d3)-sd2*cr32)
return C1 + C2
}
// GalToEq converts galactic coordinates to equatorial coordinates.
//
// Resulting equatorial coordinates will be referred to the standard equinox of
// B1950.0. For subsequent conversion to other epochs, see package precess and
// utility functions in package meeus.
func (eq *Equatorial) GalToEq(g *Galactic) *Equatorial {
sdLon, cdLon := math.Sincos(g.Lon - galacticLon0)
sgδ, cgδ := math.Sincos(galacticNorth.Dec)
sb, cb := math.Sincos(g.Lat)
y := math.Atan2(sdLon, cdLon*sgδ-(sb/cb)*cgδ)
eq.RA = base.PMod(y+galacticNorth.RA, 2*math.Pi)
eq.Dec = math.Asin(sb*sgδ + cb*cgδ*cdLon)
return eq
}
// EqToGal converts equatorial coordinates to galactic coordinates.
//
// Equatorial coordinates must be referred to the standard equinox of B1950.0.
// For conversion to B1950, see package precess and utility functions in
// package "common".
func EqToGal(α, δ float64) (l, b float64) {
sdα, cdα := math.Sincos(galacticNorth.RA - α)
sgδ, cgδ := math.Sincos(galacticNorth.Dec)
sδ, cδ := math.Sincos(δ)
x := math.Atan2(sdα, cdα*sgδ-(sδ/cδ)*cgδ) // (13.7) p. 94
l = math.Mod(math.Pi+galacticLon0-x, 2*math.Pi) // (13.8) p. 94
b = math.Asin(sδ*sgδ + cδ*cgδ*cdα)
return
}
// EqToGal converts equatorial coordinates to galactic coordinates.
//
// Equatorial coordinates must be referred to the standard equinox of B1950.0.
// For conversion to B1950, see package precess and utility functions in
// package "common".
func (g *Galactic) EqToGal(eq *Equatorial) *Galactic {
sdα, cdα := math.Sincos(galacticNorth.RA - eq.RA)
sgδ, cgδ := math.Sincos(galacticNorth.Dec)
sδ, cδ := math.Sincos(eq.Dec)
x := math.Atan2(sdα, cdα*sgδ-(sδ/cδ)*cgδ) // (13.7) p. 94
g.Lon = math.Mod(math.Pi+galacticLon0-x, 2*math.Pi) // (13.8) p. 94
g.Lat = math.Asin(sδ*sgδ + cδ*cgδ*cdα)
return g
}
// EqToHz computes Horizontal coordinates from equatorial coordinates.
//
// α: right ascension coordinate to transform, in radians
// δ: declination coordinate to transform, in radians
// φ: latitude of observer on Earth
// ψ: longitude of observer on Earth
// st: sidereal time at Greenwich at time of observation.
//
// Sidereal time must be consistent with the equatorial coordinates.
// If coordinates are apparent, sidereal time must be apparent as well.
//
// Results:
//
// A: azimuth of observed point in radians, measured westward from the South.
// h: elevation, or height of observed point in radians above horizon.
func EqToHz(α, δ, φ, ψ, st float64) (A, h float64) {
H := sexa.Time(st).Rad() - ψ - α
sH, cH := math.Sincos(H)
sφ, cφ := math.Sincos(φ)
sδ, cδ := math.Sincos(ψ)
A = math.Atan2(sH, cH*sφ-(sδ/cδ)*cφ) // (13.5) p. 93
h = math.Asin(sφ*sδ + cφ*cδ*cH) // (13.6) p. 93
return
}
// EqToHz computes Horizontal coordinates from equatorial coordinates.
//
// Argument g is the location of the observer on the Earth. Argument st
// is the sidereal time at Greenwich.
//
// Sidereal time must be consistent with the equatorial coordinates.
