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White Dwarf Masses and Accretion Rates of Recurrent Novae: an X-ray Perspective

Published online by Cambridge University Press:  17 January 2013

Koji Mukai ,
Jennifer L. Sokoloski ,
Thomas Nelson  and
Gerardo J. M. Luna
Koji Mukai
Affiliation:
CRESST and X-ray Astrophysics Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA email: Koji.Mukai@nasa.gov Also Department of Physics, University of Maryland Baltimore County, 1000 Hilltop Circle, Baltimore, MD 21250, USA
Jennifer L. Sokoloski
Affiliation:
Columbia Astrophysics Laboratory, 550 W. 120th St., 1027 Pupin Hall, Columbia University, New York, NY 10027, USA
Thomas Nelson
Affiliation:
School of Physics and Astronomy, University of Minnesota, 115 Church St. SE, Minneapolis, MN 55455, USA
Gerardo J. M. Luna
Affiliation:
Instituto de Ciencias Astronómicas, de la Tierra y del Espacio (ICATE/FCEFyN), Av. España Sur 1512, J5402DSP, San Juan, Argentina
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Abstract

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We present recent results of quiescent X-ray observations of recurrent novae (RNe) and related objects. Several RNe are luminous hard X-ray sources in quiescence, consistent with accretion onto a near Chandrasekhar mass white dwarf. Detection of similar hard X-ray emissions in old novae and other cataclysmic variables may lead to identification of additional RNe candidates. On the other hand, other RNe are found to be comparatively hard X-ray faint. We present several scenarios that may explain this dichotomy, which should be explored further.

Keywords

novaecataclysmic variables — X-rays: binariesbursts
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Issue S281: Binary Paths to Type Ia Supernovae Explosions , July 2011 , pp. 186 - 189
Copyright
Copyright © International Astronomical Union 2013

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