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
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package basic
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import "math"
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//下游研究需要，改成直接导出
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const (
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solarEclipseBesselianDefaultValidHours = 3.0
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solarEclipseBesselianSampleCount = 5
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// 恒星时每秒的角度增量，用于把 ΔT 换算成影轴时角的平移量。
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solarEclipseBesselianSiderealDegreesPerSecond = 15.041067 / 3600
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)
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// SolarEclipseBesselianPolynomial 是三次多项式系数，索引 n 对应 t 的 n 次幂，t 为自 T0 起算的 TT 小时数。
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// SolarEclipseBesselianPolynomial holds the cubic coefficients; index n multiplies t^n with t in TT hours from T0.
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type SolarEclipseBesselianPolynomial [4]float64
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// At 在自 T0 起 t 小时处求值 / evaluates the polynomial at t TT hours from T0.
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func (polynomial SolarEclipseBesselianPolynomial) At(hours float64) float64 {
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return polynomial[0] + hours*(polynomial[1]+hours*(polynomial[2]+hours*polynomial[3]))
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}
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// SolarEclipseBesselianElementsOptions 是贝塞尔根数表的生成选项 / options for a Besselian element table.
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type SolarEclipseBesselianElementsOptions struct {
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// Model 月亮半径模型；只有显式取 IAU Single-K 才切换，其余取值一律按 NASA bulletin Split-K。
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// Model is the lunar radius model; only an explicit IAU Single-K switches it.
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Model SolarEclipseRadiusModel
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// SunRadiusModel 太阳半径口径；零值为标准档。
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// SunRadiusModel is the solar radius convention; the zero value is the standard one.
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SunRadiusModel SolarEclipseSunRadiusModel
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// DeltaTSeconds 显式 ΔT（秒），非正值用进程级模型；它只改变地球自转相位，不改变任何 TT 时刻。
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// DeltaTSeconds is an explicit ΔT in seconds, non-positive uses the process model; it only sets Earth rotation.
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DeltaTSeconds float64
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// ReferenceJDE 多项式参考时刻 T0（TT 儒略日），非正值取食甚最近的整 TT 小时（四舍五入），与已发布根数表一致。
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// ReferenceJDE is the TT reference instant T0; non-positive uses the whole TT hour nearest to greatest eclipse.
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ReferenceJDE float64
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// ValidHours 多项式有效窗口半径（小时），非正值取 3；窗口内取 5 个等距时刻做三次最小二乘。
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// ValidHours is the half-width of the validity window in hours, non-positive uses 3.
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ValidHours float64
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}
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// SolarEclipseBesselianElementsResult 是一次日食的多项式贝塞尔根数及其口径 / polynomial Besselian elements and the conventions behind them.
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type SolarEclipseBesselianElementsResult struct {
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// T0JDE 多项式参考时刻（TT 儒略日），t = (jde - T0JDE) * 24。
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// T0JDE is the TT reference instant; t = (jde - T0JDE) * 24.
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T0JDE float64
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// ValidHours 有效窗口半径（小时），超出该窗口不应使用本多项式。
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// ValidHours is the half-width of the validity window in hours.
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ValidHours float64
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// X 与 Y 是月心在基本面内的坐标，单位地球赤道半径。
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// X and Y are the Moon's fundamental-plane coordinates in equatorial Earth radii.
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X, Y SolarEclipseBesselianPolynomial
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// D 是影轴赤纬，单位度。
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// D is the declination of the shadow axis in degrees.
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D SolarEclipseBesselianPolynomial
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// L1 与 L2 是基本面内的半影、本影半径，单位地球赤道半径；本影为负表示月心尚未越过本影锥顶点。
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// L1 and L2 are the penumbral and umbral radii in the fundamental plane, in equatorial Earth radii.
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L1, L2 SolarEclipseBesselianPolynomial
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// Mu 是影轴格林时角，单位度，窗口内连续、不折回 [0,360)。
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//
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// 口径与已发布根数表不同：本库的恒星时取自 UT = TT - ΔT，得到的是真实格林时角；已发布表改用
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// T0 本身的恒星时（不含 ΔT 自转），两者相差 ΔT × 15.041067/3600 度。要对表先用
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// SolarEclipseBesselianMuForPublishedTable 换算。
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// Mu is the Greenwich hour angle of the shadow axis in degrees, continuous and not folded into [0,360).
