feat: 完善时标与天象几何计算并扩展输出接口
- 新增时标、ΔT 模型、质心时间与 UT1 支持 - 改进日月食、月掩、行星事件及路径边界计算 - 完善恒星三维自行与动态距离传播 - 扩展 SVG、GeoJSON、KML 输出与底层距离换算工具 - 整理中英文手册、示例资源及回归测试
This commit is contained in:
+177
-93
@@ -12,6 +12,24 @@ const (
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SolarEclipseModelNASABulletinSplitK SolarEclipseRadiusModel = "nasa_bulletin_split_k"
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)
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// SolarEclipseSunRadiusModel 日食几何的太阳半径口径 / solar radius convention for eclipse geometry.
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type SolarEclipseSunRadiusModel string
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const (
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// SolarEclipseSunRadiusStandard 标准档，1 AU 处 959.639″，复现已发布星历表与目录 / standard.
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SolarEclipseSunRadiusStandard SolarEclipseSunRadiusModel = "standard"
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// SolarEclipseSunRadiusMeasured 边缘档，1 AU 处 959.95″：全食带每侧约窄 0.6 千米、中心食时长约短 1.5 秒 / measured.
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SolarEclipseSunRadiusMeasured SolarEclipseSunRadiusModel = "measured"
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)
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// SolarEclipseOptions 日食计算的半径口径 / radius conventions for a solar eclipse computation.
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type SolarEclipseOptions struct {
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// RadiusModel 月亮平均半径 k 的口径，零值为 NASA bulletin Split-K / lunar radius model.
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RadiusModel SolarEclipseRadiusModel
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// SunRadiusModel 太阳半径口径，零值为标准档 / solar radius convention.
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SunRadiusModel SolarEclipseSunRadiusModel
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}
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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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@@ -45,9 +63,12 @@ const (
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// 所有时刻字段都使用力学时儒略日（JDE, TT）。
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// 输入 seedJDE 只需要落在目标朔月附近，允许相差数天。
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type SolarEclipseResult struct {
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Model SolarEclipseRadiusModel
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Type SolarEclipseType
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Centrality SolarEclipseCentrality
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// 下列字段是决定上述数值的口径，随结果一起保留。
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// The fields below are the conventions that fix the numbers above.
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Model SolarEclipseRadiusModel
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SunRadiusModel SolarEclipseSunRadiusModel
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Type SolarEclipseType
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Centrality SolarEclipseCentrality
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// GreatestEclipse 是全局“影轴最接近地心”的时刻。
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GreatestEclipse float64
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@@ -68,8 +89,17 @@ type SolarEclipseResult struct {
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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 是食甚处中心食带宽度；非中心食为 0；单侧极限（中心带仅触及地球边缘）时该解析式
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// 失效并一并置 0，此时 PathWidthDefined 为 false，NASA 目录该栏印 '-'。
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// PathWidthKM is the central path width at greatest eclipse, 0 for a non-central
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// event, and 0 when the analytic formula fails at a single-sided limit where the
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// band only grazes the Earth's limb; PathWidthDefined is false there and
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// catalogues print '-' for this column.
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PathWidthKM float64
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// PathWidthDefined 表示上面的带宽是否有定义：只有南北两限都存在（central_two_limits）时才为 true。
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// PathWidthDefined reports whether the width above is defined: it is true only
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// when both band limits exist, that is for central_two_limits.
