Golang unit.Angle类代码示例

// 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 unit.Angle, a float64) (lines []Line, center Point, u float64) {
	sφ, cφ := φ.Sincos()
	tφ := sφ / cφ
	sD, cD := D.Sincos()
	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
}

// Kepler1 solves Kepler's equation by iteration.
//
// The iterated formula is
//
//	E1 = M + e * sin(E0)
//
// Argument e is eccentricity, M is mean anomaly,
// places is the desired number of decimal places in the result.
//
// Result E is eccentric anomaly.
//
// For some vaues of e and M it will fail to converge and the
// function will return an error.
func Kepler1(e float64, M unit.Angle, places int) (E unit.Angle, err error) {
	f := func(E0 float64) float64 {
		return M.Rad() + e*math.Sin(E0) // (30.5) p. 195
	}
	ea, err := iterate.DecimalPlaces(f, M.Rad(), places, places*5)
	return unit.Angle(ea), err
}

func (m *moon) physical(A, bʹ unit.Angle) (lʺ, bʺ unit.Angle) {
	// (53.2) p. 373
	sA, cA := A.Sincos()
	lʺ = -m.τ + (m.ρ.Mul(cA) + m.σ.Mul(sA)).Mul(bʹ.Tan())
	bʺ = m.σ.Mul(cA) - m.ρ.Mul(sA)
	return
}

// Kepler2 solves Kepler's equation by iteration.
//
// The iterated formula is
//
//	E1 = E0 + (M + e * sin(E0) - E0) / (1 - e * cos(E0))
//
// Argument e is eccentricity, M is mean anomaly,
// places is the desired number of decimal places in the result.
//
// Result E is eccentric anomaly.
//
// The function converges over a wider range of inputs than does Kepler1
// but it also fails to converge for some values of e and M.
func Kepler2(e float64, M unit.Angle, places int) (E unit.Angle, err error) {
	f := func(E0 float64) float64 {
		se, ce := math.Sincos(E0)
		return E0 + (M.Rad()+e*se-E0)/(1-e*ce) // (30.7) p. 199
	}
	ea, err := iterate.DecimalPlaces(f, M.Rad(), places, places)
	return unit.Angle(ea), err
}

// 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 unit.Angle) unit.Angle {
	sd1, cd1 := d1.Sincos()
	sd2, cd2 := d2.Sincos()
	cdr := (r2 - r1).Cos()
	x := cd1*sd2 - sd1*cd2*cdr
	y := cd2 * (r2 - r1).Sin()
	z := sd1*sd2 + cd1*cd2*cdr
	return unit.Angle(math.Atan2(math.Hypot(x, y), z))
}

// 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 unit.Angle) (α unit.RA, δ unit.Angle) {
	sdLon, cdLon := (l - galacticLon0).Sincos()
	sgδ, cgδ := galacticNorth.Dec.Sincos()
	sb, cb := b.Sincos()
	y := math.Atan2(sdLon, cdLon*sgδ-(sb/cb)*cgδ)
	α = unit.RAFromRad(y + galacticNorth.RA.Rad())
	δ = unit.Angle(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
// in the sense that tf coordinates are apparent, sidereal time must be
// apparent as well.
//
// Results:
//
//	α: right ascension
//	δ: declination
func HzToEq(A, h, φ, ψ unit.Angle, st unit.Time) (α unit.RA, δ unit.Angle) {
	sA, cA := A.Sincos()
	sh, ch := h.Sincos()
	sφ, cφ := φ.Sincos()
	H := math.Atan2(sA, cA*sφ+sh/ch*cφ)
	α = unit.RAFromRad(st.Rad() - ψ.Rad() - H)
	δ = unit.Angle(math.Asin(sφ*sh - cφ*ch*cA))
	return
}

// Kepler2a solves Kepler's equation by iteration.
//
// The iterated formula is the same as in Kepler2 but a limiting function
// avoids divergence.
//
// Argument e is eccentricity, M is mean anomaly,
// places is the desired number of decimal places in the result.
//
// Result E is eccentric anomaly.
func Kepler2a(e float64, M unit.Angle, places int) (E unit.Angle, err error) {
	f := func(E0 float64) float64 {
		se, ce := math.Sincos(E0)
		// method of Leingärtner, p. 205
		return E0 + math.Asin(math.Sin((M.Rad()+e*se-E0)/(1-e*ce)))
	}
	ea, err := iterate.DecimalPlaces(f, M.Rad(), places, places*5)
	return unit.Angle(ea), err
}

