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首页> 外文期刊>The Astrophysical Journal. Letters >HEAD-ON COLLISIONS OF WHITE DWARFS IN TRIPLE SYSTEMS COULD EXPLAIN TYPE Ia SUPERNOVAE
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HEAD-ON COLLISIONS OF WHITE DWARFS IN TRIPLE SYSTEMS COULD EXPLAIN TYPE Ia SUPERNOVAE

机译：三重系统中白矮人的正面碰撞可能解释了Ia型超新星

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摘要

Type Ia supernovae (SNe Ia), thermonuclear explosions of carbon-oxygen white dwarfs (CO-WDs), are currently the best cosmological "standard candles," but the triggering mechanism of the explosion is unknown. It was recently shown that the rate of head-on collisions of typical field CO-WDs in triple systems may be comparable to the SNe Ia rate. Here we provide evidence supporting a scenario in which the majority of SNe Ia are the result of such head-on collisions of CO-WDs. In this case, the nuclear detonation is due to a well understood shock ignition, devoid of commonly introduced free parameters such as the deflagration velocity or transition to detonation criteria. By using two-dimensional hydrodynamical simulations with a fully resolved ignition process, we show that zero-impact-parameter collisions of typical CO-WDs with masses 0.5?1M_⊙ result in explosions that synthesize ~(56)Ni masses in the range of ～0.1?1M_⊙, spanning the wide distribution of yields observed for the majority of SNe Ia. All collision models yield the same late-time (≥60 days since explosion) bolometric light curve when normalized by ~(56)Ni masses (to better than 30%), in agreement with observations. The calculated widths of the 56Ni-mass-weighted line-of-sight velocity distributions are correlated with the calculated ~(56)Ni yield, agreeing with the observed correlation. The strong correlation, shown here for the first time, between ~(56)Ni yield and total mass of the colliding CO-WDs (insensitive to their mass ratio), is suggestive as the source for the continuous distribution of observed SN Ia features, possibly including the Philips relation.
机译：Ia型超新星（SNe Ia）是碳氧白矮星（CO-WDs）的热核爆炸，是目前最好的宇宙学“标准蜡烛”，但爆炸的触发机制尚不清楚。最近显示，在三重系统中典型的现场CO-WD正面碰撞的速率可能与SNe Ia速率相当。在这里，我们提供的证据支持一种场景，其中大多数SNe Ia是CO-WD正面碰撞的结果。在这种情况下，核爆炸是由于众所周知的冲击点火，没有通常引入的自由参数，例如爆燃速度或过渡到爆炸标准。通过使用具有完全解析的点火过程的二维流体动力学模拟，我们发现，质量为0.5？1M_⊙的典型CO-WD的零冲击参数碰撞会导致爆炸，爆炸产生的〜（56）Ni质量在〜范围内0.1？1M_⊙，涵盖了大多数SNe Ia的单产。与观察结果一致，当通过〜（56）Ni质量归一化（好于30％）时，所有碰撞模型均产生相同的后期（爆炸后≥60天）辐射热光曲线。计算得出的56Ni质量加权视线速度分布的宽度与计算出的〜（56）Ni产率相关，与观察到的相关性一致。这是首次显示〜（56）Ni产率与碰撞的CO-WD的总质量之间的强相关性（对它们的质量比不敏感），这提示了所观察到的SN Ia特征的连续分布来源，可能包括飞利浦关系。

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