Dynamical Interaction of Supernova Remnant with Pre-Existing Wind Bubble

Details Dynamical Interaction of Supernova Remnant with Pre-Existing Wind Bubble Dynamical Interaction of Supernova Remnant with Pre-Existing Wind Bubble

Dec 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996pkas...11...27c&link_type=abstract

Publications of the Korean Astronomical Society, vol.11, no.1, p.27-47

Astronomy and Astrophysics

Astronomy

Scientific paper

We have performed the high resolution computer simulation with 1D spherical hydrodynamic code in order to study the dynamical evolution of supernova ejecta interacting with a pre-existing fast wind structure. The fast wind structure has been calculated with M_in=3x10e-6 Mo yr^-1 and v_in=1000km/sec, which velocity is higher than the critical velocity relating to the initial radiative cooling. The fast wind becomes initially adiabatic. After a shell formation time of ~4000yrs, the wind becomes radiative cooling at the shell zone, forming a thin dense radiative shell and an adiabatic wind bubble afterward. When supernova explodes in the wind center at 20,000yrs after the wind evolves, the supernova ejecta, which has a dense distribution of rho~r^-n(here we have n = 9), interacts initially with the understood wind zone, producing forward and reverse shocks. The reverse shock has the supernova ejecta and its temperature increases. In this study, as the mass of the supernova ejecta is larger than that of the wind shell(M_ej=5Mo, M_sw=2Mo), we can confirm two shell structures: an outer shell by the supernova ejecta and a secondarily shocked wind shell by it. The secondarily shocked wind shell should accelerates in this case to be R-T unstable, consequently producing the knots.

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