Thermonuclear explosions as Type II supernovae

We consider a binary stellar system, in which a low-mass, of 0.6 Msun, carbon-oxygen white dwarf (WD) mergers with a degenerate helium core of 0.4 Msun of a red giant. We analyse the outcome of a merger within a common envelope (CE). We predict the observational properties of the resulting transient...

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Bibliographic Details
Published in:arXiv.org 2024-01
Main Authors: Kozyreva, Alexandra, Moran-Fraile, Javier, Holas, Alexander, Bronner, Vincent A, Roepke, Friedrich K, Pavlyuk, Nikolay, Mironov, Alexey, Tsvetkov, Dmitriy
Format: Article
Language:English
Subjects:
Binary stars
Detonation
Explosions
Light curve
Massive stars
Neutrinos
Red giant stars
Supernovae
Thermonuclear explosions
White dwarf stars
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Summary:We consider a binary stellar system, in which a low-mass, of 0.6 Msun, carbon-oxygen white dwarf (WD) mergers with a degenerate helium core of 0.4 Msun of a red giant. We analyse the outcome of a merger within a common envelope (CE). We predict the observational properties of the resulting transient. We find that the double detonation of the WD, being a pure thermonuclear explosion and embedded into the hydrogen-rich CE, has a light curve with the distinct plateau shape, i.e. looks like a supernova (SN) Type IIP, with a duration of about 40 days. We find five observed SNe IIP: SN 2004dy, SN 2005af, SN 2005hd, SN 2007aa, and SN 2008bu, that match the V-band light curve of our models. Hence, we show that a thermonuclear explosion within a CE might be mistakenly identified as a SN IIP, which are believed to be an outcome of a core-collapse neutrino-driven explosion of a massive star. We discuss a number of diagnostics, that may help to distinguish this kind of a thermonuclear explosion from a core-collapse SN.
ISSN:2331-8422