9-13 July 2012
Africa/Johannesburg timezone
<a href="http://events.saip.org.za/internalPage.py?pageId=11&confId=14"><font color=#ff0000>SAIP2012 PROCEEDINGS AVAILABLE</font></a>

The Asymmetric Outflow of RS Ophiuchi

11 Jul 2012, 17:30
Oral Presentation Track D1 - Astrophysics Astrophysics


Dr Shazrene Mohamed (SAAO)

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Dr. Stephen Potter, sbp@saao.ac.za, SAAO

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Abstract content <br> &nbsp; (Max 300 words)

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 equa- torial 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.

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