论文标题
部分恒星爆炸 - 弹出质量和最小能量
Partial Stellar Explosions -- Ejected Mass and Minimal Energy
论文作者
论文摘要
在其进化后期，许多巨大的恒星似乎会增加质量损失。在某些情况下，排出的质量可能起源于非末端爆炸性爆发，而不是连续的风。在这里，我们使用分析论证和数值流体动力学模拟，研究了弹出质量的依赖性，$ m _ {\ rm ej} $，对恒星深处的能量预算$ e $。 Focusing on polytropic stellar models, we find that for explosion energies smaller than the stellar binding energy, the ejected mass scales as $m_{\rm ej} \propto E^{\varepsilon_{m}}$, where $\varepsilon_m = 2.4-3.0$ depending on the polytropic index.恒星边缘附近的冲击突出发射引起的能量损失导致存在最小的质量爆炸能量，这对应于最小的喷射质量。对于从狼射线星到红色超级巨人的各种祖细胞，我们发现$ e _ {\ rm min} \ of 10^{46} {46} -10^{47} \ rm \ \ rm \，几乎独立于恒星半径。相应的最小喷射质量在不同的祖细胞之间差异很大，范围从$ \ sim \！ 10^{ - 8} \，\ rm m_ \ odot $在紧凑的星星中，最多$ \ sim \！ 10^{ - 2} \，\ rm m_ \ odot $ in Red Supergiants。我们讨论了我们的结果对由波加热驱动的苏佩诺娃爆发的含义，以及由逼真的恒星的非构成不透明和绝热指数引起的并发症。
Many massive stars appear to undergo enhanced mass loss during late stages of their evolution. In some cases, the ejected mass likely originates from non-terminal explosive outbursts, rather than continuous winds. Here we study the dependence of the ejecta mass, $m_{\rm ej}$, on the energy budget $E$ of an explosion deep within the star, using both analytical arguments and numerical hydrodynamics simulations. Focusing on polytropic stellar models, we find that for explosion energies smaller than the stellar binding energy, the ejected mass scales as $m_{\rm ej} \propto E^{\varepsilon_{m}}$, where $\varepsilon_m = 2.4-3.0$ depending on the polytropic index. The loss of energy due to shock breakout emission near the stellar edge leads to the existence of a minimal mass-shedding explosion energy, corresponding to a minimal ejecta mass. For a wide range of progenitors, from Wolf-Rayet stars to red supergiants, we find a similar limiting energy of $E_{\rm min} \approx 10^{46}-10^{47} \rm \, erg$, almost independent of the stellar radius. The corresponding minimal ejecta mass varies considerably across different progenitors, ranging from $\sim \! 10^{-8} \, \rm M_\odot$ in compact stars, up to $\sim \! 10^{-2} \, \rm M_\odot$ in red supergiants. We discuss implications of our results for pre-supernova outbursts driven by wave heating, and complications caused by the non-constant opacity and adiabatic index of realistic stars.
