WDs in Binaries That Can Lead to SNIa

Y. Hillman; D. Prialnik; A. Kovetz; M.M. Shara

doi:10.1051/eas/1571033

All issues

Volume 71-72 (2015)

EAS Publications Series, 71-72 (2015) 151-153

Abstract

Issue		EAS Publications Series Volume 71-72, 2015 The Physics of Evolved Stars: A Conference Dedicated to the Memory of Olivier Chesneau


Page(s)		151 - 153
Section		Binaries
DOI		https://doi.org/10.1051/eas/1571033
Published online		01 December 2015

The Physics of Evolved Stars: A Conference Dedicated to the Memory of Olivier Chesneau
E. Lagadec, F. Millour and T. Lanz (eds)
EAS Publications Series, 71–72 (2015) 151-153

WDs in Binaries That Can Lead to SNIa

Y. Hillman¹, D. Prialnik¹, A. Kovetz¹^,2 and M.M. Shara³

¹ Department of Geosciences, Tel-Aviv University, Tel-Aviv 69978, Israel
² School of Physics and Astronomy, Tel Aviv University, Tel-Aviv 69978, Israel
³ Department of Astrophysics, American Museum of Natural History, New York, NY, USA

e-mail: yaelhill@post.tau.ac.il

Abstract

Focusing on recurrent novae (RN), we explore white dwarf (WD) masses and accretion rates (Ṁ), to determine the combinations that will retain some of the accreted mass at the end of each cycle. Thus, the WD may grow toward the Chandrasekhar mass (M_Ch) and explode as a Type Ia Supernova (SNIa). We discuss limits imposed by the secondary mass (M_s) and evolution time scales. We also discuss observables which can assist in detecting potential progenitors of SNIa.