feat: 完善日月食与月掩几何链路并扩展历法接口
- 新增日月食中心带、偏食带、阴影足迹、等时线、食分线及升落边界计算，支持极区与混合食拓扑 - 新增日食单时刻阴影求解器、站心状态查询、批量采样和 ΔT 覆盖接口 - 重构恒星与行星月掩路径，补充有限盘面接触、站心修正、掩带宽度、极区投影及升落边界 - 扩展 SVG 与 GeoJSON 输出，支持详细面板、全球/极区/地球投影、边界闭合、时间标记和拓扑签名 - 扩展日月食候选搜索、局地搜索、沙罗序列预计算与范围外推，补充系列锚点和成员一致性校验 - 补齐古历纪年、儒略历独有闰日、多公历候选、历法改革跨日及精确日期运算接口 - 优化 ΔT、章动、恒星时、月球地平线、事件根搜索和本地星历缓存，降低重复计算开销并提升边界稳定
This commit is contained in:
+352
-28
@@ -12,7 +12,7 @@ const (
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SolarEclipseModelNASABulletinSplitK SolarEclipseRadiusModel = "nasa_bulletin_split_k"
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)
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// SolarEclipseType 表示整场日食的全局食型。
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// SolarEclipseType 整场日食的全局食型。
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type SolarEclipseType string
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const (
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@@ -63,6 +63,11 @@ type SolarEclipseResult struct {
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Magnitude float64
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// Gamma 是月影轴到地心的有符号最小距离，单位为地球赤道半径。
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Gamma float64
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// CentralDurationDays 是食甚点的中心食持续时间，单位为日；没有中心食时为 0。
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// 这是日食目录（如 NASA「Central Dur.」）采用的口径：食甚点的中心食时长。
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// CentralDurationDays is the central-phase duration at the greatest eclipse,
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// in days, and 0 when the event has no central phase.
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CentralDurationDays float64
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// PathWidthKM 是食甚点处中心食带宽度。非中心食时为 0。
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PathWidthKM float64
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@@ -100,11 +105,37 @@ type solarEclipseSolver struct {
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model SolarEclipseRadiusModel
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params solarEclipseModelParameters
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localStateContextCache map[uint64]localSolarEclipseStateContext
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localEphemeris *solarEclipseLocalEphemeris
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// deltaTSeconds 是调用方显式给出的 ΔT（秒）；NaN 表示未覆盖，用进程级模型。
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// 只影响地球自转相位（轴的 gst），不改变任何 TT 时刻。
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deltaTSeconds float64
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besselGeometryCache map[uint64]solarEclipseBesselGeometryCacheEntry
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besselCandidateCache map[uint64]solarEclipseBesselGeometryCacheEntry
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exactCentralContact bool
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meanSunMoonDistance float64
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penumbraConeTangent float64
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umbraConeTangent float64
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}
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const solarEclipseBesselGeometryCacheMaximumEntries = movingDiskEventCacheMaximumEntries
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// solarEclipseBesselGeometryCacheEntry keeps exact and candidate geometry in
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// separate maps. Candidate geometry is interpolated and is only suitable for
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// coarse scans; mixing it with exact geometry would silently reduce contact
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// and topology accuracy.
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type solarEclipseBesselGeometryCacheEntry struct {
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// generation 记录写入时的 ΔT 世代：轴里的 gst 由 ΔT 决定，ΔT 覆盖后条目必须失效。
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// generation is the ΔT generation at write time: the axis carries a ΔT-dependent
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// gst, so overriding ΔT has to invalidate the entry.
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generation uint64
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moon [3]float64
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axis solarEclipseAxis
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sun [3]float64
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valid bool
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}
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type solarEclipseFeature struct {
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greatestEclipseJDE float64
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greatestLongitude float64
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@@ -132,19 +163,31 @@ type solarEclipseLineIntersection struct {
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const (
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solarEclipseEarthEquatorialRadiusKM = 6378.1366
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solarEclipseEarthPolarRatio = 0.99664719
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solarEclipseEarthPolarRatioSquared = solarEclipseEarthPolarRatio * solarEclipseEarthPolarRatio
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solarEclipseAstronomicalUnitKM = 1.49597870691e8
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// 赤道自转线速度，用于把 ΔT 误差换算成地面横移（见 DeltaTGroundShiftKM）。
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// Equatorial rotation speed, used to convert a ΔT error into ground displacement.