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PathWidthDefined bool
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// GreatestLongitude / GreatestLatitude 是日食食甚点地理坐标，东经为正，西经为负。
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GreatestLongitude float64
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@@ -83,8 +113,9 @@ type SolarEclipseResult struct {
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}
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type solarEclipseModelParameters struct {
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penumbralK float64
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umbralK float64
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penumbralK float64
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umbralK float64
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sunRadiusRatio float64
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}
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type solarEclipseShadowRadii struct {
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@@ -101,9 +132,10 @@ type solarEclipseAxis struct {
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}
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type solarEclipseSolver struct {
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newMoonJDE float64
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model SolarEclipseRadiusModel
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params solarEclipseModelParameters
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newMoonJDE float64
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model SolarEclipseRadiusModel
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sunRadiusModel SolarEclipseSunRadiusModel
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params solarEclipseModelParameters
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localStateContextCache map[uint64]localSolarEclipseStateContext
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localEphemeris *solarEclipseLocalEphemeris
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@@ -170,17 +202,23 @@ const (
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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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// 标准档与边缘档在 1 AU 处的太阳视半径（角秒），日食与月食几何共用这一组常量。
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eclipseSunRadiusStandardArcsec = 959.639
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eclipseSunRadiusMeasuredArcsec = 959.95
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// 标准档太阳半径是地球赤道半径的 109.1222 倍，与上面的标准档视半径等价；边缘档按视半径比例放大。
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solarEclipseSunRadiusRatioStandard = 109.1222
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solarEclipseSunRadiusRatioMeasured = solarEclipseSunRadiusRatioStandard * eclipseSunRadiusMeasuredArcsec / eclipseSunRadiusStandardArcsec
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// Split-K：半影（偏食）0.2724880、本影与反本影 0.2722810；IAU Single-K 全部使用 0.2725076。
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solarEclipsePenumbralK = 0.2724880
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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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solarEclipseIAUSingleRadiusK = 0.2725076
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// SolarEclipsePenumbralK / SolarEclipseUmbralK 是 Split-K 的半影与本影月地半径比 k1/k2，
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// SolarEclipseIAUSingleRadiusK 是 IAU Single-K 的单一值。
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// SolarEclipsePenumbralK / SolarEclipseUmbralK are the split-k lunar-to-terrestrial radius ratios,
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// SolarEclipseIAUSingleRadiusK the IAU single value.
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SolarEclipsePenumbralK = solarEclipsePenumbralK
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SolarEclipseUmbralK = solarEclipseUmbralK
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SolarEclipseIAUSingleRadiusK = solarEclipseIAUSingleRadiusK
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solarEclipseNodeCount = 7
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solarEclipseNodeStepDays = 0.04
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@@ -196,11 +234,42 @@ const (
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var solarEclipseArcsecPerRadian = 180.0 * 3600.0 / math.Pi
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// SolarEclipse 计算给定近朔时刻附近的一次全局日食，默认使用 NASABulletin Split-K 模型。
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func normalizeSolarEclipseRadiusModel(model SolarEclipseRadiusModel) SolarEclipseRadiusModel {
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if model == SolarEclipseModelIAUSingleK {
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return SolarEclipseModelIAUSingleK
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}
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return SolarEclipseModelNASABulletinSplitK
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}
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func normalizeSolarEclipseSunRadiusModel(model SolarEclipseSunRadiusModel) SolarEclipseSunRadiusModel {
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if model == SolarEclipseSunRadiusMeasured {
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return SolarEclipseSunRadiusMeasured
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}
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return SolarEclipseSunRadiusStandard
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}
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func solarEclipseSunRadiusRatio(model SolarEclipseSunRadiusModel) float64 {
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if normalizeSolarEclipseSunRadiusModel(model) == SolarEclipseSunRadiusMeasured {
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return solarEclipseSunRadiusRatioMeasured
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}
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return solarEclipseSunRadiusRatioStandard
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}
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// SolarEclipseSunSemidiameter 指定太阳半径口径下的视半径，单位角秒 / apparent solar semidiameter in arcseconds under a given eclipse sun radius convention.
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func SolarEclipseSunSemidiameter(jde float64, model SolarEclipseSunRadiusModel) float64 {
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return angularSemidiameterFromAU(solarEclipseSunRadiusRatio(model)*solarEclipseEarthEquatorialRadiusKM, EarthAwayN(jde, -1))
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}
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// SolarEclipse 计算给定近朔时刻附近的一次全局日食，默认使用 NASABulletin Split-K 模型与标准太阳半径。
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func SolarEclipse(seedJDE float64) SolarEclipseResult {
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return SolarEclipseNASABulletinSplitK(seedJDE)
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}
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// SolarEclipseWithOptions 计算给定近朔时刻附近的一次全局日食，半径口径由 options 指定 / computes one global solar eclipse with the given radius conventions.
