论文标题
远处伽玛射线BUSRT GRB 201216c的非常高能量排放的时间依赖性数值模型
Time dependent numerical model for the very high energy emissions of distant gamma-ray busrt GRB 201216C
论文作者
论文摘要
最近，魔术合作报告了$ \ sim5σ$统计显着性（从遥远的GRB，GRB 201216c发出）发射的统计意义（VHE）。这种遥远的GRB可以通过乳乳外背景光（EBL）有效地吸收。从这种遥远的物体发射的VHE发射的起源仍然未知。在这里，我们提出了一个数值模型，用于研究此遥远的GRB的余辉发射。该模型求解了管理电子分布时间演变的连续性方程，并且可以通过synchrotron Plus Synchrotron Self-Compton（SSC）辐射的宽带观察到的数据来解释。预测的0.1 TEV通量可以达到$ \ sim 10^{ - 9} -10^{ - 10} \ rm erg〜cm^{ - 2} 〜s^{ - 1} $ at $ t \ sim 10^3 -10^3 -10^4 \ rm S $，即使具有强大的EBL吸收，也可以通过强烈的sib-temions观察到了强大的EBL吸收。使用此数值模型，模型中的冲击参数与其他两个子TEV GRB相似（即GRB 190114C和GRB 180720b），这意味着子TEV GRB具有一些共同点：它们具有充满活力的爆发能量，低圆形爆发能量，低圆螺旋中型中等密度和低磁均衡因子。我们将GRB 201216C视为典型的GRB，并估计GRB的最大红移可以通过魔术望远镜检测到，即$ z \ sim 1.6 $。我们还发现，这种遥远的GRB的VHE光子能量只能达到$ \ sim 0.1〜 \ rm tev $。提高VHE望远镜的低能灵敏度对于检测这些遥远GRB的子TEV排放非常重要。
Recently, the MAGIC Collaboration reported a $\sim 5σ$ statistical significance of the very-high-energy (VHE) emission from a distant GRB, GRB 201216C. Such distant GRB may be effectively absorbed by the extragalactic background light (EBL). The origin of the VHE emission from such distant objects is still unknown. Here, we propose a numerical model for studying the afterglow emission of this distant GRB. The model solves the continuity equation governing the temporal evolution of electron distribution, and the broad-band observed data can be explained by the synchrotron plus synchrotron self-Compton (SSC) radiation of the forward shock. The predicted observed 0.1 TeV flux can reach $\sim 10^{-9} -10^{-10}\rm erg ~ cm^{-2} ~ s^{-1}$ at $t \sim 10^3 -10^4 \rm s$, even with strong EBL absorption, such strong Sub-TeV emissions still can be observed by MAGIC telescope. Using this numerical model, the shock parameters in the modeling are similar with two other Sub-TeV GRBs (i.e., GRB 190114C and GRB 180720B), implying that the Sub-TeV GRBs have some commonalities: they have energetic burst energy, low circum-burst medium density and low magnetic equipartition factor. We regard GRB 201216C as a typical GRB, and estimate the maximum redshift of GRB that can be detected by MAGIC telescope, i.e., $z \sim 1.6$. We also find that the VHE photon energy of such distant GRB can only reach $\sim 0.1 ~\rm TeV$. Improving the low energy sensitivity of the VHE telescope is very important to detect the Sub-TeV emissions of these distant GRBs.