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solarEclipseEarthEquatorialRotationKMPerSecond = 0.4651
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solarEclipseEarthPolarRatio = 0.99664719
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solarEclipseEarthPolarRatioSquared = solarEclipseEarthPolarRatio * solarEclipseEarthPolarRatio
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solarEclipseAstronomicalUnitKM = 1.49597870691e8
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// IAU Single-K 对所有接触统一使用 0.2725076；
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// NASA bulletin Split-K 对半影仍使用 0.2725076，对本影/反本影使用 0.2722810。
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solarEclipseSolarRadiusRatio = 109.1222
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solarEclipsePenumbralK = 0.2725076
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solarEclipseUmbralK = 0.2722810
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// SolarEclipsePenumbralK 与 SolarEclipseUmbralK 是月面半径与地球赤道半径之比，
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// 即 NASA 星历表里的 k1（半影）与 k2（本影/反本影）；IAU Single-K 两者都用 k1。
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// SolarEclipsePenumbralK and SolarEclipseUmbralK are the lunar-to-terrestrial radius ratios
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// published as k1 (penumbra) and k2 (umbra/antumbra); IAU Single-K uses k1 for both.
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SolarEclipsePenumbralK = solarEclipsePenumbralK
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SolarEclipseUmbralK = solarEclipseUmbralK
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solarEclipseNodeCount = 7
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solarEclipseNodeStepDays = 0.04
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solarEclipseMoonLonAberrRad = -3.4e-6
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solarEclipseNodeCount = 7
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solarEclipseNodeStepDays = 0.04
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solarEclipseMoonLonAberrRad = -3.4e-6
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solarEclipseAxisContactInitialStepDays = 1.0 / 86400.0
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solarEclipseAxisContactMaximumStepDays = 30.0 / 1440.0
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solarEclipseAxisContactToleranceDays = 1e-9
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// 这两个系数沿用经典贝塞尔近似中的极区有效半径经验值。
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solarEclipseNonCentralLimit = 0.9972
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@@ -169,8 +212,21 @@ func SolarEclipseNASABulletinSplitK(seedJDE float64) SolarEclipseResult {
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}
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func solarEclipse(seedJDE float64, model SolarEclipseRadiusModel) SolarEclipseResult {
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return solarEclipseWithDeltaT(seedJDE, model, 0)
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}
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func solarEclipseWithDeltaT(
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seedJDE float64,
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model SolarEclipseRadiusModel,
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deltaTSeconds float64,
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) SolarEclipseResult {
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newMoonJDE := CalcMoonSHByJDE(seedJDE, 0)
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solver := newSolarEclipseSolver(newMoonJDE, model)
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solver := newSolarEclipseSolver(newMoonJDE, model).withDeltaTSeconds(deltaTSeconds)
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return solver.eclipseResult()
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}
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func (solver solarEclipseSolver) eclipseResult() SolarEclipseResult {
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model := solver.model
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feature := solver.feature()
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result := SolarEclipseResult{
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@@ -213,6 +269,7 @@ func solarEclipse(seedJDE float64, model SolarEclipseRadiusModel) SolarEclipseRe
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result.HasCentral = true
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result.CentralBeginOnEarth = feature.centralBeginJDE
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result.CentralEndOnEarth = feature.centralEndJDE
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result.CentralDurationDays = solver.greatestCentralDuration(result)
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}
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switch result.Type {
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@@ -229,6 +286,18 @@ func solarEclipse(seedJDE float64, model SolarEclipseRadiusModel) SolarEclipseRe
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return result
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}
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// greatestCentralDuration 在食甚点解一次站心中心食并返回中心相时长（日）；没有中心相时为 0。
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// greatestCentralDuration solves the local eclipse at the greatest eclipse point and
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// returns its central-phase duration in days.
