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Hydrodynamic Studies of the Evolution of Recurrent Novae to Supernova Ia Explosions

Published online by Cambridge University Press:  17 January 2013

S. Starrfield ,
F. X. Timmes ,
W. R. Hix ,
C. Iliadis ,
W. D. Arnett ,
C. Meakin  and
W. M. Sparks
S. Starrfield
Affiliation:
School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287-1404, email: [email protected]; [email protected]
F. X. Timmes
Affiliation:
School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287-1404, email: [email protected]; [email protected]
W. R. Hix
Affiliation:
Dept. of Physics and Astronomy, University of Tennessee, Knoxville, TN 37996-1200 email: [email protected]
C. Iliadis
Affiliation:
Dept. of Physics & Astronomy, University of North Carolina, Chapel Hill, NC 27599-3255, email: [email protected]
W. D. Arnett
Affiliation:
Dept. of Astronomy, University of Arizona, Tucson, AZ, 85721; email: [email protected]
C. Meakin
Affiliation:
Los Alamos National Laboratory, Los Alamos, NM, 87545; email: [email protected]; [email protected]
W. M. Sparks
Affiliation:
Los Alamos National Laboratory, Los Alamos, NM, 87545; email: [email protected]; [email protected]
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Abstract

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We have begun new studies of the evolution of thermonuclear runaways (TNRs) in the accreted envelopes of white dwarfs (WDs). Here we focus on the recent outbursts of RS Oph (2006), U Sco (2010) and T Pyx (2011). U Sco explodes about every 10 years and the ejected material from the WD is helium rich. It has a short orbital period for recurrent novae (RNe) but the secondary is likely to be evolved. The WD is thought to be close in mass to the Chandrasekhar limit. T Pyx has just suffered its first outburst since 1966 and it was predicted to never experience another outburst. It has a short orbital period and has formed dust in the ejecta as this paper was being written. One important question is the secular evolution of the WD. Do the repeated outbursts cause the WD to gain or lose mass? If it is gaining mass, it could eventually reach the Chandrasekhar limit and become a Type Ia supernova (SNe Ia) if it can hide the hydrogen and helium in the system. Here, we report on our latest studies of TNRs in accreted envelopes on WDs using a variety of initial WD masses, luminosities, and mass accretion rates. Of great importance to our conclusions, we assume a solar composition (Lodders abundance distribution). We use our 1-D hydro code, NOVA, that includes the Hix and Thielemann nuclear reaction network, the Iliadis reaction rate library, the Timmes equation of state, OPAL opacities, and the new convection of Arnett, Meakin, and Young. We report on the amount of ejected mass, evolution time to explode, and whether or not the WD is growing or losing mass.

Keywords

stars: white dwarfsclose binariesdwarf novaeinteriorsnovaecataclysmic variablessupernovae
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Issue S281: Binary Paths to Type Ia Supernovae Explosions , July 2011 , pp. 166 - 171
Copyright
Copyright © International Astronomical Union 2013

References

Arnett, W. D., Meakin, C., & Young, P. A. 2010, ApJ, 710, 1619Google Scholar
Fujimoto, M. Y. 1982a, ApJ, 257, 752Google Scholar
Fujimoto, M. Y. 1982b, ApJ, 257, 767Google Scholar
Howell, D. A. 2011, Nature Comm., 2, 350CrossRefGoogle Scholar
Iliadis, C., et al. 2010, Nuclear Physics A, 841, 31Google Scholar
Kahabka, P. & van den Heuvel, E. P. J. 1997, ARAA, 35, 69CrossRefGoogle Scholar
Nomoto, K. 1982, ApJ, 253, 798Google Scholar
Schwarzschild, M. & Härm, R. 1965, ApJ, 142, 855CrossRefGoogle Scholar
Starrfield, S. 1989, in Classical Novae, ed. Bode, M. & Evans, A., Wiley, 39Google Scholar
Starrfield, S., Iliadis, C., & Hix, W. R. 2008, “Thermonuclear Processes,” in Classical Novae II, ed. Bode, M. & Evans, A., Cambridge University Press, 77Google Scholar
Starrfield, S., Iliadis, C., Hix, W. R., Timmes, F. X., & Sparks, W. M. 2009, ApJ, 692, 1532Google Scholar
Whelan, J. & Iben, I. 1973, ApJ, 186, 1007Google Scholar
Woosley, S. E. & Kasen, D. 2011, ApJ, 734, 38Google Scholar
Woudt, P. A., et al. 2009, ApJ, 706, 738Google Scholar
Zorotovic, M., Schreiber, M. R., & Gänsicke, B. T. 2011, A&A, 536, 42Google Scholar