SNR

class gammapy.astro.source.SNR(e_sn='1e51 erg', theta=<Quantity 0.1>, n_ISM=<Quantity 1. 1 / cm3>, m_ejecta=<<class 'astropy.constants.iau2015.IAU2015'> name='Solar mass' value=1.988409870698051e+30 uncertainty=4.468805426856864e+25 unit='kg' reference='IAU 2015 Resolution B 3 + CODATA 2018'>, t_stop=<Quantity 1000000. K>, age=None, morphology='Shell2D', spectral_index=2.1)

Bases: object

Simple supernova remnant (SNR) evolution model.

The model is based on the Sedov-Taylor solution for strong explosions.

Reference: https://ui.adsabs.harvard.edu/abs/1950RSPSA.201..159T

Parameters

e_snQuantity

SNR energy (erg), equal to the SN energy after neutrino losses

thetaQuantity

Fraction of E_SN that goes into cosmic rays

n_ISMQuantity

ISM density (g cm^-3)

m_ejectaQuantity

Ejecta mass (g)

t_stopQuantity

Post-shock temperature where gamma-ray emission stops

Attributes Summary

sedov_taylor_begin	Characteristic time scale when the Sedov-Taylor phase of the SNR's evolution begins.
sedov_taylor_end	Characteristic time scale when the Sedov-Taylor phase of the SNR's evolution ends.

Methods Summary

luminosity_tev(t[, energy_min])	Gamma-ray luminosity above energy_min at age t.
radius(t)	Outer shell radius at age t.
radius_inner(t[, fraction])	Inner radius at age t of the SNR shell.

Attributes Documentation

Methods Documentation