Possible X-ray Cocoon Emission from GRB 050709

Naoki Ogino; Makoto Arimoto; Hamid Hamidani; Takanori Sakamoto; Daisuke Yonetoku; Tatsuya Sawano; Motoko Serino; Katsuaki Asano; Nobuyuki Kawai

arXiv · 2404.02627

Possible X-ray Cocoon Emission from GRB 050709

Naoki Ogino·Makoto Arimoto·Hamid Hamidani·Takanori Sakamoto·Daisuke Yonetoku·Tatsuya Sawano·Motoko Serino·Katsuaki Asano·Nobuyuki Kawai

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Abstract

The detection of the short gamma-ray burst (SGRB) 050709 by the HETE-2 satellite opened a new window into understanding the nature of SGRBs, offering clues about their emission mechanism and progenitors, with the crucial aid of optical follow-up observations. Here, we revisit the prompt emission of GRB 050709. Our analysis reveals an initial hard spike ~200 ms long, followed by a subsequent soft tail emission lasting ~300 ms. These components could be common among other SGRBs originating from binary neutron merger events, such as GW/GRB 170817A. Detailed temporal and spectral analyses indicate that the soft tail emission might be attributed to the cocoon formed by the relativistic jet depositing energy into the surrounding material. We find the necessary cocoon parameters at the breakout, as consistent with numerical simulation results. We compared the physical parameters of this cocoon with those of other SGRBs. The relatively higher cocoon pressure and temperature in GRB 050709 may indicate a more on-axis jet compared to GRB 170817A and GRB 150101B.

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Naoki Ogino, Makoto Arimoto, Hamid Hamidani, Takanori Sakamoto, Daisuke Yonetoku, Tatsuya Sawano, Motoko Serino, Katsuaki Asano, Nobuyuki Kawai. 2024-04-03. Possible X-ray Cocoon Emission from GRB 050709. https://arxiv.org/abs/2404.02627

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