redback.transient_models.supernova_models.shockcooling_sapirwaxman_and_arnett

redback.transient_models.supernova_models.shockcooling_sapirwaxman_and_arnett(time, redshift, v_shock, m_env, mej, f_rho, f_nickel, radius, kappa, **kwargs)[source]

Assumes Shock cooling following Sapir and Waxman and arnett model for radioactive decay

Parameters:

  • time – time in source frame in days

  • v_shock – shock speed in km/s, also the ejecta velocity in the arnett calculation

  • m_env – envelope mass in solar masses

  • mej – ejecta mass in solar masses

  • f_rho – f_rho. Typically, of order unity

  • f_nickel – fraction of nickel mass

  • radius – star/envelope radius in units of 10^13 cm

  • kappa – opacity in cm^2/g

  • kwargs – Additional parameters required by model

  • n – index of progenitor density profile, 1.5 (default) or 3.0

  • RW – If True, use the simplified Rabinak & Waxman formulation (off by default)

  • 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’