meepmeep.numba3d.emission_phase_curve_cd

meepmeep.numba3d.emission_phase_curve_cd(time: float | ndarray[tuple[Any, ...], dtype[_ScalarT]], k: float, fratio: float, offset: float, c: ndarray[tuple[Any, ...], dtype[_ScalarT]], dc: ndarray[tuple[Any, ...], dtype[_ScalarT]])

Evaluate the cosine emission phase-curve flux and its parameter derivatives at an expansion-point-centered time.

Derivative-returning counterpart of emission.emission_phase_curve_c: forms \(F = k^2 f_\mathrm{ratio} (1 + \cos\delta\,c_z + \sin\delta\,s)/2\) and propagates the chain rule through the position and velocity (the signed in-plane component depends on the orbital normal \(w = r\times v\)).

Accepts a scalar time or a 1-D array of times and dispatches to the appropriate kernel at compile time (inside @njit) or at call time (pure Python).

Parameters:

timefloat or ndarray

Time(s) relative to the Taylor series expansion point.

kfloat

Planet-to-star radius ratio \(R_p/R_\star\).

fratiofloat

Dayside-to-nightside per-surface-element flux ratio (amplitude scaling).

offsetfloat

Hotspot offset [radians].

cNDArray

A (3, 5) Taylor coefficient matrix produced by solve3d.

dcNDArray

A (7, 3, 5) parameter-derivative tensor produced by solve3d_d, with the leading axis ordered as (tc, p, a, i, e, w, lan).

Returns:

fluxfloat or ndarray

Emitted planet-to-star flux ratio. Shape (N,) for an array time.

dfluxNDArray

Partial derivatives of flux with respect to (tc, p, a, i, e, w, lan, k, fratio, offset). Shape (10,) for a scalar time, (N, 10) for an array time.