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func (solver solarEclipseSolver) greatestCentralDuration(result SolarEclipseResult) float64 {
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if !result.HasCentral || result.GreatestEclipse <= 0 {
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return 0
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}
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return solver.centralPhaseDurationDaysAt(
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result.GreatestEclipse, result.GreatestLongitude, result.GreatestLatitude,
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)
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}
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func newSolarEclipseSolver(newMoonJDE float64, model SolarEclipseRadiusModel) solarEclipseSolver {
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params := solarEclipseModelParameters{
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penumbralK: solarEclipsePenumbralK,
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@@ -246,22 +315,67 @@ func newSolarEclipseSolver(newMoonJDE float64, model SolarEclipseRadiusModel) so
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meanSunMoonDistance := ((firstSun[2] + lastSun[2]) - (firstMoon[2] + lastMoon[2])) / 2 / solarEclipseEarthEquatorialRadiusKM
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return solarEclipseSolver{
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newMoonJDE: newMoonJDE,
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model: model,
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params: params,
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meanSunMoonDistance: meanSunMoonDistance,
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penumbraConeTangent: (solarEclipseSolarRadiusRatio + params.penumbralK) / meanSunMoonDistance,
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umbraConeTangent: (solarEclipseSolarRadiusRatio - params.umbralK) / meanSunMoonDistance,
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newMoonJDE: newMoonJDE,
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model: model,
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params: params,
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deltaTSeconds: math.NaN(),
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localStateContextCache: make(map[uint64]localSolarEclipseStateContext),
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besselGeometryCache: make(map[uint64]solarEclipseBesselGeometryCacheEntry),
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besselCandidateCache: make(map[uint64]solarEclipseBesselGeometryCacheEntry),
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meanSunMoonDistance: meanSunMoonDistance,
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penumbraConeTangent: (solarEclipseSolarRadiusRatio + params.penumbralK) / meanSunMoonDistance,
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umbraConeTangent: (solarEclipseSolarRadiusRatio - params.umbralK) / meanSunMoonDistance,
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}
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}
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// withDeltaTSeconds 固定本求解器使用的 ΔT（秒），非正值表示回到进程级模型。覆盖会改变
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// 轴里的 gst，因此所有按精确 float 位键控的几何缓存必须同时作废。
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func (solver solarEclipseSolver) withDeltaTSeconds(deltaTSeconds float64) solarEclipseSolver {
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if deltaTSeconds <= 0 || math.IsNaN(deltaTSeconds) || math.IsInf(deltaTSeconds, 0) {
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deltaTSeconds = math.NaN()
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}
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solver.deltaTSeconds = deltaTSeconds
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solver.besselGeometryCache = make(map[uint64]solarEclipseBesselGeometryCacheEntry)
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solver.besselCandidateCache = make(map[uint64]solarEclipseBesselGeometryCacheEntry)
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solver.localStateContextCache = make(map[uint64]localSolarEclipseStateContext)
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return solver
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}
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// effectiveDeltaTSeconds 返回本求解器在某 TT 时刻实际使用的 ΔT（秒）。
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func (solver solarEclipseSolver) effectiveDeltaTSeconds(jd float64) float64 {
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if math.IsNaN(solver.deltaTSeconds) {
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return DeltaT(jd, true)
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}
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return solver.deltaTSeconds
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}
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// siderealTimeAt 返回某 TT 时刻的视恒星时（弧度），ΔT 覆盖时同样生效。
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func (solver solarEclipseSolver) siderealTimeAt(jd float64) float64 {
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utJDE := TD2UT(jd, false)
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if !math.IsNaN(solver.deltaTSeconds) {
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utJDE = jd - solver.deltaTSeconds/86400
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}
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return ApparentSiderealTime(utJDE) * 15 * rad
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}
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// withLocalEphemeris prepares the immutable event-local interpolator used by
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// coarse candidate scans. The exact ephemeris remains the fallback outside its
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// bounded window and is used by all contact and topology refinements.
