Theoretical Models of RS Ophiuchi and its γ-ray Emission: Comparison with SWIFT/BAT Observations

Details Theoretical Models of RS Ophiuchi and its γ-ray Emission: Comparison with SWIFT/BAT Observations Theoretical Models of RS Ophiuchi and its γ-ray Emission: Comparison with SWIFT/BAT Observations

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aspc..401..313h&link_type=abstract

RS Ophiuchi (2006) and the Recurrent Nova Phenomenon ASP Conference Series, Vol. 401, proceedings of the conference held 12-14 J

Astronomy and Astrophysics

Astronomy

Scientific paper

Theoretical hydrodynamical models, including complete nucleosynthesis, of the recent outburst of RS Oph are presented, which are able to reproduce the short recurrence period as well as the close to solar ejecta abundances. In addition, we show that the decay of radioactive isotopes in the ejecta can not account for the prompt hard X/soft γ-ray emission detected by the Swift/BAT instrument, in the 10-100 keV range. An important result is that the mass of the white dwarf is expected to rise in RS Oph, needing ˜ 3 × 10^4 years to reach the Chandrasekhar mass, and thus explode as a thermonuclear supernova.

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