Constraining the spin-down timescale of the white-dwarf progenitors of Type Ia supernovae

Abstract

Justham (2011) and DiStefano et al.\ (2011) proposed that the white-dwarf progenitor of a Type Ia supernova (SN Ia) may have to spin down before it can explode. As the white dwarf spin-down timescale is not well known theoretically, we here try to constrain it empirically (within the framework of this spin-down model) for progenitor systems that contain a giant donor and for which circumbinary material has been detected after the explosion: we obtain an upper limit of a few $10^7\mathrm{yr}$. Based on the study of Di Stefano & Kilic (2012) this means that it is too early to rule out the existence of a surviving companion in SNR 0509-67.5.

4 figures, accepted for publication in ApJ letter

References in corpus (4)

• Constraining the Type Ia Supernova Progenitor: The Search for Hydrogen in Nebular Spectra
• A statistical analysis of circumstellar material in Type Ia supernovae
• The single-degenerate channel for the progenitor of type Ia supernovae with different metallicities
• On the progenitors of super-Chandrasekhar mass type Ia supernovae

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• Blue Large-Amplitude Pulsators: the Possible Surviving Companions of Type Ia Supernovae
• The X-ray/radio and UV luminosity expected from symbiotic systems as the progenitor of SNe Ia
• No Surviving SN Ia Companion In SNR 0509-67.5: Stellar Population Characterization and Comparison To Models
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• Why Are Peculiar Type Ia Supernovae More Likely to Show the Signature of a Single-degenerate Model?
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