In recent years we have witnessed a growing interest in stars in the mass range at the edge between experiencing asymptotic giant branch (AGB) evolution or undergoing a supernova explosion.The final fate of these objects depends on a series of complex physical phenomena,primarily the rate of mass-loss, which determines whether the core can grow big enough to reach the Chandrasekhar mass and explode as an electron-capture supernova (EC-SN). As a members of binary systems, the C-O (or O-Ne) white dwarf cores can grow in mass as a consequence of mass transfer from a companion and may eventually explode as a thermonuclear supernova (SNtype Ia).
Karakas, A., Ventura, P., Dell’Agli, F., & Di Criscienzo, M. (2017). Foreword. Societa Astronomica Italiana. Memorie, 88(3), 231-232. http://sait.oat.ts.astro.it/MSAIt880317/PDF/2017MmSAI..88..231I.pdf