Velocity limits in the thermonuclear supernova ejection scenario for hypervelocity stars and the origin of US 708

Abstract

Hypervelocity stars (HVS) are a class of stars moving at high enough velocities to be gravitationally unbound from the Galaxy. Ejection from a close binary system in which one of the components undergoes a thermonuclear supernova (SN) has emerged as a promising candidate production mechanism for the least massive specimens of this class. This study presents a thorough theoretical analysis of candidate progenitor systems of thermonuclear SNe in the single degenerate helium donor scenario in the relevant parameter space leading to the ejection of HVS. The primary goal is investigation of the, previously unclear, characteristics of the velocity spectra of the ejected component. Presented are the results of 390 binary model sequences computed with the MESA framework, investigating the evolution of supernova progenitors composed of a helium-rich hot subdwarf and a accreting white dwarf. Results are then correlated with an idealized kinematic analysis of the observed object US 708. It is seen that the ejection velocity spectra reach a maximum in the range $0.19M_{\odot }<M_{HVS}<0.25M_{\odot }$. Depending on the local Galactic potential, all donors below $0.4{\text{M}}_{\odot }$ are expected to become HVS. This channel is able to account for runaway velocities up to $\sim 1150{\text{km s}}^{-1}$ with a Chandrasekhar mass accretor, exceeding $1200{\text{km s}}^{-1}$ if super-Chandrasekhar mass detonations are taken into account. It is found that the previously assumed mass of $0.3M_{\odot }$ for US 708, combined with more recently obtained proper motions, favor a sub-Chandrasekhar mass explosion with a terminal WD mass between $1.1M_{\odot }$ and $1.2M_{\odot }$. The presence of clear ejection velocity maxima provides constraints on the terminal state of a supernova progenitor. It is possible to discern certain types of explosion mechanisms from the inferred ejection velocities alone.

17 pages, 14 figures, accepted for publication by A&A, replacement due to typo in Fig. 11

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