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Mu SolarEclipseBesselianPolynomial
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// TanF1 与 TanF2 是半影、本影锥半顶角正切，本次日食内为常数。
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// TanF1 and TanF2 are the penumbral and umbral cone half-angle tangents, constant over the eclipse.
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TanF1, TanF2 float64
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// Gamma 是食甚时刻影轴到地心的距离，单位地球赤道半径。
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// Gamma is the shadow-axis distance from the Earth's centre at greatest eclipse, in equatorial Earth radii.
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Gamma float64
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// Magnitude 是食甚时刻的全局食分。
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// Magnitude is the global eclipse magnitude at greatest eclipse.
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Magnitude float64
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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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PenumbralK float64
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UmbralK float64
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DeltaTSeconds float64
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}
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// SolarEclipseBesselianMuForPublishedTable 把本库的 Mu 换算成与已发布根数表直接可比的取值。
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// 已发布表用 T0 本身的恒星时，本库用 UT = TT - ΔT，两者只差一个常数，因此只有常数项平移。
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// SolarEclipseBesselianMuForPublishedTable shifts Mu onto the argument used by published element tables.
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func SolarEclipseBesselianMuForPublishedTable(
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mu SolarEclipseBesselianPolynomial, deltaTSeconds float64,
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) SolarEclipseBesselianPolynomial {
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shift := deltaTSeconds * solarEclipseBesselianSiderealDegreesPerSecond
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return SolarEclipseBesselianPolynomial{mu[0] + shift, mu[1], mu[2], mu[3]}
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}
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// SolarEclipseBesselianElements 计算给定近朔时刻附近一次日食的多项式贝塞尔根数，窗口内无日食时返回 false。
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// Polynomial Besselian elements for the solar eclipse near the given new-moon instant; false when there is none.
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func SolarEclipseBesselianElements(
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seedJDE float64, options SolarEclipseBesselianElementsOptions,
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) (SolarEclipseBesselianElementsResult, bool) {
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options.Model = normalizeSolarEclipseRadiusModel(options.Model)
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options.SunRadiusModel = normalizeSolarEclipseSunRadiusModel(options.SunRadiusModel)
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validHours := options.ValidHours
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if !(validHours > 0) {
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validHours = solarEclipseBesselianDefaultValidHours
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}
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solver := newSolarEclipseSolverWithOptions(CalcMoonSHByJDE(seedJDE, 0), SolarEclipseOptions{
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RadiusModel: options.Model,
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SunRadiusModel: options.SunRadiusModel,
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}).
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withDeltaTSeconds(options.DeltaTSeconds)
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feature := solver.feature()
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if feature.typeCode == "N" {
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return SolarEclipseBesselianElementsResult{}, false
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}
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t0 := options.ReferenceJDE
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if !(t0 > 0) {
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// 已发布表按最近整小时取 T0（食甚 02:36 TDT 的表 T0 是 03:00），不是取整点下界。
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t0 = math.Round(feature.greatestEclipseJDE*24) / 24
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}
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step := 2 * validHours / float64(solarEclipseBesselianSampleCount-1)
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times := make([]float64, solarEclipseBesselianSampleCount)
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columns := [6][]float64{}
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for index := range columns {
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columns[index] = make([]float64, solarEclipseBesselianSampleCount)
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}
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for index := range times {
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hours := -validHours + step*float64(index)
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times[index] = hours
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point := solver.besselianElementsAt(t0 + hours/24)
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columns[0][index] = point.x
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columns[1][index] = point.y
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columns[2][index] = point.d
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columns[3][index] = point.l1
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columns[4][index] = point.l2
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columns[5][index] = point.mu
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}
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// μ 每窗口跨越的角量远小于 180°，可以先展开成连续序列再归一到 [0,360)。
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columns[5] = solarEclipseUnwrapDegrees(columns[5], solarEclipseBesselianSampleCount/2)
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return SolarEclipseBesselianElementsResult{
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T0JDE: t0,
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ValidHours: validHours,
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X: solarEclipseFitCubic(times, columns[0]),
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Y: solarEclipseFitCubic(times, columns[1]),
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D: solarEclipseFitCubic(times, columns[2]),
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L1: solarEclipseFitCubic(times, columns[3]),
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L2: solarEclipseFitCubic(times, columns[4]),
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Mu: solarEclipseFitCubic(times, columns[5]),
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TanF1: solver.penumbraConeTangent,
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TanF2: solver.umbraConeTangent,
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Gamma: feature.gamma,
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Magnitude: feature.magnitude,
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Model: options.Model,
