Near-Chandrasekhar-mass type Ia supernovae from the double-degenerate channel
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Cita com:
hdl:2117/368109
Tipus de documentArticle
Data publicació2022-01-01
EditorInstitute of Physics (IOP)
Condicions d'accésAccés obert
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continguts d'aquesta obra estan subjectes a la llicència de Creative Commons
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Reconeixement 4.0 Internacional
Abstract
Recent observational evidence has demonstrated that white dwarf (WD) mergers are a highly efficient mechanism for mass accretion onto WDs in the galaxy. In this paper, we show that WD mergers naturally produce highly magnetized, uniformly rotating WDs, including a substantial population within a narrow mass range close to the Chandrasekhar mass (MCh). These near-MCh WD mergers subsequently undergo rapid spin up and compression on a ~ 102 yr timescale, either leading to central ignition and a normal SN Ia via the DDT mechanism, or alternatively to a failed detonation and SN Iax through pure deflagration. The resulting SNe Ia and SNe Iax will have spectra, light curves, polarimetry, and nucleosynthetic yields similar to those predicted to arise through the canonical near-MCh single degenerate (SD) channel, but with a t-1 delay time distribution characteristic of the double-degenerate channel. Furthermore, in contrast to the SD channel, WD merger near-MCh SNe Ia and SNe Iax will not produce observable companion signatures. We discuss a range of implications of these findings, from SNe Ia explosion mechanisms, to galactic nucleosynthesis of iron peak elements including manganese
CitacióNeopane, S. [et al.]. Near-Chandrasekhar-mass type Ia supernovae from the double-degenerate channel. "The astrophysical journal letters", 1 Gener 2022, vol. 925, núm. 92, p. 1-13.
ISSN1538-4357
Versió de l'editorhttps://iopscience.iop.org/article/10.3847/1538-4357/ac3b52
Altres identificadorshttps://arxiv.org/abs/2111.09890
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