redback.transient_models.magnetar_driven_ejecta_models.general_mergernova_evolution

redback.transient_models.magnetar_driven_ejecta_models.general_mergernova_evolution(time, redshift, mej, beta, ejecta_radius, kappa, n_ism, logbint, logbext, p0, chi0, radius, logmoi, kappa_gamma, **kwargs)[source]
Parameters:

  • time – time in observer frame in days

  • redshift – redshift

  • mej – ejecta mass in solar units

  • beta – initial ejecta velocity

  • ejecta_radius – initial ejecta radius

  • kappa – opacity

  • n_ism – ism number density

  • logbint – log10 internal magnetic field in G

  • logbext – log10 external magnetic field in G

  • p0 – spin period in s

  • chi0 – initial inclination angle

  • radius – radius of NS in KM

  • logmoi – log10 moment of inertia of NS

  • kappa_gamma – gamma-ray opacity used to calculate magnetar thermalisation efficiency

  • kwargs – Additional parameters

  • pair_cascade_switch – whether to account for pair cascade losses, default is True

  • albedo (ejecta) – ejecta albedo; default is 0.5

  • pair_cascade_fraction – fraction of magnetar luminosity lost to pair cascades; default is 0.05

  • 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’

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

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

Returns:

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