// If coordinates are apparent, sidereal time must be apparent as well.
func (hz *Horizontal) EqToHz(eq *Equatorial, g *globe.Coord, st float64) *Horizontal {
H := sexa.Time(st).Rad() - g.Lon - eq.RA
sH, cH := math.Sincos(H)
sφ, cφ := math.Sincos(g.Lat)
sδ, cδ := math.Sincos(eq.Dec)
hz.Az = math.Atan2(sH, cH*sφ-(sδ/cδ)*cφ) // (13.5) p. 93
hz.Alt = math.Asin(sφ*sδ + cφ*cδ*cH) // (13.6) p. 93
return hz
}
// GalToEq converts galactic coordinates to equatorial coordinates.
//
// Resulting equatorial coordinates will be referred to the standard equinox of
// B1950.0. For subsequent conversion to other epochs, see package precess and
// utility functions in package meeus.
func GalToEq(l, b float64) (α, δ float64) {
sdLon, cdLon := math.Sincos(l - galacticLon0)
sgδ, cgδ := math.Sincos(galacticNorth.Dec)
sb, cb := math.Sincos(b)
y := math.Atan2(sdLon, cdLon*sgδ-(sb/cb)*cgδ)
α = base.PMod(y+galacticNorth.RA, 2*math.Pi)
δ = math.Asin(sb*sgδ + cb*cgδ*cdLon)
return
}
// HzToEq transforms horizontal coordinates to equatorial coordinates.
//
// A: azimuth
// h: elevation
// φ: latitude of observer on Earth
// ψ: longitude of observer on Earth
// st: sidereal time at Greenwich at time of observation.
//
// Sidereal time must be consistent with the equatorial coordinates.
// If coordinates are apparent, sidereal time must be apparent as well.
//
// Results:
//
// α: right ascension
// δ: declination
func HzToEq(A, h, φ, ψ, st float64) (α, δ float64) {
sA, cA := math.Sincos(A)
sh, ch := math.Sincos(h)
sφ, cφ := math.Sincos(φ)
H := math.Atan2(sA, cA*sφ+sh/ch*cφ)
α = base.PMod(sexa.Time(st).Rad()-ψ-H, 2*math.Pi)
δ = math.Asin(sφ*sh - cφ*ch*cA)
return
}
// HzToEq transforms horizontal coordinates to equatorial coordinates.
//
// Sidereal time must be consistent with the equatorial coordinates.
// If coordinates are apparent, sidereal time must be apparent as well.
func (eq *Equatorial) HzToEq(hz *Horizontal, g globe.Coord, st float64) *Equatorial {
sA, cA := math.Sincos(hz.Az)
sh, ch := math.Sincos(hz.Alt)
sφ, cφ := math.Sincos(g.Lat)
H := math.Atan2(sA, cA*sφ+sh/ch*cφ)
eq.RA = base.PMod(sexa.Time(st).Rad()-g.Lon-H, 2*math.Pi)
eq.Dec = math.Asin(sφ*sh - cφ*ch*cA)
return eq
}
// ApparentEquatorial returns the apparent position of the Sun as equatorial coordinates.
//
// α: right ascension in radians
// δ: declination in radians
func ApparentEquatorial(jde float64) (α, δ float64) {
T := base.J2000Century(jde)
λ := ApparentLongitude(T)
ε := nutation.MeanObliquity(jde)
sλ, cλ := math.Sincos(λ)
// (25.8) p. 165
sε, cε := math.Sincos(ε + .00256*math.Pi/180*math.Cos(node(T)))
return math.Atan2(cε*sλ, cλ), math.Asin(sε * sλ)
}
// Sep returns the angular separation between two celestial bodies.
//
// The algorithm is numerically naïve, and while patched up a bit for
// small separations, remains unstable for separations near π.
func Sep(r1, d1, r2, d2 float64) float64 {
sd1, cd1 := math.Sincos(d1)
sd2, cd2 := math.Sincos(d2)
cd := sd1*sd2 + cd1*cd2*math.Cos(r1-r2) // (17.1) p. 109
if cd < base.CosSmallAngle {
return math.Acos(cd)
}
return math.Hypot((r2-r1)*cd1, d2-d1) // (17.2) p. 109
}
// SepPauwels returns the angular separation between two celestial bodies.
