Models of pulsationally assisted gravitationally confined detonations with different ignition conditions
Models of pulsationally assisted gravitationally confined detonations with different ignition conditions
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DOI：
10.1051/0004-6361/202142194
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发表时间：
2021-11
影响因子：
6.5
通讯作者：
F. Lach;F. Callan;S. Sim;F. Röpke
中科院分区：
文献类型：
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作者：
F. Lach;F. Callan;S. Sim;F. Röpke
在过去的几十年里，许多Ia型超新星的爆炸方案已经被提出和研究，包括各种不同质量的白色矮星中的衰变和爆炸的组合，最高可达乌拉塞卡质量。其中之一是重力约束爆炸模型。在这种情况下，一个弱的反重力会燃烧到表面，包裹在束缚的核心周围，并在对极发生碰撞。随后在碰撞区域引爆。由于这种情况下的参数空间，即不同的中心密度和点火几何形状，还没有被详细研究，我们使用了以前专门用于Iax型超新星的参数研究的纯退化模型作为初始模型来研究引力约束的爆炸场景。我们的目标是判断这个通道是否可以解释Ia型超新星的许多亚群之一，甚至是正常事件。为此，我们采用了一个全面的管道三维Ia型超新星建模，包括流体动力学爆炸模拟，核网络计算和辐射传输。然后将从辐射传递中提取的可观测量与观测到的光变曲线和光谱进行比较。该研究产生了广泛的合成56镍的质量范围从0.257到1。057 M（cid：12），因此，就亮度而言，可以潜在地解释亚发光和过发光的Ia型超新星。然而，与观测到的光变曲线和光谱的粗略一致性只能在类91T天体中找到。尽管仍存在一些差异，但我们得出结论，不能排除引力约束爆炸模型作为产生91T类物体的机制。然而，这些模型并不能很好地解释正常的Ia型超新星或Iax型超新星。
Over the past decades, many explosion scenarios for Type Ia supernovae have been proposed and investigated including various combinations of deflagrations and detonations in white dwarfs of di ff erent masses up to the Chandrasekhar mass. One of these is the gravitationally confined detonation model. In this case a weak deflagration burns to the surface, wraps around the bound core, and collides at the antipode. A subsequent detonation is then initiated in the collision area. Since the parameter space for this scenario, that is, varying central densities and ignition geometries, has not been studied in detail, we used pure deflagration models of a previous parameter study dedicated to Type Iax supernovae as initial models to investigate the gravitationally confined detonation scenario. We aim to judge whether this channel can account for one of the many subgroups of Type Ia supernovae, or even normal events. To this end, we employed a comprehensive pipeline for three-dimensional Type Ia supernova modeling that consists of hydrodynamic explosion simulations, nuclear network calculations, and radiative transfer. The observables extracted from the radiative transfer are then compared to observed light curves and spectra. The study produces a wide range in masses of synthesized 56 Ni ranging from 0.257 to 1 . 057 M (cid:12) , and, thus, can potentially account for subluminous as well as overluminous Type Ia supernovae in terms of brightness. However, a rough agreement with observed light curves and spectra can only be found for 91T-like objects. Although several discrepancies remain, we conclude that the gravitationally confined detonation model cannot be ruled out as a mechanism to produce 91T-like objects. However, the models do not provide a good explanation for either normal Type Ia supernovae or Type Iax supernovae.