坍缩星模型的原中子星相和长软伽马射线暴和超新星的路径
The Proto-neutron Star Phase of the Collapsar Model and the Route to Long-soft Gamma-ray Bursts and Hypernovae
摘要：
最近的恒星演化计算的低金属丰度大质量快速旋转的主序星产生铁的核心在崩溃赋予高角动量。高角动量和黑洞的形成被认为是长软伽马射线暴（GRB）的Eksar模型的关键组成部分。在这里，我们提出了2D多组，通量限制扩散MHD模拟的崩溃，反弹，并立即反弹后阶段的35 Msun的Woosley & Heger的候选人模型。我们发现，磁旋转不稳定性（MRI）的毫秒周期中子星，磁驱动的爆炸englomerate在原中子星阶段，在重子加载的非相对论性喷流的形式，并没有形成的黑洞，中央的Eksar模型的表面层的微分旋转。巧合的是，尽管围绕恒星质量损失、角动量输运、磁场和磁共振成像的不确定性很大，但目前的低金属丰度化学均匀演化模型产生了具有铁核的大质量恒星，这些恒星可能有太多的角动量，无法避免在反弹后立即发生磁驱动的超超新星爆炸。我们推测，在铁的核心快速旋转可能会抑制，而不是使，双星的形成，这需要一个大的角动量不是在核心，但以上it. Variations在大质量恒星的角动量分布在核心坍缩可能解释的多样性Ic型超新星/hypernovae和他们可能与伽玛暴。一个推论可能是，通过角动量分布对磁场放大的影响，而不是原始质量来区分这些结果。
英文摘要：
Recent stellar evolutionary calculations of low-metallicity massive fast-rotating main-sequence stars yield iron cores at collapse endowed with high angular momentum. It is thought that high angular momentum and black hole formation are critical ingredients of the collapsar model of long-soft gamma-ray bursts (GRBs). Here, we present 2D multi-group, flux-limited-diffusion MHD simulations of the collapse, bounce, and immediate post-bounce phases of a 35-Msun collapsar-candidate model of Woosley & Heger. We find that, provided the magneto-rotational instability (MRI) operates in the differentially-rotating surface layers of the millisecond-period neutron star, a magnetically-driven explosion ensues during the proto-neutron star phase, in the form of a baryon-loaded non-relativistic jet, and that a black hole, central to the collapsar model, does not form. Paradoxically, and although much uncertainty surrounds stellar mass loss, angular momentum transport, magnetic fields, and the MRI, current models of chemically homogeneous evolution at low metallicity yield massive stars with iron cores that may have too much angular momentum to avoid a magnetically-driven, hypernova-like, explosion in the immediate post-bounce phase. We surmise that fast rotation in the iron core may inhibit, rather than enable, collapsar formation, which requires a large angular momentum not in the core but above it. Variations in the angular momentum distribution of massive stars at core collapse might explain both the diversity of Type Ic supernovae/hypernovae and their possible association with a GRB. A corollary might be that, rather than the progenitor mass, the angular momentum distribution, through its effect on magnetic field amplification, distinguishes these outcomes.
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