可能的GRB祖先的磁旋转核心坍塌。II。原磁星和磁星的形成
Magnetorotational core collapse of possible GRB progenitors. II. Formation of protomagnetars and collapsars
摘要：
我们评估的紧凑，大质量，低金属含量的恒星，在选定的前超新星核心的旋转和磁场的程度的微小变化的崩溃后的演化残余物的方差。这些恒星模型通常被认为是长伽马射线暴的祖先。坍缩后形成的原中子星（PNS），其质量可能由于吸积而不断增长，其命运关键取决于反弹时的极向磁场强度。如果极向磁场足够弱，PNS会在几秒钟内坍缩成黑洞（BH）。在这条进化轨道上的模型包含有前途的BMSAR引擎。极向磁场在大的径向尺度上平滑（例如偶极场），或者相对于原始的超新星前核心稍微增强，产生持久的PNS。在这些模型中，BH的形成被避免或推迟了很长一段时间，因此，它们可能会产生原磁星（PM）。我们的一些PM候选人已经在核心反弹后运行了$\lesssim 10\,$ s，但他们还没有进入开尔文-亥姆霍兹阶段。在这些模型中，一些显示出自旋下降的偶发事件，在此期间，我们发现PM（$M_{PNS} \approx 1.85\,M_\odot - 2.5\,M_\odot$，$\bar{P}_{PNS} \approx 1.5 - 4\,$ ms和$b^{\rm surf}_{PNS} \lesssim 10^{15}\,$ G）的理论预期与性能广泛兼容，并且它们非常准直的超新星喷出物几乎到达恒星表面，爆炸能量（仍在增长）$\gtrsim 2\times 10^{51}\,$ erg。
英文摘要：
We assess the variance of the post-collapse evolution remnants of compact, massive, low-metallicity stars, under small changes in the degrees of rotation and magnetic field of selected pre-supernova cores. These stellar models are commonly considered progenitors of long gamma-ray bursts. The fate of the proto-neutron star (PNS) formed after collapse, whose mass may continuously grow due to accretion, critically depends on the poloidal magnetic field strength at bounce. Should the poloidal magnetic field be sufficiently weak, the PNS collapses to a black hole (BH) within a few seconds. Models on this evolutionary track contain promising collapsar engines. Poloidal magnetic fields smooth over large radial scales (e.g. dipolar fields) or slightly augmented with respect to the original pre-supernova core yield long-lasting PNSs. In these models, BH formation is avoided or staved off for a long time, hence, they may produce proto-magnetars (PMs). Some of our PM candidates have been run for $\lesssim 10\,$s after core bounce, but they have not entered the Kelvin-Helmholtz phase yet. Among these models, some display episodic events of spin-down during which we find properties broadly compatible with the theoretical expectations for PMs ($M_{PNS} \approx 1.85\,M_\odot - 2.5\,M_\odot$, $\bar{P}_{PNS} \approx 1.5 - 4\,$ms, and $b^{\rm surf}_{PNS} \lesssim 10^{15}\,$G) and their very collimated supernova ejecta has nearly reached the stellar surface with (still growing) explosion energies $\gtrsim 2\times 10^{51}\,$erg.
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