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func (solver solarEclipseSolver) withLocalEphemeris() solarEclipseSolver {
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if solver.localEphemeris == nil {
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solver.localEphemeris = newSolarEclipseLocalEphemeris(solver.newMoonJDE)
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}
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return solver
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}
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func (solver solarEclipseSolver) feature() solarEclipseFeature {
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const finiteDifferenceStep = 0.04
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candidateSolver := solver.withLocalEphemeris()
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jd := solver.newMoonJDE
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before := solver.besselMoonAt(jd - finiteDifferenceStep)
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center := solver.besselMoonAt(jd)
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after := solver.besselMoonAt(jd + finiteDifferenceStep)
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before := candidateSolver.besselMoonCandidateAt(jd - finiteDifferenceStep)
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center := candidateSolver.besselMoonCandidateAt(jd)
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after := candidateSolver.besselMoonCandidateAt(jd + finiteDifferenceStep)
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vx := (after[0] - before[0]) / (2 * finiteDifferenceStep)
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vy := (after[1] - before[1]) / (2 * finiteDifferenceStep)
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@@ -271,9 +385,15 @@ func (solver solarEclipseSolver) feature() solarEclipseFeature {
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t0 := -(center[0]*vx + center[1]*vy) / speedSquared
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greatestEclipseJDE := jd + t0
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xc := center[0] + vx*t0
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yc := center[1] + vy*t0
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zc := center[2] + vz*t0 - 1.37*t0*t0
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// The three-node velocity fit locates greatest eclipse accurately, but its
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// linearly extrapolated coordinates can miss the true Bessel position by
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// tens of kilometres in a grazing non-central event. Re-evaluate the
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// ephemeris at the solved time before deriving surface coordinates and
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// shadow radii so markers and path geometry use the same state.
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greatestMoon := solver.besselMoonAt(greatestEclipseJDE)
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xc := greatestMoon[0]
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yc := greatestMoon[1]
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zc := greatestMoon[2]
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gamma := (vx*center[1] - vy*center[0]) / speed
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minimumDistance := math.Abs(gamma)
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axis := solver.besselAxisAt(greatestEclipseJDE)
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@@ -379,14 +499,120 @@ func (solver solarEclipseSolver) feature() solarEclipseFeature {
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_, _, feature.partialEndJDE, _ = solver.quickContactAt(partialEndParam+jd, vx, vy, true)
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}
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if typeCode != "N" && typeCode != "P" {
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if axisIntersection.valid && typeCode != "N" && typeCode != "P" {
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_, _, feature.centralBeginJDE, _ = solver.quickContactAt(centralStartParam+jd, vx, vy, false)
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_, _, feature.centralEndJDE, _ = solver.quickContactAt(centralEndParam+jd, vx, vy, false)
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if refined, ok := solver.centralAxisContactJDE(feature.centralBeginJDE, greatestEclipseJDE, -1); ok {
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feature.centralBeginJDE = refined
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}
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if refined, ok := solver.centralAxisContactJDE(feature.centralEndJDE, greatestEclipseJDE, 1); ok {
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feature.centralEndJDE = refined
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}
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}
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return feature
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}
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func (solver solarEclipseSolver) centralAxisContactJDE(
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approximateJDE, greatestJDE, direction float64,
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) (float64, bool) {
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if !finite(approximateJDE) || !finite(greatestJDE) || direction == 0 {
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return 0, false
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}
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insideJDE, insideResidual := approximateJDE, solver.centralAxisEarthDiscriminant(approximateJDE)
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if !finite(insideResidual) || insideResidual < 0 {
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insideJDE = greatestJDE
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insideResidual = solver.centralAxisEarthDiscriminant(insideJDE)
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if !finite(insideResidual) || insideResidual < 0 {
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return 0, false
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}
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}
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outsideJDE, outsideResidual := 0.0, 0.0
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foundOutside := false
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for step := solarEclipseAxisContactInitialStepDays; step <= solarEclipseAxisContactMaximumStepDays; step *= 2 {
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candidateJDE := approximateJDE + direction*step
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candidateResidual := solver.centralAxisEarthDiscriminant(candidateJDE)
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if !finite(candidateResidual) {
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continue
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}
