meepmeep.numba3d.emission_phase_curve

meepmeep.numba3d.emission_phase_curve(time: float | ndarray[tuple[Any, ...], dtype[_ScalarT]], k: float, fratio: float, offset: float, tc: float, p: float, c: ndarray[tuple[Any, ...], dtype[_ScalarT]], te: float = 0.0) → float | ndarray[tuple[Any, ...], dtype[_ScalarT]]

Evaluate the cosine emission phase-curve flux at an absolute time.

Folds the absolute observation time back to an expansion-point-centered offset and delegates to the centered kernel. Returns the planet-to-star flux ratio of a simple cosine thermal-emission model with a hotspot offset (see emission_phase_curve_c).

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

Absolute observation time(s).

kfloat

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

fratiofloat

Dayside-to-nightside per-surface-element flux ratio (amplitude scaling); the peak-to-peak swing is \(k^2 f_\mathrm{ratio}\).

offsetfloat

Hotspot offset [radians].

tcfloat

Transit-centre time (time of inferior conjunction), on the same time axis as time.

pfloat

Orbital period.

cNDArray

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

tefloat, optional

Expansion-point offset from the transit centre [days] - the same value that was passed to solve3d. Defaults to 0.0, the expansion point at the transit centre.

Returns:

fluxfloat or NDArray

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