// ApparentEccentricity returns apparent eccenticity of a binary star
// given true orbital elements.
//
//  e is eccentricity of the true orbit
//  i is inclination relative to the line of sight
//  ω is longitude of periastron
func ApparentEccentricity(e float64, i, ω unit.Angle) float64 {
	ci := i.Cos()
	sω, cω := ω.Sincos()
	A := (1 - e*e*cω*cω) * ci * ci
	B := e * e * sω * cω * ci
	C := 1 - e*e*sω*sω
	d := A - C
	sD := math.Sqrt(d*d + 4*B*B)
	return math.Sqrt(2 * sD / (A + C + sD))
}

// 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 unit.Angle) unit.Angle {
	sd1, cd1 := d1.Sincos()
	sd2, cd2 := d2.Sincos()
	cd := sd1*sd2 + cd1*cd2*(r1-r2).Cos() // (17.1) p. 109
	if cd < base.CosSmallAngle {
		return unit.Angle(math.Acos(cd))
	}
	// (17.2) p. 109
	return unit.Angle(math.Hypot((r2-r1).Rad()*cd1, (d2 - d1).Rad()))
}

// Times computes UT rise, transit and set times for a celestial object on
// a day of interest.
//
// The function argurments do not actually include the day, but do include
// a number of values computed from the day.
//
//	p is geographic coordinates of observer.
//	ΔT is delta T.
//	h0 is "standard altitude" of the body.
//	Th0 is apparent sidereal time at 0h UT at Greenwich.
//	α3, δ3 are slices of three right ascensions and declinations.
//
// h0 unit is radians.
//
// Th0 must be the time on the day of interest, in seconds.
// See sidereal.Apparent0UT.
//
// α3, δ3 must be values at 0h dynamical time for the day before, the day of,
// and the day after the day of interest.  Units are radians.
//
// Result units are seconds of day and are in the range [0,86400).
func Times(p globe.Coord, ΔT unit.Time, h0 unit.Angle, Th0 unit.Time, α3 []unit.RA, δ3 []unit.Angle) (tRise, tTransit, tSet unit.Time, err error) {
	tRise, tTransit, tSet, err = ApproxTimes(p, h0, Th0, α3[1], δ3[1])
	if err != nil {
		return
	}
	αf := make([]float64, 3)
	for i, α := range α3 {
		αf[i] = α.Rad()
	}
	δf := make([]float64, 3)
	for i, δ := range δ3 {
		δf[i] = δ.Rad()
	}
	var d3α, d3δ *interp.Len3
	d3α, err = interp.NewLen3(-86400, 86400, αf)
	if err != nil {
		return
	}
	d3δ, err = interp.NewLen3(-86400, 86400, δf)
	if err != nil {
		return
	}
	// adjust tTransit
	{
		th0 := (Th0 + tTransit.Mul(360.985647/360)).Mod1()
		α := d3α.InterpolateX((tTransit + ΔT).Sec())
		// local hour angle as Time
		H := th0 - unit.TimeFromRad(p.Lon.Rad()+α)
		tTransit -= H
	}
	// adjust tRise, tSet
	sLat, cLat := p.Lat.Sincos()
	adjustRS := func(m unit.Time) (unit.Time, error) {
		th0 := (Th0 + m.Mul(360.985647/360)).Mod1()
		ut := (m + ΔT).Sec()
		α := d3α.InterpolateX(ut)
		δ := d3δ.InterpolateX(ut)
		Hrad := th0.Rad() - p.Lon.Rad() - α
		sδ, cδ := math.Sincos(δ)
		sH, cH := math.Sincos(Hrad)
		h := math.Asin(sLat*sδ + cLat*cδ*cH)
		md := (unit.TimeFromRad(h) - h0.Time()).Div(cδ * cLat * sH)
		return m + md, nil
	}
	tRise, err = adjustRS(tRise)
	if err != nil {
		return
	}
	tSet, err = adjustRS(tSet)
	return
}

