Evaporating Planets in SNe Ia

Abstract

I suggest that in rare cases type Ia supernovae (SNe Ia) evaporate Jupiter-like planets that reside within a=50Ro from the SN, accounting for the presence of ~0.001Mo of hydrogen in the ejecta. It is not easy to form such planets. The common envelope evolution (CEE) might end with the formation of a circumbinary disk with a typical size of R(disk)~10-50Ro. However, the bright central star might prevent the formation of planets. Alternatively, the planets might be first-generation planets that survived the entire evolution. Interestingly, all five SN Ia binary scenarios (core degenerate; double degenerate; double detonation; single degenerate; WD-WD collision) might account for the presence of planets.

Published in Research Notes of the American Astronomical Society, 3, 153 (2019, October 14)

References in corpus (2)

• First versus second generation planet formation in post common envelope binary (PCEB) planetary systems
• H-$\alpha$ emission in the nebular spectrum of the Type Ia supernova ASASSN-18tb

Cited by in corpus (2)

• Spectral signatures of H-rich material stripped from a non-degenerate companion by a Type Ia supernova
• The effect of aspherical stellar wind of giant stars on the symbiotic channel of type Ia supernovae