celeries.mmr.MMR.v2ell

MMR.v2ell(v, delta, Gamma=1, phiG=0, phiGamma=0, km_max=None)

Convert the coordinates of the average problem v = (y, phi, x, dL) to elliptical coordinates.

Parameters:

v(4*npla-4,) ndarray

Normalized coordinates (y, phi, x, dL).

deltafloat

Value of delta (normalized by Gamma).

Gammafloat

Value of Gamma, setting the scale of the system.

phiG, phiGammafloat

Values of the angles associated to G and Gamma (which do not appear in the Hamiltonian).

km_maxint or None

If provided, the change of variables due to averaging is peformed, including terms up to km_max.

Returns:

ell(npla, 4,) ndarray

Astrocentric coordinates: a (semi-major axis), e (eccentricity), \(\lambda_0\) (mean longitude), and \(\varpi\) (longitude of periastron) of the planets.