AI 中文总结
本研究针对红移z=4.61的高能量GRB 220101A，提出双二元驱动超巨新星（BdP-N）模型，解释其7个能量阶段的起源，揭示其由两次间隔3.5秒的超新星触发的物理机制。
AI 中文摘要
GRB 220101A是一个长伽马射线暴（long GRB），其总能量超过10^54 erg，红移量z=4.61，拥有迄今为止最大规模的高质量多波段观测覆盖，来自大量天基和地基望远镜。我们用双二元驱动的超巨新星（doubly Binary driven peta nova，BdP-N）模型解释该源。其前身由质量约10倍太阳质量（~10 M☉）、磁场强度约10^6 G的高度磁化大质量碳氧（CO）核心，以及中子星（NS）和白矮星（WD）组成，三者的轨道周期从数分钟到数小时不等。该伽马射线暴的高光度可通过7个连续爆发阶段解释：第1阶段由一种新型对超新星（pair supernova，HB）触发，该超新星源于强磁化CO核心的坍缩；HB超新星的抛射物（ejecta）吸积到白矮星伴星上，3.5秒后触发第2阶段，即发射中微子并形成新中子星（νNS）的第二次超新星；抛射物与二元中子星伴星的磁层相互作用产生第3阶段——超相对论瞬时辐射（Ultra relativistic Prompt Emission，UPE），这是该伽马射线暴中能量最高的阶段，形成了垂直于伽马射线暴平面的强大喷流；UPE能量损失后，抛射物吸积到中子星伴星上导致第4阶段形成2.3倍太阳质量（2.3 M☉）的黑洞（BH），进而产生观测到的GeV余辉辐射；抛射物的进一步吸积将νNS自旋加速至1.3毫秒的周期，从而产生第5阶段——脉冲星的诞生；该毫秒脉冲星与抛射物遗迹的相互作用导致第6阶段——在X射线、光学和射电波段观测到的同步辐射；第7阶段是一个周期为56.7毫秒的脉冲星，于首次爆发后10^10秒在蟹状星云中被观测到。
英文摘要
GRB 220101A is a long GRB, with a total energy exceeding $10^{54}$ erg with a redshift $z = 4.61$ and one of the largest ever high-quality multi-wavelength observational coverage, from a large number of space-based and ground-based telescopes. We interpret this source in a doubly Binary driven peta nova (BdP-N) model. The progenitor is composed of a massive CO core of $\sim 10\,M_\odot$, highly magnetized with $B \sim 10^{6}$ G, associated to a neutron star (NS) and a white dwarf (WD) with orbital periods from minutes to hours. The large GRB luminosity is explained by a sequence of 7 episodes: episode 1 is triggered by a new kind of pair supernova (HB) which originates from the collapse of the strongly magnetized CO core. Accretion of the HB supernova ejecta (the ejecta) onto the white dwarf companion triggers after 3.5 sec the episode 2: the second supernova emitting neutrinos and creating a new neutron star ($ν$NS). The ejecta, interacting with the magnetosphere of the binary NS companion originate the episode 3: the Ultra relativistic Prompt Emission (UPE) emission by far the most energetic episode of this GRB, with the formation of a powerful jet normal to the plane of the GRB. Following the UPE energy loss, the accretion of the ejecta on the NS companion leads to the episode 4: the formation of a black hole (BH) of $2.3 \ M_\odot$ leading to the observed GeV afterglow emission. Further accretion of the ejecta spin up the $ν$NS to a period of $1.3$ ms which gives origin to the episode 5: the birth of a pulsar. The interaction of this milli-second pulsar with the remnants lead to the Episode 6: the synchrotron emission observed in the X-ray, optical and radio, The episode 7 is a 56.7 ms pulsar, as observed $10^{10}$ s after the first burst in the crab nebula.
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