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func SolarEclipseWithOptions(seedJDE float64, options SolarEclipseOptions) SolarEclipseResult {
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return solarEclipseWithDeltaT(seedJDE, options, 0)
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}
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// SolarEclipseIAUSingleK 计算给定近朔时刻附近的一次全局日食，使用 IAU Single-K 模型。
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func SolarEclipseIAUSingleK(seedJDE float64) SolarEclipseResult {
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return solarEclipse(seedJDE, SolarEclipseModelIAUSingleK)
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@@ -212,16 +281,16 @@ 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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return solarEclipseWithDeltaT(seedJDE, SolarEclipseOptions{RadiusModel: 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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options SolarEclipseOptions,
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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).withDeltaTSeconds(deltaTSeconds)
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solver := newSolarEclipseSolverWithOptions(newMoonJDE, options).withDeltaTSeconds(deltaTSeconds)
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return solver.eclipseResult()
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}
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@@ -231,6 +300,7 @@ func (solver solarEclipseSolver) eclipseResult() SolarEclipseResult {
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result := SolarEclipseResult{
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Model: model,
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SunRadiusModel: solver.sunRadiusModel,
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Type: SolarEclipseNone,
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Centrality: SolarEclipseNonCentral,
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GreatestEclipse: feature.greatestEclipseJDE,
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@@ -252,12 +322,12 @@ func (solver solarEclipseSolver) eclipseResult() SolarEclipseResult {
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result.Type = SolarEclipseHybrid
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}
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switch feature.typeCode {
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case "A1", "T1":
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result.Centrality = SolarEclipseCentralOneLimit
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case "A", "T", "H", "H2", "H3":
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if solarEclipseTwoLimitsTypeCode(feature.typeCode) {
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result.Centrality = SolarEclipseCentralTwoLimits
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} else if feature.typeCode == "A1" || feature.typeCode == "T1" {
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result.Centrality = SolarEclipseCentralOneLimit
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}
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result.PathWidthDefined = result.Centrality == SolarEclipseCentralTwoLimits
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if result.Type != SolarEclipseNone {
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result.HasPartial = true
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@@ -299,13 +369,13 @@ func (solver solarEclipseSolver) greatestCentralDuration(result SolarEclipseResu
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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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umbralK: solarEclipsePenumbralK,
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}
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if model == SolarEclipseModelNASABulletinSplitK {
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params.umbralK = solarEclipseUmbralK
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}
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return newSolarEclipseSolverWithOptions(newMoonJDE, SolarEclipseOptions{RadiusModel: model})
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}
