论文标题
强烈磁性的非旋转超新星的3D模拟：爆炸动力学和残余特性
3D Simulations of Strongly Magnetised Non-Rotating Supernovae: Explosion Dynamics and Remnant Properties
论文作者
论文摘要
We investigate the impact of strong initial magnetic fields in core-collapse supernovae of non-rotating progenitors by simulating the collapse and explosion of a 16.9 Msun star for a strong- and weak-field case assuming a twisted-torus field with initial central field strengths of ~1012 G and ~106 G. The strong-field model has been set up with a view to the fossil-field scenario for magnetar formation and emulates a可能发生在合并形成的巨大恒星中的爆发前场配置。反弹后，该模型在100 s发生冲击复兴，并在310毫秒时达到9.3 x 10^50 ERG的爆炸能量，与弱场模型中更延迟且能量较低的爆炸相反。强磁场有助于早期引发中微子驱动的爆炸，从而导致爆炸能量的快速上升和饱和。从动态上讲，强的初始场会导致增益区域中的磁场快速积累至动力学等级的40％，还会产生相当大的震动前RAM压力扰动，已知有利于不对称的冲击膨胀。对于强场模型，我们发现一个外推的中子星踢约350 km/s，旋转周期约70毫秒，没有自旋踢对准。在模拟结束时，原始恒星的偶极磁场强度为2 x 10^14 g，趋势下降。令人惊讶的是，弱场模型中的表面偶极子场更强，它反对爆发前场与中子星的出生磁场之间的直接连接。
We investigate the impact of strong initial magnetic fields in core-collapse supernovae of non-rotating progenitors by simulating the collapse and explosion of a 16.9 Msun star for a strong- and weak-field case assuming a twisted-torus field with initial central field strengths of ~1012 G and ~106 G. The strong-field model has been set up with a view to the fossil-field scenario for magnetar formation and emulates a pre-collapse field configuration that may occur in massive stars formed by a merger. This model undergoes shock revival already 100 s after bounce and reaches an explosion energy of 9.3 x 10^50 erg at 310 ms, in contrast to a more delayed and less energetic explosion in the weak-field model. The strong magnetic fields help trigger a neutrino-driven explosion early on, which results in a rapid rise and saturation of the explosion energy. Dynamically, the strong initial field leads to a fast build-up of magnetic fields in the gain region to 40% of kinetic equipartition and also creates sizable pre-shock ram pressure perturbations that are known to be conducive to asymmetric shock expansion. For the strong-field model, we find an extrapolated neutron star kick of ~350 km/s, a spin period of ~70 ms, and no spin-kick alignment. The dipole field strength of the proto-neutron star is 2 x 10^14 G by the end of the simulation with a declining trend. Surprisingly, the surface dipole field in the weak-field model is stronger, which argues against a straightforward connection between pre-collapse fields and the birth magnetic fields of neutron stars.
