Context. The progenitors of many core-collapse supernovae (CCSNe) are expected to be in binary systems. After the SN explosion in a binary, the companion star may suffer from mass stripping and be shock heated as a result of the impact of the SN ejecta. If the binary system is disrupted by the SN explosion, the companion star is ejected as a runaway star, and in some cases as a hypervelocity star. Aims. By performing a series of three-dimensional (3D) hydrodynamical simulations of the collision of SN ejecta with the companion star, we investigate how CCSN explosions affect their binary companion. Methods. We use the BEC stellar evolution code to construct the detailed companion structure at the moment of SN explosion. The impact of the SN blast wave on the companion star is followed by means of 3D smoothed particle hydrodynamics (SPH) simulations using the Stellar GADGET code. Results. For main-sequence (MS) companion stars, we find that the amount of removed stellar mass, the resulting impact velocity, and the chemical contamination of the companion that results from the impact of the SN ejecta strongly increases with decreasing binary separation and increasing explosion energy. Their relationship can be approximately fitted by power laws, which is consistent with the results obtained from impact simulations of Type Ia SNe. However, we find that the impact velocity is sensitive to the momentum profile of the outer SN ejecta and, in fact, may decrease with increasing ejecta mass, depending on the modeling of the ejecta. Because most companion stars to Type Ib/c CCSNe are in their MS phase at the moment of the explosion, combined with the strongly decaying impact effects with increasing binary separation, we argue that the majority of these SNe lead to inefficient mass stripping and shock heating of the companion star following the impact of the ejecta. Conclusions. Our simulations show that the impact effects of Type Ib/c SN ejecta on the structure of MS companion stars, and thus their long-term post-explosion evolution, is in general not dramatic. We find that at most 10% of their mass is lost and their resulting impact velocities are less than 100 km s-1.
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机译：上下文。许多核心坍塌超新星（CCSNe）的祖先预计将处于二元系统中。在双星SN爆炸之后，由于SN喷射的撞击，伴星可能会发生质量剥离并被激波加热。如果双星系统被SN爆炸破坏，则伴星会像失控星一样被弹出，在某些情况下会作为超高速星被弹出。目的通过对SN射流与伴星碰撞的一系列三维（3D）流体动力学模拟，我们研究了CCSN爆炸如何影响其双星伴星。方法。我们使用BEC恒星演化代码在SN爆炸时构造详细的伴随结构。 SN爆炸波对伴星的影响是通过使用Stellar GADGET代码进行的3D平滑粒子流体动力学（SPH）模拟实现的。结果。对于主序（MS）伴星，我们发现，随着双星间隔的减小和爆炸的增加，恒星质量的去除量，由此产生的撞击速度以及由SN喷出的撞击所导致的伴星的化学污染会大大增加。能源。它们的关系可以由幂定律近似拟合，这与从Ia型SNe碰撞仿真获得的结果一致。但是，我们发现，撞击速度对外部SN射流的动量曲线很敏感，实际上，可能会随着射流质量的增加而降低，具体取决于射流的模型。因为大多数Ib / c型CCSNe伴星在爆炸时都处于MS阶段，再加上强烈衰减的撞击效应和增加的双星分离，我们认为这些SNe的大多数导致了低质量的汽提和冲击加热受到喷射器撞击后伴星的变化结论。我们的模拟结果表明，Ib / c型SN射流对MS伴星结构的影响以及爆炸后的长期演化通常并不显着。我们发现，他们最多损失了10％的质量，因此产生的撞击速度小于100 km s-1。
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