//
// The algorithm is a numerically stable form of that used in Sep.
func SepPauwels(r1, d1, r2, d2 float64) float64 {
sd1, cd1 := math.Sincos(d1)
sd2, cd2 := math.Sincos(d2)
cdr := math.Cos(r2 - r1)
x := cd1*sd2 - sd1*cd2*cdr
y := cd2 * math.Sin(r2-r1)
z := sd1*sd2 + cd1*cd2*cdr
return math.Atan2(math.Hypot(x, y), z)
}
func (m *moon) optical(λ, β float64) (lʹ, bʹ, A float64) {
// (53.1) p. 372
W := λ - m.Ω // (λ without nutation)
sW, cW := math.Sincos(W)
sβ, cβ := math.Sincos(β)
A = math.Atan2(sW*cβ*cI-sβ*sI, cW*cβ)
lʹ = base.PMod(A-m.F, 2*math.Pi)
bʹ = math.Asin(-sW*cβ*sI - sβ*cI)
return
}
// EclipticAtHorizon computes how the plane of the ecliptic intersects
// the horizon at a given local sidereal time as observed from a given
// geographic latitude.
//
// ε is obliquity of the ecliptic.
// φ is geographic latitude of observer.
// θ is local sidereal time expressed as an hour angle.
//
// λ1 and λ2 are ecliptic longitudes where the ecliptic intersects the horizon.
// I is the angle at which the ecliptic intersects the horizon.
//
// All angles, arguments and results, are in radians.
func EclipticAtHorizon(ε, φ, θ float64) (λ1, λ2, I float64) {
sε, cε := math.Sincos(ε)
sφ, cφ := math.Sincos(φ)
sθ, cθ := math.Sincos(θ)
λ := math.Atan2(-cθ, sε*(sφ/cφ)+cε*sθ) // (14.2) p. 99
if λ < 0 {
λ += math.Pi
}
return λ, λ + math.Pi, math.Acos(cε*sφ - sε*cφ*sθ) // (14.3) p. 99
}
// EclToEq converts ecliptic coordinates to equatorial coordinates.
//
// λ: ecliptic longitude coordinate to transfrom, in radians
// β: ecliptic latitude coordinate to transform, in radians
// sε: sine of obliquity of the ecliptic
// cε: cosine of obliquity of the ecliptic
//
// Results:
// α: right ascension in radians
// δ: declination in radians
func EclToEq(λ, β, sε, cε float64) (α, δ float64) {
sλ, cλ := math.Sincos(λ)
sβ, cβ := math.Sincos(β)
α = math.Atan2(sλ*cε-(sβ/cβ)*sε, cλ) // (13.3) p. 93
if α < 0 {
α += 2 * math.Pi
}
δ = math.Asin(sβ*cε + cβ*sε*sλ) // (13.4) p. 93
return
}
// EclToEq converts ecliptic coordinates to equatorial coordinates.
func (eq *Equatorial) EclToEq(ecl *Ecliptic, ε *Obliquity) *Equatorial {
sβ, cβ := math.Sincos(ecl.Lat)
sλ, cλ := math.Sincos(ecl.Lon)
eq.RA = math.Atan2(sλ*ε.C-(sβ/cβ)*ε.S, cλ) // (13.3) p. 93
if eq.RA < 0 {
eq.RA += 2 * math.Pi
}
eq.Dec = math.Asin(sβ*ε.C + cβ*ε.S*sλ) // (13.4) p. 93
return eq
}
// Topocentric2 returns topocentric corrections including parallax.
//
// This function implements the "non-rigorous" method descripted in the text.
//
// Note that results are corrections, not corrected coordinates.