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SunRadiusModel: options.SunRadiusModel,
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PenumbralK: solver.params.penumbralK,
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UmbralK: solver.params.umbralK,
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DeltaTSeconds: solver.effectiveDeltaTSeconds(t0),
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}, true
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}
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// solarEclipseBesselianPoint 是单一 TT 时刻的经典口径贝塞尔根数。
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type solarEclipseBesselianPoint struct {
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x, y, z, d, mu, l1, l2 float64
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}
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// besselianElementsAt 按经典口径取该时刻的根数：d 为影轴赤纬，μ 为真实格林时角，
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// L1/L2 用含 1/cos f 的 ES 形式，且本影取负号口径。
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func (solver solarEclipseSolver) besselianElementsAt(jde float64) solarEclipseBesselianPoint {
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moon, axis, _ := solver.besselGeometryAt(jde)
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penumbraHalfAngle := math.Atan(solver.penumbraConeTangent)
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umbraHalfAngle := math.Atan(solver.umbraConeTangent)
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return solarEclipseBesselianPoint{
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x: moon[0],
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y: moon[1],
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z: moon[2],
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d: (math.Pi/2 - axis.tilt) / rad,
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mu: (axis.gst - (axis.rightAscension - math.Pi/2)) / rad,
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l1: moon[2]*solver.penumbraConeTangent + solver.params.penumbralK/math.Cos(penumbraHalfAngle),
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l2: moon[2]*solver.umbraConeTangent - solver.params.umbralK/math.Cos(umbraHalfAngle),
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}
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}
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// solarEclipseUnwrapDegrees 把按时间升序的角量展开成连续序列，并把 reference 号样本归入 [0,360)。
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func solarEclipseUnwrapDegrees(values []float64, reference int) []float64 {
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unwrapped := make([]float64, len(values))
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copy(unwrapped, values)
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for index := 1; index < len(unwrapped); index++ {
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for unwrapped[index]-unwrapped[index-1] > 180 {
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unwrapped[index] -= 360
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}
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for unwrapped[index]-unwrapped[index-1] < -180 {
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unwrapped[index] += 360
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}
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}
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if reference >= 0 && reference < len(unwrapped) {
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shift := 360 * math.Floor(unwrapped[reference]/360)
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for index := range unwrapped {
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unwrapped[index] -= shift
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}
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}
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return unwrapped
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}
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// solarEclipseFitCubic 用样本做三次最小二乘拟合，样本少于 4 个时返回零值。
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func solarEclipseFitCubic(times, values []float64) SolarEclipseBesselianPolynomial {
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if len(times) < 4 || len(times) != len(values) {
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return SolarEclipseBesselianPolynomial{}
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}
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var normal [4][5]float64
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for index := range times {
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powers := [7]float64{1}
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for n := 1; n < len(powers); n++ {
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powers[n] = powers[n-1] * times[index]
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}
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for row := range normal {
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for column := range normal[row][:4] {
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normal[row][column] += powers[row+column]
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}
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normal[row][4] += powers[row] * values[index]
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}
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}
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for column := range normal {
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pivot := column
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for row := column + 1; row < len(normal); row++ {
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if math.Abs(normal[row][column]) > math.Abs(normal[pivot][column]) {
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pivot = row
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}
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}
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normal[column], normal[pivot] = normal[pivot], normal[column]
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if normal[column][column] == 0 {
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return SolarEclipseBesselianPolynomial{}
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}
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for row := range normal {
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if row == column {
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continue
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}
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factor := normal[row][column] / normal[column][column]
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for c := column; c < len(normal[row]); c++ {
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normal[row][c] -= factor * normal[column][c]
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}
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}
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}
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var polynomial SolarEclipseBesselianPolynomial
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for n := range polynomial {
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polynomial[n] = normal[n][4] / normal[n][n]
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}
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return polynomial
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}
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