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A peculiarly short-duration gamma-ray burst from massive star core collapse
Nature Astronomy ( IF 14.1 ) Pub Date : 2021-07-26 , DOI: 10.1038/s41550-021-01395-z
B.-B. Zhang 1, 2, 3 , Z.-K. Liu 1, 2 , Z.-K. Peng 1, 2 , J. Yang 1, 2 , Y.-S. Yang 1, 2 , Y.-H. Yang 1, 2 , Y.-Z. Meng 1, 2 , J.-H. Zou 1, 2, 4 , H.-Y. Ye 1 , Z.-G. Dai 1, 2, 5 , B. Zhang 3 , Y. Li 6, 7 , H.-J. Lü 8 , X.-G. Wang 8 , E.-W. Liang 8 , J.-R. Mao 9 , X.-H. Zhao 9 , J.-M. Bai 9 , A. J. Castro-Tirado 10, 11 , Y.-D. Hu 10, 12
Affiliation  

Gamma-ray bursts (GRBs) have been phenomenologically classified into long and short populations based on the observed bimodal distribution of duration1. Multi-wavelength and multi-messenger observations in recent years have revealed that in general long GRBs originate from massive star core collapse events2, whereas short GRBs originate from binary neutron star mergers3. It has been known that the duration criterion is sometimes unreliable, and multi-wavelength criteria are needed to identify the physical origin of a particular GRB4. Some apparently long GRBs have been suggested to have a neutron star merger origin5, whereas some apparently short GRBs have been attributed to genuinely long GRBs6 whose short, bright emission is slightly above the detector’s sensitivity threshold. Here, we report the comprehensive analysis of the multi-wavelength data of the short, bright GRB 200826A. Characterized by a sharp pulse, this burst shows a duration of 1 second and no evidence of an underlying longer-duration event. Its other observational properties such as its spectral behaviours, total energy and host galaxy offset are, however, inconsistent with those of other short GRBs believed to originate from binary neutron star mergers. Rather, these properties resemble those of long GRBs. This burst confirms the existence of short-duration GRBs with stellar core-collapse origin4, and presents some challenges to the existing models.



中文翻译:

来自大质量恒星核心坍缩的特别短持续时间的伽马射线爆发

伽马射线暴 (GRB) 已根据观察到的持续时间1的双峰分布在现象学上分为长群体和短群体。近年来的多波长和多信使观测表明,一般来说,长伽马暴起源于大质量星核坍缩事件2,而短伽马暴则起源于双中子星合并3。众所周知,持续时间标准有时是不可靠的,需要多波长标准来识别特定 GRB 4的物理起源。一些明显长的 GRB 被认为是中子星合并起源5,而一些明显短的 GRB 被认为是真正的长 GRB 6其短暂而明亮的发射略高于探测器的灵敏度阈值。在这里,我们报告了对短而明亮的 GRB 200826A 的多波长数据的综合分析。该爆发以尖锐脉冲为特征,持续时间为 1 秒,没有证据表明潜在的持续时间较长的事件。然而,它的其他观测特性,如光谱行为、总能量和宿主星系偏移,与其他被认为源自双中子星合并的短 GRB 的特性不一致。相反,这些特性类似于长 GRB 的特性。这次爆发证实了恒星核心坍缩起源的短时伽马暴的存在4,并对现有模型提出了一些挑战。

更新日期:2021-07-26
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