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func newSolarEclipseSolverWithOptions(newMoonJDE float64, options SolarEclipseOptions) solarEclipseSolver {
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options.RadiusModel = normalizeSolarEclipseRadiusModel(options.RadiusModel)
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options.SunRadiusModel = normalizeSolarEclipseSunRadiusModel(options.SunRadiusModel)
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params := solarEclipseModelParams(options.RadiusModel, options.SunRadiusModel)
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firstNodeJDE := newMoonJDE + (0-float64(solarEclipseNodeCount)/2+0.5)*solarEclipseNodeStepDays
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lastNodeJDE := newMoonJDE + (float64(solarEclipseNodeCount-1)-float64(solarEclipseNodeCount)/2+0.5)*solarEclipseNodeStepDays
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@@ -316,15 +386,16 @@ func newSolarEclipseSolver(newMoonJDE float64, model SolarEclipseRadiusModel) so
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return solarEclipseSolver{
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newMoonJDE: newMoonJDE,
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model: model,
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model: options.RadiusModel,
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sunRadiusModel: options.SunRadiusModel,
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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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penumbraConeTangent: (params.sunRadiusRatio + params.penumbralK) / meanSunMoonDistance,
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umbraConeTangent: (params.sunRadiusRatio - params.umbralK) / meanSunMoonDistance,
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}
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}
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@@ -342,20 +413,22 @@ func (solver solarEclipseSolver) withDeltaTSeconds(deltaTSeconds float64) solarE
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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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// 未覆盖时用真 TT−UT1（观测表/外推），不能回退到混入 UTC 的进程级 DeltaT，
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// 否则恒星时相位会少掉 DUT1，站心与影轴两条路径就不一致。
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func (solver solarEclipseSolver) effectiveDeltaTSeconds(jde float64) float64 {
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if math.IsNaN(solver.deltaTSeconds) {
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return DeltaT(jd, true)
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return ut1ToTTOffsetSeconds(ttToUT1JDE(jde))
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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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func (solver solarEclipseSolver) siderealTimeAt(jde float64) float64 {
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ut1JDE := TT2UT1(jde)
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if !math.IsNaN(solver.deltaTSeconds) {
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utJDE = jd - solver.deltaTSeconds/86400
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ut1JDE = jde - solver.deltaTSeconds/86400
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}
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return ApparentSiderealTime(utJDE) * 15 * rad
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return ApparentSiderealTime(ut1JDE) * 15 * rad
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}
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// withLocalEphemeris prepares the immutable event-local interpolator used by
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@@ -368,14 +441,23 @@ func (solver solarEclipseSolver) withLocalEphemeris() solarEclipseSolver {
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return solver
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}
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// solarEclipseTwoLimitsTypeCode 报告该类型码的南北两限是否都存在，带宽解析式只在这一类中心食上有定义。
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func solarEclipseTwoLimitsTypeCode(typeCode string) bool {
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switch typeCode {
