posydon.binary_evol.DT.winds

posydon.binary_evol.DT.winds.default_winds

posydon.binary_evol.DT.winds.default_winds.default_sep_from_winds(a, e, primary, secondary, verbose=False)[source]

This function calculates the change in orbital separation from

wind loss, as e.g., in:

Tauris, T. M., & van den Heuvel, E. 2006,

Compact stellar X-ray sources, 1, 623

from simple arguments regarding the balance of orbital angular

momentum.

Parameters:

  • a (float) – The current orbital separation. [Rsolar]

  • e (float) – The current orbital eccentricity.

  • primary (SingleStar object) – A single star object, representing the primary (more evolved) star in the binary and containing its properties.

  • secondary (SingleStar object) – A single star object, representing the secondary (less evolved) star in the binary and containing its properties.

  • verbose (bool) – True if we want to print stuff.

Returns:

  • da_mt_tot (float) – The change in orbital separation from both stars

  • for a time step in step_detached’s solve_ivp(). [Rsolar/yr]

posydon.binary_evol.DT.winds.default_winds.default_spin_from_winds(a, e, primary, secondary, verbose=False)[source]

This function calculates the change in angular rotation rates

from wind loss.

Parameters:

  • a (float) – The current orbital separation (unused in calculation, and only present in debugging output). [Rsolar]

  • e (float) – The current orbital eccentricity (unused in calculation, and only present in debugging output).

  • primary (SingleStar object) – A single star object, representing the primary (more evolved) star in the binary and containing its properties.

  • secondary (SingleStar object) – A single star object, representing the secondary (less evolved) star in the binary and containing its properties.

  • verbose (bool) – True if we want to print stuff.

Returns:

  • dOmega_sec (float) – The change in rotation rate of the secondary (less evolved)

  • star for a time step in step_detached’s solve_ivp(). [rad/yr^2]

  • dOmega_pri (float) – The change in rotation rate of the primary (more evolved)

  • star for a time step in step_detached’s solve_ivp(). [rad/yr^2]