Possible Contribution of Magnetized White Dwarf Binaries to Type Ia Supernova Populations
Possible Contribution of Magnetized White Dwarf Binaries to Type Ia Supernova Populations
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DOI：
10.3847/1538-4357/ab4814
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发表时间：
2019-10
期刊：
影响因子：
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通讯作者：
I. Ablimit;K. Maeda
中科院分区：
文献类型：
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作者：
I. Ablimit;K. Maeda
具有强磁场的吸积白矮星（WD）向 Ia 型超新星（SN Ia）的演化可能与经典的单简并（SD）通道不同。在本文中，我们对具有主序 (MS) 伴星（包括强磁化 WD 吸积）的 SD 通道进行二元布居合成模拟。在合理的假设下，此类系统的比例约为 15%，所得延迟时间分布大致遵循 t−1 幂律分布。在 (WD/MS) SD 通道内，高度磁化 WD 的贡献估计与经典非磁化 WD 通道的贡献相当。 SD 通道对 SNe Ia 的贡献至少占整个 SN Ia 群体的 30%。我们认为，由高度磁化的 WD 系统产生的 SNe Ia 不会具有经典 SD 通道所预期的观测特性；对于观察到的与 SD 通道相关的每个（可能是特殊的）SN，我们预计有相当数量的“隐藏”SD 群体属于正常类别。
The evolution of an accreting white dwarf (WD) with a strong magnetic field toward a Type Ia supernova (SN Ia) may differ from the classical single-degenerate (SD) channel. In this paper, we perform binary population synthesis simulations for the SD channel with a main-sequence (MS) companion, including the strongly magnetized WD accretion. Under a reasonable assumption that the fraction of such systems is ∼15%, the resulting delay-time distribution roughly follows the t−1 power-law distribution. Within the (WD/MS) SD channel, the contribution from the highly magnetized WD is estimated to be comparable to that from the classical, non-magnetized WD channel. The contribution of the SD channel toward SNe Ia can be at least ∼30% among the whole SN Ia population. We suggest that the SNe Ia resulting from the highly magnetized WD systems would not share the observational properties expected for the classical SD channel; for every (potentially peculiar) SN observationally associated with the SD channel, we expect a comparable number of the “hidden” SD population to be in the normal class.