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case "A", "T", "H", "H2", "H3":
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return true
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}
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return false
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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 := 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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jde := solver.newMoonJDE
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before := candidateSolver.besselMoonCandidateAt(jde - finiteDifferenceStep)
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center := candidateSolver.besselMoonCandidateAt(jde)
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after := candidateSolver.besselMoonCandidateAt(jde + 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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@@ -384,7 +466,7 @@ func (solver solarEclipseSolver) feature() solarEclipseFeature {
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speedSquared := speed * speed
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t0 := -(center[0]*vx + center[1]*vy) / speedSquared
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greatestEclipseJDE := jd + t0
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greatestEclipseJDE := jde + 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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@@ -476,7 +558,9 @@ func (solver solarEclipseSolver) feature() solarEclipseFeature {
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}
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}
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if typeCode != "N" && typeCode != "P" {
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// 单侧极限（A1/T1）只有一侧限界，非中心中心食（A0/T0）连限界都没有：解析式 2r/|sin h|
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// 在 h→0 时发散，两类事件该栏都无定义，与中心线逐点宽度一起置 0。
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if solarEclipseTwoLimitsTypeCode(typeCode) {
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sunAltitude := solarEclipseSunAltitudeAtGreatest(greatestEclipseJDE, greatestLongitude, greatestLatitude, axis.gst)
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if math.Abs(math.Sin(sunAltitude)) > 1e-12 {
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pathWidthKM = math.Abs(2*greatestRadii.umbraRadius*solarEclipseEarthEquatorialRadiusKM) / math.Abs(math.Sin(sunAltitude))
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@@ -495,13 +579,13 @@ func (solver solarEclipseSolver) feature() solarEclipseFeature {
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}
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if typeCode != "N" {
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_, _, feature.partialBeginJDE, _ = solver.quickContactAt(partialStartParam+jd, vx, vy, true)
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_, _, feature.partialEndJDE, _ = solver.quickContactAt(partialEndParam+jd, vx, vy, true)
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_, _, feature.partialBeginJDE, _ = solver.quickContactAt(partialStartParam+jde, vx, vy, true)
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_, _, feature.partialEndJDE, _ = solver.quickContactAt(partialEndParam+jde, vx, vy, true)
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}
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|
||||
if axisIntersection.valid && typeCode != "N" && typeCode != "P" {
|
||||
_, _, feature.centralBeginJDE, _ = solver.quickContactAt(centralStartParam+jd, vx, vy, false)
|
||||
_, _, feature.centralEndJDE, _ = solver.quickContactAt(centralEndParam+jd, vx, vy, false)
|
||||
_, _, feature.centralBeginJDE, _ = solver.quickContactAt(centralStartParam+jde, vx, vy, false)
|
||||
_, _, feature.centralEndJDE, _ = solver.quickContactAt(centralEndParam+jde, vx, vy, false)
|
||||
if refined, ok := solver.centralAxisContactJDE(feature.centralBeginJDE, greatestEclipseJDE, -1); ok {
|
||||
feature.centralBeginJDE = refined
|
||||
}
|
||||
@@ -569,8 +653,8 @@ func (solver solarEclipseSolver) centralAxisContactJDE(
|
||||
return (insideJDE + outsideJDE) / 2, true
|
||||
}
|
||||
|
||||
func (solver solarEclipseSolver) centralAxisEarthDiscriminant(jd float64) float64 {
|
||||
moon, axis, _ := solver.besselGeometryAt(jd)
