Why Are Peculiar Type Ia Supernovae More Likely to Show the Signature of a Single-degenerate Model?

Abstract

Although type Ia supernovae (SNe Ia) are very useful in many astrophysical fields, their exact progenitor nature is still unclear. A basic method to distinguish the different progenitor models is to search the signal from the single degenerate (SD) model, e.g. the signal for the existence of a non-degenerate companion before or after supernova explosion. Observationally, some SNe Ia show such signal, while the others do not. Here, we propose a universal model to explain these observations based on the spin-up/spin-down model, in which a white dwarf (WD) will experience a spin-down phase before supernova explosion, and the spin-down timescale is determined by its initial mass, i.e. the more massive the initial WD, the shorter the spin-down timescale and then the more likely the SN Ia to show the SD signature. Therefore, our model predicts that the SNe Ia from hybrid carbon-oxygen-neon WDs are more likely to show the SD signature observationally, as some peculiar SNe Ia showed.

2 figures, ApJ Letter on line

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Cited by in corpus (5)

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• Oxygen-neon rich merger during common envelope evolution
• High-velocity feature as the indicator of the stellar population of Type Ia supernovae
• Possible white dwarf progenitors of type Ia supernovae
• Hot subdwarfs from the surviving companions of the white dwarf + main-sequence channel of Type Ia supernovae