phoebe.dynamics.keplerian.
dynamics_from_bundle
(b, times, compute=None, return_euler=False, **kwargs)[source]¶Parse parameters in the bundle and call dynamics()
.
See dynamics()
for more detailed information.
NOTE: you must either provide compute (the label) OR all relevant options as kwargs (ltte)
b: (Bundle) the bundle with a set hierarchy times: (list or array) times at which to run the dynamics return_euler: (bool, default=False) whether to include euler angles
in the return
phoebe.dynamics.keplerian.
dynamics
(times, periods, eccs, smas, t0_perpasses, per0s, long_ans, incls, dpdts, deccdts, dperdts, components, t0=0.0, vgamma=0.0, mass_conservation=True, ltte=False, return_euler=False)[source]¶Compute the positions and velocites of each star in their nested Keplerian orbits at a given list of times.
See dynamics_from_bundle()
for a wrapper around this function
which automatically handles passing everything in the correct order
and in the correct units.
eccs: (iterable) eccentricity of the parent orbit for each star smas: (iterable) semi-major axis of the parent orbit for each
star [solRad]
phoebe.dynamics.nbody.
dynamics_from_bundle
(b, times, compute=None, return_roche_euler=False, use_kepcart=False, **kwargs)[source]¶Parse parameters in the bundle and call dynamics()
.
See dynamics()
for more detailed information.
NOTE: you must either provide compute (the label) OR all relevant options as kwargs (ltte, stepsize, gr, integrator)
b: (Bundle) the bundle with a set hierarchy times: (list or array) times at which to run the dynamics stepsize: (float, optional) stepsize for the integration
[default: 0.01]
ltte: (bool, default False) whether to account for light travel time effects. gr: (bool, default False) whether to account for general relativity effects.
phoebe.dynamics.nbody.
dynamics
(times, masses, smas, eccs, incls, per0s, long_ans, mean_anoms, rotperiods=None, t0=0.0, vgamma=0.0, stepsize=0.01, ltte=False, gr=False, integrator='ias15', return_roche_euler=False, use_kepcart=False)[source]¶phoebe.dynamics.nbody.
dynamics_from_bundle_bs
(b, times, compute=None, return_roche_euler=False, **kwargs)[source]¶Parse parameters in the bundle and call dynamics()
.
See dynamics()
for more detailed information.
NOTE: you must either provide compute (the label) OR all relevant options as kwargs (ltte)
b: (Bundle) the bundle with a set hierarchy times: (list or array) times at which to run the dynamics stepsize: (float, optional) stepsize for the integration
[default: 0.01]
ltte: (bool, default False) whether to account for light travel time effects.
phoebe.dynamics.nbody.
dynamics_bs
(times, masses, smas, eccs, incls, per0s, long_ans, mean_anoms, t0=0.0, vgamma=0.0, stepsize=0.01, orbiterror=1e-16, ltte=False, return_roche_euler=False)[source]¶Burlisch-Stoer integration of orbits to give positions and velocities of any given number of stars in hierarchical orbits. This code currently uses the NBody code in Josh Carter’s photodynam code available here:
[[TODO: include link]]
If using the Nbody mode in PHOEBE, please cite him as well:
[[TODO: include citation]]
See dynamics_from_bundle()
for a wrapper around this function
which automatically handles passing everything in the correct order
and in the correct units.
For each iterable input, stars and orbits should be listed in order from primary -> secondary for each nested hierarchy level. Each iterable for orbits should have length one less than those for each star (ie if 3 masses are provided, then 2 smas, eccs, etc need to be provided)
masses: (iterable) mass for each star in [solMass] smas: (iterable) semi-major axis for each orbit [AU] eccs: (iterable) eccentricities for each orbit incls: (iterable) inclinations for each orbit [rad] per0s: (iterable) longitudes of periastron for each orbit [rad] long_ans: (iterable) longitudes of the ascending node for each
orbit [rad]
mean_anoms: (iterable) mean anomalies for each orbit t0: (float) time at which to start the integrations stepsize: (float, optional) stepsize of the integrations
[default: 0.01]
ltte: (bool, default False) whether to account for light travel time effects.