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if candidateResidual <= 0 {
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outsideJDE, outsideResidual = candidateJDE, candidateResidual
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foundOutside = true
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break
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}
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insideJDE, insideResidual = candidateJDE, candidateResidual
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}
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if !foundOutside {
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return 0, false
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}
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for iteration := 0; iteration < 24 && math.Abs(outsideJDE-insideJDE) > solarEclipseAxisContactToleranceDays; iteration++ {
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candidateJDE := (insideJDE + outsideJDE) / 2
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denominator := insideResidual - outsideResidual
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if denominator != 0 {
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fraction := insideResidual / denominator
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if fraction > 0.1 && fraction < 0.9 {
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candidateJDE = insideJDE + fraction*(outsideJDE-insideJDE)
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}
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}
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candidateResidual := solver.centralAxisEarthDiscriminant(candidateJDE)
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if !finite(candidateResidual) {
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return 0, false
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}
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if candidateResidual >= 0 {
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insideJDE, insideResidual = candidateJDE, candidateResidual
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} else {
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outsideJDE, outsideResidual = candidateJDE, candidateResidual
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}
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}
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return (insideJDE + outsideJDE) / 2, true
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}
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func (solver solarEclipseSolver) centralAxisEarthDiscriminant(jd float64) float64 {
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moon, axis, _ := solver.besselGeometryAt(jd)
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return solarEclipseLineEllipsoidDiscriminant(
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moon[0], moon[1], 2,
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moon[0], moon[1], 0,
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solarEclipseEarthPolarRatio, 1, axis,
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)
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}
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func (solver solarEclipseSolver) centralAxisContactPointAt(jd float64) (SolarEclipsePathPoint, bool) {
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moon, axis, _ := solver.besselGeometryAt(jd)
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cosTilt, sinTilt := math.Cos(axis.tilt), math.Sin(axis.tilt)
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x1 := moon[0]
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y1 := cosTilt*moon[1] - 2*sinTilt
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z1 := sinTilt*moon[1] + 2*cosTilt
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x2 := moon[0]
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y2 := cosTilt * moon[1]
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z2 := sinTilt * moon[1]
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dx, dy, dz := x2-x1, y2-y1, z2-z1
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polarRatioSquared := solarEclipseEarthPolarRatioSquared
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a := dx*dx + dy*dy + dz*dz/polarRatioSquared
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if !finite(a) || a <= 0 {
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return SolarEclipsePathPoint{}, false
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}
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b := x1*dx + y1*dy + z1*dz/polarRatioSquared
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t := -b / a
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intersection := solarEclipseLineIntersection{
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valid: true,
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x: x1 + dx*t,
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y: y1 + dy*t,
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z: z1 + dz*t,
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}
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longitude, latitude := solarEclipseIntersectionGeodetic(intersection, axis)
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if !finite(longitude) || !finite(latitude) {
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return SolarEclipsePathPoint{}, false
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}
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return SolarEclipsePathPoint{
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JDE: jd,
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Longitude: longitude,
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Latitude: latitude,
|
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SunAltitude: solarEclipseSunAltitudeAtGreatest(jd, longitude, latitude, axis.gst) / rad,
|
||||
}, true
|
||||
}
|
||||
|
||||
func (solver solarEclipseSolver) quickContactAt(jd, dx, dy float64, penumbral bool) (float64, float64, float64, bool) {
|
||||
moon := solver.besselMoonAt(jd)
|
||||
radii := solver.shadowRadiiAt(moon[2])
|
||||
@@ -431,11 +657,28 @@ func (solver solarEclipseSolver) shadowRadiiAt(moonBesselZ float64) solarEclipse
|
||||
|
||||
func (solver solarEclipseSolver) besselAxisAt(jd float64) solarEclipseAxis {
|
||||
sun, moon := solarEclipseSunMoonEquatorial(jd)
|
||||
return solarEclipseBesselAxisFromEquatorialWithDeltaT(
|
||||
jd, sun, moon, solver.effectiveDeltaTSeconds(jd),
|
||||
)
|
||||
}
|
||||
|
||||
func solarEclipseBesselAxisFromEquatorial(jd float64, sun, moon [3]float64) solarEclipseAxis {
|
||||
return solarEclipseBesselAxisFromEquatorialWithDeltaT(jd, sun, moon, DeltaT(jd, true))
|
||||
}
|
||||
|
||||
// solarEclipseBesselAxisFromEquatorialWithDeltaT 用显式 ΔT 构造贝塞尔轴：TT 时刻保持
|
||||
// 不变，ΔT 只决定地球自转相位（恒星时），因此同一 TT 在不同 ΔT 下得到的地面足迹会
|
||||
// 沿经度平移，这正是"ΔT 只影响自转、不影响几何时刻"的实现点。
|
||||
// solarEclipseBesselAxisFromEquatorialWithDeltaT builds the Besselian axis with an
|
||||
// explicit ΔT: the TT instant is untouched and ΔT only sets Earth rotation.
