meepmeep.numba3d.rv_d

meepmeep.numba3d.rv_d(time: float | ndarray[tuple[Any, ...], dtype[_ScalarT]], k: float, tc: float, p: float, a: float, i: float, e: float, c: ndarray[tuple[Any, ...], dtype[_ScalarT]], dc: ndarray[tuple[Any, ...], dtype[_ScalarT]], te: float = 0.0)

Evaluate the stellar radial velocity and its parameter derivatives at an absolute time.

Direct counterpart of rv_cd: epoch-folds the absolute time time around the expansion point and delegates to rv_cd.

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), mirroring the value-only radial_velocity.rv.

Parameters:

timefloat or ndarray

Absolute observation time(s) in the same units as tc and p.

kfloat

Radial-velocity semi-amplitude of the star, in physical velocity units (e.g. m/s). The function output inherits these units.

tcfloat

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

tefloat, optional

Expansion-point offset from the transit centre [days] - the same value that was passed to solve3d_d. Defaults to 0.0, the expansion point at the transit centre.

pfloat

Orbital period.

afloat

Scaled semi-major axis in units of stellar radii.

ifloat

Orbital inclination in radians.

efloat

Orbital eccentricity.

cNDArray

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

dcNDArray

A (7, 3, 5) parameter-derivative tensor produced by solve3d_d.

Returns:

rvfloat or ndarray

Stellar radial velocity in the same units as k. Shape (N,) for an array time.

drvNDArray

Partial derivatives of rv with respect to (tc, p, a, i, e, w, lan). Shape (7,) for a scalar time, (N, 7) for an array time.