redback.transient_models.kilonova_models.polytrope_eos_two_component_bns

redback.transient_models.kilonova_models.polytrope_eos_two_component_bns(time, redshift, mass_1, mass_2, log_p, gamma_1, gamma_2, gamma_3, zeta, vej_2, kappa_1, kappa_2, tf_1, tf_2, **kwargs)[source]

Assumes two kilonova components corresponding to dynamical and disk wind ejecta with properties derived using ejecta relation specified by keyword argument and lambda set by polytropic EOS.

Parameters:

  • time – observer frame time in days

  • redshift – redshift

  • mass_1 – mass of primary in solar masses

  • mass_2 – mass of secondary in solar masses

  • log_p – log central pressure in SI units

  • gamma_1 – polytrope index 1

  • gamma_2 – polytrope index 2

  • gamma_3 – polytrope index 3

  • zeta – fraction of disk that gets unbound

  • vej_2 – disk wind velocity in c

  • kappa_1 – gray opacity of first component

  • kappa_2 – gracy opacity of second component

  • tf_1 – floor temperature of first component

  • tf_2 – floor temperature of second component

  • kwargs – additional keyword arguments

  • ejecta_relation – a class that relates the instrinsic parameters to the kilonova parameters default is TwoComponentBNS

  • frequency – Required if output_format is ‘flux_density’. frequency to calculate - Must be same length as time array or a single number).

  • bands – Required if output_format is ‘magnitude’ or ‘flux’.

  • output_format – ‘flux_density’, ‘magnitude’, ‘spectra’, ‘flux’, ‘sncosmo_source’

  • lambda_array – Optional argument to set your desired wavelength array (in Angstroms) to evaluate the SED on.

  • cosmology – Cosmology to use for luminosity distance calculation. Defaults to Planck18. Must be a astropy.cosmology object.

Returns:

set by output format - ‘flux_density’, ‘magnitude’, ‘spectra’, ‘flux’, ‘sncosmo_source’