|
||||
func (solver solarEclipseSolver) centralAxisEarthDiscriminant(jde float64) float64 {
|
||||
moon, axis, _ := solver.besselGeometryAt(jde)
|
||||
return solarEclipseLineEllipsoidDiscriminant(
|
||||
moon[0], moon[1], 2,
|
||||
moon[0], moon[1], 0,
|
||||
@@ -578,8 +662,8 @@ func (solver solarEclipseSolver) centralAxisEarthDiscriminant(jd float64) float6
|
||||
)
|
||||
}
|
||||
|
||||
func (solver solarEclipseSolver) centralAxisContactPointAt(jd float64) (SolarEclipsePathPoint, bool) {
|
||||
moon, axis, _ := solver.besselGeometryAt(jd)
|
||||
func (solver solarEclipseSolver) centralAxisContactPointAt(jde float64) (SolarEclipsePathPoint, bool) {
|
||||
moon, axis, _ := solver.besselGeometryAt(jde)
|
||||
cosTilt, sinTilt := math.Cos(axis.tilt), math.Sin(axis.tilt)
|
||||
x1 := moon[0]
|
||||
y1 := cosTilt*moon[1] - 2*sinTilt
|
||||
@@ -606,15 +690,15 @@ func (solver solarEclipseSolver) centralAxisContactPointAt(jd float64) (SolarEcl
|
||||
return SolarEclipsePathPoint{}, false
|
||||
}
|
||||
return SolarEclipsePathPoint{
|
||||
JDE: jd,
|
||||
JDE: jde,
|
||||
Longitude: longitude,
|
||||
Latitude: latitude,
|
||||
SunAltitude: solarEclipseSunAltitudeAtGreatest(jd, longitude, latitude, axis.gst) / rad,
|
||||
SunAltitude: solarEclipseSunAltitudeAtGreatest(jde, longitude, latitude, axis.gst) / rad,
|
||||
}, true
|
||||
}
|
||||
|
||||
func (solver solarEclipseSolver) quickContactAt(jd, dx, dy float64, penumbral bool) (float64, float64, float64, bool) {
|
||||
moon := solver.besselMoonAt(jd)
|
||||
func (solver solarEclipseSolver) quickContactAt(jde, dx, dy float64, penumbral bool) (float64, float64, float64, bool) {
|
||||
moon := solver.besselMoonAt(jde)
|
||||
radii := solver.shadowRadiiAt(moon[2])
|
||||
radius := 0.0
|
||||
if penumbral {
|
||||
@@ -635,15 +719,15 @@ func (solver solarEclipseSolver) quickContactAt(jd, dx, dy float64, penumbral bo
|
||||
correction := (effectiveRadius*effectiveRadius - moon[0]*moon[0] - moon[1]*moon[1]) / (2 * velocityProjection)
|
||||
x := moon[0] + correction*dx
|
||||
y := moon[1] + correction*dy
|
||||
jd += correction
|
||||
jde += correction
|
||||
|
||||
curvature := (1 - solarEclipseEarthPolarRatioSquared) * radius * x * y / math.Pow(effectiveRadius, 3)
|
||||
x += curvature * y
|
||||
y -= curvature * x
|
||||
|
||||
axis := solver.besselAxisAt(jd)
|
||||
axis := solver.besselAxisAt(jde)
|
||||
longitude, latitude, ok := solarEclipseBesselXYToGeodetic(x/effectiveRadius, y/effectiveRadius, axis, true)
|
||||
return longitude, latitude, jd, ok
|
||||
return longitude, latitude, jde, ok
|
||||
}
|
||||
|
||||
func (solver solarEclipseSolver) shadowRadiiAt(moonBesselZ float64) solarEclipseShadowRadii {
|
||||
@@ -651,14 +735,14 @@ func (solver solarEclipseSolver) shadowRadiiAt(moonBesselZ float64) solarEclipse
|
||||
penumbraRadius: solver.params.penumbralK + solver.penumbraConeTangent*moonBesselZ,
|
||||
umbraRadius: solver.params.umbralK - solver.umbraConeTangent*moonBesselZ,
|
||||
absUmbraRadius: math.Abs(solver.params.umbralK - solver.umbraConeTangent*moonBesselZ),
|
||||
magnitude: solver.params.umbralK / moonBesselZ / solarEclipseSolarRadiusRatio * (solver.meanSunMoonDistance + moonBesselZ),
|
||||
magnitude: solver.params.umbralK / moonBesselZ / solver.params.sunRadiusRatio * (solver.meanSunMoonDistance + moonBesselZ),
|
||||
}
|
||||
}
|
||||
|
||||
func (solver solarEclipseSolver) besselAxisAt(jd float64) solarEclipseAxis {
|
||||
sun, moon := solarEclipseSunMoonEquatorial(jd)
|
||||
func (solver solarEclipseSolver) besselAxisAt(jde float64) solarEclipseAxis {
|
||||
sun, moon := solarEclipseSunMoonEquatorial(jde)
|
||||
return solarEclipseBesselAxisFromEquatorialWithDeltaT(
|
||||
jd, sun, moon, solver.effectiveDeltaTSeconds(jd),
|
||||
jde, sun, moon, solver.effectiveDeltaTSeconds(jde),
|
||||
)
|
||||
}
|
||||
|
||||
@@ -686,30 +770,30 @@ func solarEclipseBesselAxisFromEquatorialWithDeltaT(
|
||||
}
|
||||
}
|
||||
|
||||
func (solver solarEclipseSolver) besselMoonAt(jd float64) [3]float64 {
|
||||
moon, _, _ := solver.besselGeometryAt(jd)
|
||||
func (solver solarEclipseSolver) besselMoonAt(jde float64) [3]float64 {
|
||||
moon, _, _ := solver.besselGeometryAt(jde)
|
||||
return moon
|
||||
}
|
||||
|
||||
func (solver solarEclipseSolver) besselMoonCandidateAt(jd float64) [3]float64 {
|
||||
moon, _, _, ok := solver.besselGeometryCandidateAt(jd)
