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Title: Supernova shocks cannot explain the inflated state of hypervelocity runaways from white dwarf binaries
Recent observations have found a growing number of hypervelocity stars with speeds of ≈1500 − 2500 km s−1that could have only been produced through thermonuclear supernovae in white dwarf binaries. Most of the observed hypervelocity runaways in this class display a surprising inflated structure: their current radii are roughly an order of magnitude greater than they would have been as white dwarfs filling their Roche lobe. While many simulations exist studying the dynamical phase leading to supernova detonation in these systems, no detailed calculations of the long-term structure of the runaways have yet been performed. We used an existing AREPOhydrodynamical simulation of a supernova in a white dwarf binary as a starting point for the evolution of these stars with the one-dimensional stellar evolution code MESA. We show that the supernova shock is not energetic enough to inflate the white dwarf over timescales longer than a few thousand years, significantly shorter than the 105 − 6year lifetimes inferred for observed hypervelocity runaways. Although they experience a shock from a supernova less than ≈0.02 R⊙away, our models do not experience significant interior heating, and all contract back to radii of around 0.01 R⊙within about 104years. Explaining the observed inflated states requires either an additional source of significant heating or some other physics that is not yet accounted for in the subsequent evolution.  more » « less
Award ID(s):
2206523
PAR ID:
10631858
Author(s) / Creator(s):
; ; ; ; ; ; ;
Publisher / Repository:
Astronomy & Astrophysics
Date Published:
Journal Name:
Astronomy & Astrophysics
Volume:
693
ISSN:
0004-6361
Page Range / eLocation ID:
A114
Format(s):
Medium: X
Sponsoring Org:
National Science Foundation
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