用中微子驱动机制划分大质量恒星爆炸性的双参数判据
A two-parameter criterion for classifying the explodability of massive stars by the neutrino-driven mechanism
摘要：
到目前为止，仅仅根据大质量恒星（中子星（NS）或黑洞）在核心坍缩之前的结构来判断它的命运还很模糊。我们的工作和以前的尝试发现一个非单调变化的成功和失败的超新星与零年龄的主序质量，没有一个单一的结构参数可以作为一个很好的预测措施。然而，我们确定了两个参数计算的前坍缩结构的祖先，这在组合允许一个明确的分离爆炸和非爆炸的情况下，只有少数例外（~1-2.5%），在我们的621个研究恒星模型。一个参数是M4，定义了每个核子的无量纲熵为s=4时的归一化封闭质量，另一个参数是在s=4时的mu 4 = d（m/M_sun）/d（r/1000 km），是该位置的归一化质量导数。这两个参数μ 4和M4* μ 4与坍缩恒星的质量下落率Mdot和吸积原NS的电子型中微子光度L_nue ~ M_ns*Mdot直接相关，它们在理论上描述中微子驱动的爆炸为停滞吸积激波逃逸现象的“临界光度”概念中起着至关重要的作用。所有的模型都是采用Ugliano等人的方法来模拟中微子驱动的球对称爆炸。吸积层的中微子发射用灰色输运方程近似，而1.1M太阳原NS核的不确定中微子发射用解析模型参数化。通过标定与核-边界条件相关联的自由参数，再现了5种不同的超新星前身模型的观测值。
英文摘要：
Thus far, judging the fate of a massive star (either a neutron star (NS) or a black hole) solely by its structure prior to core collapse has been ambiguous. Our work and previous attempts find a non-monotonic variation of successful and failed supernovae with zero-age main-sequence mass, for which no single structural parameter can serve as a good predictive measure. However, we identify two parameters computed from the pre-collapse structure of the progenitor, which in combination allow for a clear separation of exploding and non-exploding cases with only few exceptions (~1-2.5%) in our set of 621 investigated stellar models. One parameter is M4, defining the normalized enclosed mass for a dimensionless entropy per nucleon of s=4, and the other is mu4 = d(m/M_sun)/d(r/1000 km) at s=4, being the normalized mass-derivative at this location. The two parameters mu4 and M4*mu4 can be directly linked to the mass-infall rate, Mdot, of the collapsing star and the electron-type neutrino luminosity of the accreting proto-NS, L_nue ~ M_ns*Mdot, which play a crucial role in the "critical luminosity" concept for the theoretical description of neutrino-driven explosions as runaway phenomenon of the stalled accretion shock. All models were evolved employing the approach of Ugliano et al. for simulating neutrino-driven explosions in spherical symmetry. The neutrino emission of the accretion layer is approximated by a gray transport solver, while the uncertain neutrino emission of the 1.1 M_sun proto-NS core is parametrized by an analytic model. The free parameters connected to the core-boundary prescription are calibrated to reproduce the observables of Supernova 1987A for five different progenitor models.
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