|
||||
func (solver solarEclipseSolver) besselMoonCandidateAt(jde float64) [3]float64 {
|
||||
moon, _, _, ok := solver.besselGeometryCandidateAt(jde)
|
||||
if !ok {
|
||||
return solver.besselMoonAt(jd)
|
||||
return solver.besselMoonAt(jde)
|
||||
}
|
||||
return moon
|
||||
}
|
||||
|
||||
func (solver solarEclipseSolver) besselGeometryAt(jd float64) ([3]float64, solarEclipseAxis, [3]float64) {
|
||||
key := math.Float64bits(jd)
|
||||
func (solver solarEclipseSolver) besselGeometryAt(jde float64) ([3]float64, solarEclipseAxis, [3]float64) {
|
||||
key := math.Float64bits(jde)
|
||||
// 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)
|
||||
sun, moon := solarEclipseSunMoonEquatorial(jde)
|
||||
axis := solarEclipseBesselAxisFromEquatorialWithDeltaT(
|
||||
jd, sun, moon, solver.effectiveDeltaTSeconds(jd),
|
||||
jde, sun, moon, solver.effectiveDeltaTSeconds(jde),
|
||||
)
|
||||
geometry := solarEclipseBesselGeometryCacheEntry{
|
||||
moon: solarEclipseBesselMoonFromEquatorial(moon, axis),
|
||||
@@ -721,20 +805,20 @@ func (solver solarEclipseSolver) besselGeometryAt(jd float64) ([3]float64, solar
|
||||
return geometry.moon, geometry.axis, geometry.sun
|
||||
}
|
||||
|
||||
func (solver solarEclipseSolver) besselGeometryCandidateAt(jd float64) ([3]float64, solarEclipseAxis, [3]float64, bool) {
|
||||
key := math.Float64bits(jd)
|
||||
func (solver solarEclipseSolver) besselGeometryCandidateAt(jde float64) ([3]float64, solarEclipseAxis, [3]float64, bool) {
|
||||
key := math.Float64bits(jde)
|
||||
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)
|
||||
sun, moon, ok := solver.localEphemeris.equatorialAt(jde)
|
||||
if !ok {
|
||||
return [3]float64{}, solarEclipseAxis{}, [3]float64{}, false
|
||||
}
|
||||
axis := solarEclipseBesselAxisFromEquatorialWithDeltaT(
|
||||
jd, sun, moon, solver.effectiveDeltaTSeconds(jd),
|
||||
jde, sun, moon, solver.effectiveDeltaTSeconds(jde),
|
||||
)
|
||||
geometry := solarEclipseBesselGeometryCacheEntry{
|
||||
moon: solarEclipseBesselMoonFromEquatorial(moon, axis),
|
||||
@@ -779,20 +863,20 @@ func solarEclipseBesselMoonFromEquatorial(moon [3]float64, axis solarEclipseAxis
|
||||
}
|
||||
}
|
||||
|
||||
func solarEclipseSunMoonEquatorial(jd float64) ([3]float64, [3]float64) {
|
||||
julianCentury := (jd - 2451545.0) / 36525.0
|
||||
nutationLongitude, nutationObliquity := Nutation2000B(jd)
|
||||
obliquity := (Obliquity1980(jd) + nutationObliquity) * rad
|
||||
func solarEclipseSunMoonEquatorial(jde float64) ([3]float64, [3]float64) {
|
||||
julianCentury := (jde - 2451545.0) / 36525.0
|
||||
nutationLongitude, nutationObliquity := Nutation2000B(jde)
|
||||
obliquity := (Obliquity1980(jde) + nutationObliquity) * 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
|
||||
sunDistanceAU := EarthAway(jde)
|
||||
sunLongitude := (HSunTrueLoN(jde, -1) + nutationLongitude - 20.49552/sunDistanceAU/3600) * rad
|
||||
sunLatitude := HSunTrueBo(jde) * rad
|
||||
sunDistance := sunDistanceAU * solarEclipseAstronomicalUnitKM
|
||||
|
||||
moonLongitude := solarEclipseNormalizeRadians((HMoonTrueLoN(jd, -1)+nutationLongitude)*rad + solarEclipseMoonLonAberrRad)
|
||||
moonLatitude := HMoonTrueBo(jd)*rad + moonLatitudeAberrationRad(julianCentury)
|
||||
moonDistance := HMoonAway(jd)
|
||||
moonLongitude := solarEclipseNormalizeRadians((HMoonTrueLoN(jde, -1)+nutationLongitude)*rad + solarEclipseMoonLonAberrRad)
|
||||
moonLatitude := HMoonTrueBo(jde)*rad + moonLatitudeAberrationRad(julianCentury)
|
||||
moonDistance := HMoonAway(jde)
|
||||
|
||||
sunEquatorial := solarEclipseRotateLLR(sunLongitude, sunLatitude, sunDistance, obliquity)
|
||||
moonEquatorial := solarEclipseRotateLLR(moonLongitude, moonLatitude, moonDistance, obliquity)
|
||||
@@ -801,8 +885,8 @@ func solarEclipseSunMoonEquatorial(jd float64) ([3]float64, [3]float64) {
|
||||
[3]float64{moonEquatorial[0], moonEquatorial[1], moonEquatorial[2]}
|
||||
}
|
||||
|
||||
func solarEclipseSunAltitudeAtGreatest(jd, lonDeg, latDeg, gst float64) float64 {
|
||||
sun, _ := solarEclipseSunMoonEquatorial(jd)
|
||||
func solarEclipseSunAltitudeAtGreatest(jde, lonDeg, latDeg, gst float64) float64 {
|
||||
sun, _ := solarEclipseSunMoonEquatorial(jde)
|
||||
return solarEclipseSunAltitudeFromEquatorial(sun, lonDeg, latDeg, gst)
|
||||
}
|
||||
|
||||
|
||||
Reference in New Issue
Block a user