meepmeep.numba3d.ev_signal

meepmeep.numba3d.ev_signal(time: float | ndarray[tuple[Any, ...], dtype[_ScalarT]], alpha: float, mass_ratio: float, inc: float, tc: float, p: float, c: ndarray[tuple[Any, ...], dtype[_ScalarT]], te: float = 0.0) → float | ndarray[tuple[Any, ...], dtype[_ScalarT]]

Evaluate the ellipsoidal-variation signal at an absolute time.

Folds the absolute observation time back to an expansion-point-centered offset and delegates to the centered kernel. Returns the relative flux variation induced by the tidally distorted primary, \(S = -\alpha\,q\,\sin^2 i\,(2 c_z^2 - 1)/d^3\), with \(d\) the instantaneous 3D star-planet distance in stellar radii.

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).

alphafloat

Gravity-darkening coefficient (Lillo-Box et al. 2014, Eq. 7).

mass_ratiofloat

Planet-to-star mass ratio \(M_p / M_\star\).

incfloat

Orbital inclination [radians]. Enters only through the \(\sin^2 i\) projected-area factor.

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:

evfloat or NDArray

Relative flux variation due to ellipsoidal distortion. Shape (N,) for an array time.