# Keplerian Orbits¶

radvel.kepler.kepler(inbigM, inecc)[source]

Solve Kepler’s Equation

Parameters: inbigM (array) – input Mean anomaly inecc (array) – eccentricity array eccentric anomaly
radvel.kepler.rv_drive(t, orbel, use_c_kepler_solver=True)[source]

RV Drive

Parameters: t (array of floats) – times of observations orbel (array of floats) – [per, tp, e, om, K]. Omega is expected to be in radians use_c_kepler_solver (bool) – (default: True) If True use the Kepler solver written in C, else use the Python/NumPy version. (array of floats): radial velocity model rv
radvel.orbit.timeperi_to_timetrans(tp, per, ecc, omega, secondary=False)[source]

Convert Time of Periastron to Time of Transit

Parameters: tp (float) – time of periastron per (float) – period [days] ecc (float) – eccentricity omega (float) – argument of peri (radians) secondary (bool) – calculate time of secondary eclipse instead time of inferior conjuntion (time of transit if system is transiting) float
radvel.orbit.timetrans_to_timeperi(tc, per, ecc, omega)[source]

Convert Time of Transit to Time of Periastron Passage

Parameters: tc (float) – time of transit per (float) – period [days] ecc (float) – eccecntricity omega (float) – longitude of periastron (radians) time of periastron passage float
radvel.orbit.true_anomaly(t, tp, per, e)[source]

Calculate the true anomoly for a given time, period, eccentricity.

Parameters: t (array) – array of times in JD tp (float) – time of periastron, same units as t per (float) – orbital period in days e (float) – eccentricity true anomoly at each time array