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The Asymmetric Outflow of RS Ophiuchi

Published online by Cambridge University Press:  17 January 2013

S. Mohamed ,
R. Booth  and
Ph. Podsiadlowski
S. Mohamed
Affiliation:
Argelander Institut für Astronomie, Auf dem Hügel 71, Bonn D-53121, Germany email: [email protected]
R. Booth
Affiliation:
Department of Astrophysics, University of Oxford, Oxford OX1 3RH email: [email protected], [email protected]
Ph. Podsiadlowski
Affiliation:
Department of Astrophysics, University of Oxford, Oxford OX1 3RH email: [email protected], [email protected]
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Abstract

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RS Ophiuchi (RS Oph) is a symbiotic binary consisting of a hot white dwarf accreting from the slow, dense stellar wind of a cool, red giant companion. The system belongs to, and is one of the best studied examples of, an even smaller subclass of binaries known as recurrent novae in which the white dwarf undergoes repeated thermonuclear outbursts. We present 3D smoothed particle hydrodynamics (SPH) models of mass transfer from the red giant to the white dwarf, followed by a nova outburst. We show that the outflow in the former is strongly concentrated towards the binary orbital plane. The nova ejecta is thus constrained in the equatorial directions, resulting in a bipolar outflow. The white dwarf in RS Oph is thought to be close to the Chandrasekhar mass, making the system a likely Type Ia supernova candidate. We discuss the role that such a highly structured circumstellar medium will play in the evolution of the supernova remnant.

Keywords

hydrodynamics — binaries: symbiotic — stars: novaecataclysmic variablesindividual (RS Oph)supernovae
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Issue S281: Binary Paths to Type Ia Supernovae Explosions , July 2011 , pp. 195 - 198
Copyright
Copyright © International Astronomical Union 2013

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