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arXiv · 2109.14817

Pre-Explosion Properties of Helium Star Donors to Thermonuclear Supernovae

Tin Long Sunny Wong·Josiah Schwab·Ylva Götberg
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Abstract

Helium star - carbon-oxygen white dwarf (CO WD) binaries are potential single-degenerate progenitor systems of thermonuclear supernovae. Revisiting a set of binary evolution calculations using the stellar evolution code $\texttt{MESA}$, we refine our previous predictions about which systems can lead to a thermonuclear supernova and then characterize the properties of the helium star donor at the time of explosion. We convert these model properties to NUV/optical magnitudes assuming a blackbody spectrum and support this approach using a matched stellar atmosphere model. These models will be valuable to compare with pre-explosion imaging for future supernovae, though we emphasize the observational difficulty of detecting extremely blue companions. The pre-explosion source detected in association with SN 2012Z has been interpreted as a helium star binary containing an initially ultra-massive WD in a multi-day orbit. However, extending our binary models to initial CO WD masses of up to $1.2\,M_{\odot}$, we find that these systems undergo off-center carbon ignitions and thus are not expected to produce thermonuclear supernovae. This tension suggests that, if SN 2012Z is associated with a helium star - WD binary, then the pre-explosion optical light from the system must be significantly modified by the binary environment and/or the WD does not have a carbon-rich interior composition.

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Tin Long Sunny Wong, Josiah Schwab, Ylva Götberg. 2021-09-30. Pre-Explosion Properties of Helium Star Donors to Thermonuclear Supernovae. https://doi.org/10.3847/1538-4357%2Fac27ae

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