meepmeep.numba3d.rv#
- meepmeep.numba3d.rv(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]], te: float = 0.0) float | ndarray[tuple[Any, ...], dtype[_ScalarT]][source]#
Evaluate the stellar radial velocity induced by the planet at an absolute time.
Direct counterpart of rv_c: epoch-folds the absolute time via zvel and applies the same Perryman (2018) Eq. 2.23 conversion to physical units.
- Parameters:
- time
floatorNDArray Absolute observation time(s) in the same units as tc and p.
- k
float Radial-velocity semi-amplitude of the star, in physical velocity units (e.g. m/s). The function output inherits these units.
- tc
float Transit-centre time (time of inferior conjunction), on the same time axis as time.
- p
float Orbital period.
- a
float Scaled semi-major axis in units of stellar radii.
- i
float Orbital inclination in radians.
- e
float Orbital eccentricity.
- c
NDArray A (3, 5) coefficient matrix produced by solve3d. Only row 2 is read.
- te
float, 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.
- time
- Returns:
- rv
floatorNDArray Stellar radial velocity in the same units as k. Positive when the planet is moving toward the observer (the star’s reflex motion has the same sign convention).
- rv