func Topocentric2(α, δ, Δ, ρsφʹ, ρcφʹ, L, jde float64) (Δα, Δδ float64) {
π := Horizontal(Δ)
θ0 := base.Time(sidereal.Apparent(jde)).Rad()
H := base.PMod(θ0-L-α, 2*math.Pi)
sH, cH := math.Sincos(H)
sδ, cδ := math.Sincos(δ)
Δα = -π * ρcφʹ * sH / cδ // (40.4) p. 280
Δδ = -π * (ρsφʹ*cδ - ρcφʹ*cH*sδ) // (40.5) p. 280
return
}
func (q *qs) hyperion() (r r4) {
η := 92.39*d + .5621071*d*q.t6
ζ := 148.19*d - 19.18*d*q.t8
θ := 184.8*d - 35.41*d*q.t9
θʹ := θ - 7.5*d
as := 176*d + 12.22*d*q.t8
bs := 8*d + 24.44*d*q.t8
cs := bs + 5*d
ϖ := 69.898*d - 18.67088*d*q.t8
φ := 2 * (ϖ - q.W5)
χ := 94.9*d - 2.292*d*q.t8
sη, cη := math.Sincos(η)
sζ, cζ := math.Sincos(ζ)
s2ζ, c2ζ := math.Sincos(2 * ζ)
s3ζ, c3ζ := math.Sincos(3 * ζ)
sζpη, cζpη := math.Sincos(ζ + η)
sζmη, cζmη := math.Sincos(ζ - η)
sφ, cφ := math.Sincos(φ)
sχ, cχ := math.Sincos(χ)
scs, ccs := math.Sincos(cs)
a := 24.50601 - .08686*cη - .00166*cζpη + .00175*cζmη
e := .103458 - .004099*cη - .000167*cζpη + .000235*cζmη +
.02303*cζ - .00212*c2ζ + 0.000151*c3ζ + .00013*cφ
p := ϖ + .15648*d*sχ - .4457*d*sη - .2657*d*sζpη - .3573*d*sζmη -
12.872*d*sζ + 1.668*d*s2ζ - .2419*d*s3ζ - .07*d*sφ
λʹ := 177.047*d + 16.91993829*d*q.t6 + .15648*d*sχ + 9.142*d*sη +
.007*d*math.Sin(2*η) - .014*d*math.Sin(3*η) + .2275*d*sζpη +
.2112*d*sζmη - .26*d*sζ - .0098*d*s2ζ -
.013*d*math.Sin(as) + .017*d*math.Sin(bs) - .0303*d*sφ
i := 27.3347*d + .6434886*d*cχ + .315*d*q.cW3 + .018*d*math.Cos(θ) -
.018*d*ccs
Ω := 168.6812*d + 1.40136*d*cχ + .68599*d*q.sW3 - .0392*d*scs +
.0366*d*math.Sin(θʹ)
return q.subr(λʹ, p, e, a, Ω, i)
}
// Position returns rectangular coordinates referenced to the mean equinox of date.
func Position(e *pp.V87Planet, jde float64) (x, y, z float64) {
// (26.1) p. 171
s, β, R := solar.TrueVSOP87(e, jde)
sε, cε := math.Sincos(nutation.MeanObliquity(jde))
ss, cs := math.Sincos(s)
sβ := math.Sin(β)
x = R * cs
y = R * (ss*cε - sβ*sε)
z = R * (ss*sε + sβ*cε)
return
}
// Nutation returns corrections due to nutation for equatorial coordinates
// of an object.
//
// Results are invalid for objects very near the celestial poles.
func Nutation(α, δ, jd float64) (Δα1, Δδ1 float64) {
ε := nutation.MeanObliquity(jd)
sε, cε := math.Sincos(ε)
Δψ, Δε := nutation.Nutation(jd)
sα, cα := math.Sincos(α)
tδ := math.Tan(δ)
// (23.1) p. 151
Δα1 = (cε+sε*sα*tδ)*Δψ - cα*tδ*Δε
Δδ1 = sε*cα*Δψ + sα*Δε
return
}
func eqProperMotionToEcl(mα, mδ, epoch float64, pos *coord.Ecliptic) (mλ, mβ float64) {
ε := nutation.MeanObliquity(base.JulianYearToJDE(epoch))
sε, cε := math.Sincos(ε)
α, δ := coord.EclToEq(pos.Lon, pos.Lat, sε, cε)
sα, cα := math.Sincos(α)
sδ, cδ := math.Sincos(δ)
cβ := math.Cos(pos.Lat)
mλ = (mδ*sε*cα + mα*cδ*(cε*cδ+sε*sδ*sα)) / (cβ * cβ)
mβ = (mδ*(cε*cδ+sε*sδ*sα) - mα*sε*cα*cδ) / cβ
return
}