|
||||
func solarEclipseBesselAxisFromEquatorialWithDeltaT(
|
||||
jd float64, sun, moon [3]float64, deltaTSeconds float64,
|
||||
) solarEclipseAxis {
|
||||
sunXYZ := solarEclipseLLRToXYZ(sun[0], sun[1], sun[2])
|
||||
moonXYZ := solarEclipseLLRToXYZ(moon[0], moon[1], moon[2])
|
||||
axis := solarEclipseXYZToLLR(sunXYZ[0]-moonXYZ[0], sunXYZ[1]-moonXYZ[1], sunXYZ[2]-moonXYZ[2])
|
||||
|
||||
utJDE := TD2UT(jd, false)
|
||||
utJDE := jd - deltaTSeconds/86400
|
||||
return solarEclipseAxis{
|
||||
rightAscension: solarEclipseNormalizeRadians(math.Pi/2 + axis[0]),
|
||||
tilt: math.Pi/2 - axis[1],
|
||||
@@ -444,9 +687,83 @@ func (solver solarEclipseSolver) besselAxisAt(jd float64) solarEclipseAxis {
|
||||
}
|
||||
|
||||
func (solver solarEclipseSolver) besselMoonAt(jd float64) [3]float64 {
|
||||
_, moon := solarEclipseSunMoonEquatorial(jd)
|
||||
axis := solver.besselAxisAt(jd)
|
||||
moon, _, _ := solver.besselGeometryAt(jd)
|
||||
return moon
|
||||
}
|
||||
|
||||
func (solver solarEclipseSolver) besselMoonCandidateAt(jd float64) [3]float64 {
|
||||
moon, _, _, ok := solver.besselGeometryCandidateAt(jd)
|
||||
if !ok {
|
||||
return solver.besselMoonAt(jd)
|
||||
}
|
||||
return moon
|
||||
}
|
||||
|
||||
func (solver solarEclipseSolver) besselGeometryAt(jd float64) ([3]float64, solarEclipseAxis, [3]float64) {
|
||||
key := math.Float64bits(jd)
|
||||
// 命中要求 ΔT 世代一致：轴里的 gst 依赖 ΔT，SetDeltaTFn 之后旧条目必须视为未命中。
|
||||
// A hit requires the same ΔT generation: the cached axis carries a ΔT-dependent gst,
|
||||
// so entries written before a SetDeltaTFn override must count as misses.
|
||||
if entry, ok := solver.besselGeometryCache[key]; ok && entry.generation == deltaTGenerationValue() {
|
||||
return entry.moon, entry.axis, entry.sun
|
||||
}
|
||||
sun, moon := solarEclipseSunMoonEquatorial(jd)
|
||||
axis := solarEclipseBesselAxisFromEquatorialWithDeltaT(
|
||||
jd, sun, moon, solver.effectiveDeltaTSeconds(jd),
|
||||
)
|
||||
geometry := solarEclipseBesselGeometryCacheEntry{
|
||||
moon: solarEclipseBesselMoonFromEquatorial(moon, axis),
|
||||
axis: axis,
|
||||
sun: sun,
|
||||
valid: true,
|
||||
}
|
||||
storeSolarEclipseBesselGeometry(solver.besselGeometryCache, key, geometry)
|
||||
return geometry.moon, geometry.axis, geometry.sun
|
||||
}
|
||||
|
||||
func (solver solarEclipseSolver) besselGeometryCandidateAt(jd float64) ([3]float64, solarEclipseAxis, [3]float64, bool) {
|
||||
key := math.Float64bits(jd)
|
||||
if entry, ok := solver.besselCandidateCache[key]; ok && entry.generation == deltaTGenerationValue() {
|
||||
return entry.moon, entry.axis, entry.sun, entry.valid
|
||||
}
|
||||
if solver.localEphemeris == nil {
|
||||
return [3]float64{}, solarEclipseAxis{}, [3]float64{}, false
|
||||
}
|
||||
sun, moon, ok := solver.localEphemeris.equatorialAt(jd)
|
||||
if !ok {
|
||||
return [3]float64{}, solarEclipseAxis{}, [3]float64{}, false
|
||||
}
|
||||
axis := solarEclipseBesselAxisFromEquatorialWithDeltaT(
|
||||
jd, sun, moon, solver.effectiveDeltaTSeconds(jd),
