WDs in Binaries That Can Lead to SNIa

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.