示例#1
0
// EclipticAberration returns corrections due to aberration for ecliptic
// coordinates of an object.
func EclipticAberration(λ, β, jd float64) (Δλ, Δβ float64) {
	T := base.J2000Century(jd)
	s, _ := solar.True(T)
	e := solar.Eccentricity(T)
	π := perihelion(T)
	sβ, cβ := math.Sincos(β)
	ssλ, csλ := math.Sincos(s - λ)
	sπλ, cπλ := math.Sincos(π - λ)
	// (23.2) p. 151
	Δλ = κ * (e*cπλ - csλ) / cβ
	Δβ = -κ * sβ * (ssλ - e*sπλ)
	return
}
示例#2
0
func ExampleTrue() {
	// Example 25.a, p. 165.
	jd := julian.CalendarGregorianToJD(1992, 10, 13)
	fmt.Printf("JDE: %.1f\n", jd)
	T := base.J2000Century(jd)
	fmt.Printf("T:   %.9f\n", T)
	s, _ := solar.True(T)
	fmt.Printf("☉:   %.5f\n", (s * 180 / math.Pi))
	// Output:
	// JDE: 2448908.5
	// T:   -0.072183436
	// ☉:   199.90987
}
示例#3
0
// EclipticAberration returns corrections due to aberration for ecliptic
// coordinates of an object.
func EclipticAberration(λ, β unit.Angle, jd float64) (Δλ, Δβ unit.Angle) {
	T := base.J2000Century(jd)
	s, _ := solar.True(T)
	e := solar.Eccentricity(T)
	π := perihelion(T)
	sβ, cβ := β.Sincos()
	ssλ, csλ := (s - λ).Sincos()
	sπλ, cπλ := (π - λ).Sincos()
	// (23.2) p. 151
	Δλ = κ.Mul((e*cπλ - csλ) / cβ)
	Δβ = -κ.Mul(sβ * (ssλ - e*sπλ))
	return
}
示例#4
0
// Aberration returns corrections due to aberration for equatorial
// coordinates of an object.
func Aberration(α, δ, jd float64) (Δα2, Δδ2 float64) {
	ε := nutation.MeanObliquity(jd)
	T := base.J2000Century(jd)
	s, _ := solar.True(T)
	e := solar.Eccentricity(T)
	π := perihelion(T)
	sα, cα := math.Sincos(α)
	sδ, cδ := math.Sincos(δ)
	ss, cs := math.Sincos(s)
	sπ, cπ := math.Sincos(π)
	cε := math.Cos(ε)
	tε := math.Tan(ε)
	q1 := cα * cε
	// (23.3) p. 152
	Δα2 = κ * (e*(q1*cπ+sα*sπ) - (q1*cs + sα*ss)) / cδ
	q2 := cε * (tε*cδ - sα*sδ)
	q3 := cα * sδ
	Δδ2 = κ * (e*(cπ*q2+sπ*q3) - (cs*q2 + ss*q3))
	return
}
示例#5
0
// Aberration returns corrections due to aberration for equatorial
// coordinates of an object.
func Aberration(α unit.RA, δ unit.Angle, jd float64) (Δα2 unit.HourAngle, Δδ2 unit.Angle) {
	ε := nutation.MeanObliquity(jd)
	T := base.J2000Century(jd)
	s, _ := solar.True(T)
	e := solar.Eccentricity(T)
	π := perihelion(T)
	sα, cα := α.Sincos()
	sδ, cδ := δ.Sincos()
	ss, cs := s.Sincos()
	sπ, cπ := π.Sincos()
	cε := ε.Cos()
	tε := ε.Tan()
	q1 := cα * cε
	// (23.3) p. 152
	Δα2 = unit.HourAngle(κ.Rad() * (e*(q1*cπ+sα*sπ) - (q1*cs + sα*ss)) / cδ)
	q2 := cε * (tε*cδ - sα*sδ)
	q3 := cα * sδ
	Δδ2 = κ.Mul(e*(cπ*q2+sπ*q3) - (cs*q2 + ss*q3))
	return
}