|
||||
)
|
||||
geometry := solarEclipseBesselGeometryCacheEntry{
|
||||
moon: solarEclipseBesselMoonFromEquatorial(moon, axis),
|
||||
axis: axis,
|
||||
sun: sun,
|
||||
valid: true,
|
||||
}
|
||||
storeSolarEclipseBesselGeometry(solver.besselCandidateCache, key, geometry)
|
||||
return geometry.moon, geometry.axis, geometry.sun, geometry.valid
|
||||
}
|
||||
|
||||
func storeSolarEclipseBesselGeometry(
|
||||
cache map[uint64]solarEclipseBesselGeometryCacheEntry,
|
||||
key uint64,
|
||||
entry solarEclipseBesselGeometryCacheEntry,
|
||||
) {
|
||||
if cache == nil {
|
||||
return
|
||||
}
|
||||
if _, exists := cache[key]; !exists && len(cache) >= solarEclipseBesselGeometryCacheMaximumEntries {
|
||||
for cachedKey := range cache {
|
||||
delete(cache, cachedKey)
|
||||
}
|
||||
}
|
||||
entry.generation = deltaTGenerationValue()
|
||||
cache[key] = entry
|
||||
}
|
||||
|
||||
func solarEclipseBesselMoonFromEquatorial(moon [3]float64, axis solarEclipseAxis) [3]float64 {
|
||||
rotated := solarEclipseRotateLLR(
|
||||
solarEclipseNormalizeSignedRadians(moon[0]-axis.rightAscension),
|
||||
moon[1],
|
||||
@@ -464,13 +781,16 @@ func (solver solarEclipseSolver) besselMoonAt(jd float64) [3]float64 {
|
||||
|
||||
func solarEclipseSunMoonEquatorial(jd float64) ([3]float64, [3]float64) {
|
||||
julianCentury := (jd - 2451545.0) / 36525.0
|
||||
obliquity := EclipticObliquity(jd, true) * rad
|
||||
nutationLongitude, nutationObliquity := Nutation2000B(jd)
|
||||
obliquity := (Obliquity1980(jd) + nutationObliquity) * rad
|
||||
|
||||
sunLongitude := HSunApparentLo(jd) * rad
|
||||
// Share the full-series distance and nutation for this single TT.
|
||||
sunDistanceAU := EarthAway(jd)
|
||||
sunLongitude := (HSunTrueLoN(jd, -1) + nutationLongitude - 20.49552/sunDistanceAU/3600) * rad
|
||||
sunLatitude := HSunTrueBo(jd) * rad
|
||||
sunDistance := EarthAway(jd) * solarEclipseAstronomicalUnitKM
|
||||
sunDistance := sunDistanceAU * solarEclipseAstronomicalUnitKM
|
||||
|
||||
moonLongitude := solarEclipseNormalizeRadians(HMoonApparentLo(jd)*rad + solarEclipseMoonLonAberrRad)
|
||||
moonLongitude := solarEclipseNormalizeRadians((HMoonTrueLoN(jd, -1)+nutationLongitude)*rad + solarEclipseMoonLonAberrRad)
|
||||
moonLatitude := HMoonTrueBo(jd)*rad + moonLatitudeAberrationRad(julianCentury)
|
||||
moonDistance := HMoonAway(jd)
|
||||
|
||||
@@ -483,6 +803,10 @@ func solarEclipseSunMoonEquatorial(jd float64) ([3]float64, [3]float64) {
|
||||
|
||||
func solarEclipseSunAltitudeAtGreatest(jd, lonDeg, latDeg, gst float64) float64 {
|
||||
sun, _ := solarEclipseSunMoonEquatorial(jd)
|
||||
return solarEclipseSunAltitudeFromEquatorial(sun, lonDeg, latDeg, gst)
|
||||
}
|
||||
|
||||
func solarEclipseSunAltitudeFromEquatorial(sun [3]float64, lonDeg, latDeg, gst float64) float64 {
|
||||
horizon := solarEclipseEquatorialToHorizontal(sun[0], sun[1], sun[2], lonDeg*rad, latDeg*rad, gst)
|
||||
return horizon[1]
|
||||
}
|
||||
|
||||
Reference in New Issue
Block a user