func (m *moon) pa(λ, β, b unit.Angle) unit.Angle {
	V := m.Ω + m.Δψ + m.σ.Div(sI)
	sV, cV := V.Sincos()
	sIρ, cIρ := (_I + m.ρ).Sincos()
	X := sIρ * sV
	Y := sIρ*cV*m.cε - cIρ*m.sε
	ω := math.Atan2(X, Y)
	α, _ := coord.EclToEq(λ+m.Δψ, β, m.sε, m.cε)
	P := unit.Angle(math.Asin(math.Hypot(X, Y) * math.Cos(α.Rad()-ω) / b.Cos()))
	if P < 0 {
		P += 2 * math.Pi
	}
	return P
}

// Kepler2b solves Kepler's equation by iteration.
//
// The iterated formula is the same as in Kepler2 but a (different) limiting
// function avoids divergence.
//
// Argument e is eccentricity, M is mean anomaly,
// places is the desired number of decimal places in the result.
//
// Result E is eccentric anomaly.
func Kepler2b(e float64, M unit.Angle, places int) (E unit.Angle, err error) {
	f := func(E0 float64) float64 {
		se, ce := math.Sincos(E0)
		d := (M.Rad() + e*se - E0) / (1 - e*ce)
		// method of Steele, p. 205
		if d > .5 {
			d = .5
		} else if d < -.5 {
			d = -.5
		}
		return E0 + d
	}
	ea, err := iterate.DecimalPlaces(f, M.Rad(), places, places)
	return unit.Angle(ea), err
}

// TopocentricEcliptical returns topocentric ecliptical coordinates including parallax.
//
// Arguments λ, β are geocentric ecliptical longitude and latitude of a body,
// s is its geocentric semidiameter. φ, h are the observer's latitude and
// and height above the ellipsoid in meters.  ε is the obliquity of the
// ecliptic, θ is local sidereal time, π is equatorial horizontal parallax
// of the body (see Horizonal()).
//
// Results are observed topocentric coordinates and semidiameter.
func TopocentricEcliptical(λ, β, s, φ unit.Angle, h float64, ε unit.Angle, θ unit.Time, π unit.Angle) (λʹ, βʹ, sʹ unit.Angle) {
	S, C := globe.Earth76.ParallaxConstants(φ, h)
	sλ, cλ := λ.Sincos()
	sβ, cβ := β.Sincos()
	sε, cε := ε.Sincos()
	sθ, cθ := θ.Angle().Sincos()
	sπ := π.Sin()
	N := cλ*cβ - C*sπ*cθ
	λʹ = unit.Angle(math.Atan2(sλ*cβ-sπ*(S*sε+C*cε*sθ), N))
	if λʹ < 0 {
		λʹ += 2 * math.Pi
	}
	cλʹ := λʹ.Cos()
	βʹ = unit.Angle(math.Atan(cλʹ * (sβ - sπ*(S*cε-C*sε*sθ)) / N))
	sʹ = unit.Angle(math.Asin(cλʹ * βʹ.Cos() * s.Sin() / N))
	return
}

// Time computes the time at which a moving body is on a straight line (great
// circle) between two fixed points, such as stars.
//
// Coordinates may be right ascensions and declinations or longitudes and
// latitudes.  Fixed points are r1, d1, r2, d2.  Moving body is an ephemeris
// of 5 rows, r3, d3, starting at time t1 and ending at time t5.  Time scale
// is arbitrary.
//
// Result is time of alignment.
func Time(r1, d1, r2, d2 unit.Angle, r3, d3 []unit.Angle, t1, t5 float64) (float64, error) {
	if len(r3) != 5 || len(d3) != 5 {
		return 0, errors.New("r3, d3 must be length 5")
	}
	gc := make([]float64, 5)
	for i, r3i := range r3 {
		// (19.1) p. 121
		gc[i] = d1.Tan()*(r2-r3i).Sin() +
			d2.Tan()*(r3i-r1).Sin() +
			d3[i].Tan()*(r1-r2).Sin()
	}
	l5, err := interp.NewLen5(t1, t5, gc)
	if err != nil {
		return 0, err
	}
	return l5.Zero(false)
}