论文标题
红色超级爆发前的苏佩诺娃爆发的流体动力学模拟：无球性和质量损失
Hydrodynamic Simulations of Pre-Supernova Outbursts in Red Supergiants: Asphericity and Mass Loss
论文作者
论文摘要
接近核心折叠的巨大恒星的活性会强烈影响恒星的外观及其随后的超新星的外观。后期对流核燃烧产生的波会向恒星表面传播，加热包膜并可能触发质量损失。在这项工作中，我们通过对Supernova质量射血量的二维模拟进行二维模拟来改进一维模型。从15 $ M _ {\ odot} $红色超级恒星的恒星进化模型开始，我们将能量沉积速率和持续时间视为模型参数，并检查质量 - 损失依赖性以及相应地探索前探索的形态。与一维模型不同，由于雷利 - 泰勒的不稳定性，由于波加热而引起的密度反转，波加热的主要效果是径向扩展恒星的氢包膜。对于长时间持续时间的低加热速率，该膨胀几乎是同源的，而高但短寿命的加热可以产生冲击，从而驱动信封膨胀，并在核心爆发时产生质量不同的密度曲线。不对称的数量很小，除非波加热超过预期，否则不太可能大量的质量损失。我们讨论对Supernova恒星变异性和超新星光曲线的影响。
The activity of massive stars approaching core-collapse can strongly affect the appearance of the star and its subsequent supernova. Late-phase convective nuclear burning generates waves that propagate toward the stellar surface, heating the envelope and potentially triggering mass loss. In this work, we improve on previous one-dimensional models by performing two-dimensional simulations of the pre-supernova mass ejection phase due wave heat deposition. Beginning with stellar evolutionary models of a 15 $M_{\odot}$ red supergiant star during core O-burning, we treat the energy deposition rate and duration as model parameters and examine the mass-loss dependence and the pre-explosion morphology accordingly. Unlike one-dimensional models, density inversions due to wave heating are smoothed by Rayleigh-Taylor instabilities, and the primary effect of wave heating is to radially expand the star's hydrogen envelope. For low heating rates with long durations, the expansion is nearly homologous, whereas high but short-lived heating can generate a shock that drives envelope expansion and results in a qualitatively different density profile at the time of core-collapse. Asymmetries are fairly small, and large amounts of mass loss are unlikely unless the wave heating exceeds expectations. We discuss implications for pre-supernova stellar variability and supernovae light curves.
