Astronomy and Astrophysics – Astronomy
Scientific paper
May 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21642801m&link_type=abstract
American Astronomical Society, AAS Meeting #216, #428.01; Bulletin of the American Astronomical Society, Vol. 41, p.840
Astronomy and Astrophysics
Astronomy
Scientific paper
The characteristics of the progenitors of Type Ia supernovae (SNe) are unknown. One viable theory involves close binary systems containing a white dwarf and a companion donor star. Such systems are expected to have substantial circumstellar material (CSM) at the time of the supernova explosion, yet almost all Ia SNe show no signs of circumstellar interaction. We want to know where this CSM ends up. This knowledge of the distribution of matter around the progenitor system will tell us more about the interaction of the blast wave through the CSM from the Ia SNe.
One possible evolutionary channel involves a symbiotic binary containing a WD and a low-mass red giant. The interaction of strong winds from the WD and red giant should leave behind substantial CSM. We investigate the distribution of this circumstellar medium using 3D hydrodynamic simulations. Our simulation uses binary system parameters resembling RS Ophiuchi, and considers wind properties such that the two stellar winds have a comparable momentum flux. The interacting winds are followed out to a distance of 5.4 times the binary separation. The distribution of CSM is analyzed using several methods, including tracking streamlines of the wind from the red star, quantifying the volume filling fraction of dense gas, or finding the average mass-loss rate as a function of azimuthal angle from the orbital plane. Knowing these characteristics will help us better understand the system both before and after the supernova explosion.
Blondin John M.
Borkowski Kazimierz J.
Marcus Aaron
Reynolds Stephen P.
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