论文标题
超高能量宇宙射线签名在GRB 221009a中
Ultrahigh-energy cosmic-ray signature in GRB 221009A
论文作者
论文摘要
迄今为止，由Swift-Bat和Fermi-GBM望远镜GRB〜221009A检测到的最明亮的长伽马射线爆发为理解极端短暂现象中的高能过程提供了前所未有的机会。我们发现，对于该来源的余旋发射，传统的Leptonic模型，同步器和同步型循环循环，很难解释$ \ gtrsim 10 $ \ gtrsim 10 $ \ gtrsim tev $γ$ rays，lhaaso检测器，并驱逐了多达18 tev envies。我们通过费米 - 拉特检测器在能量范围0.1-1 GEV估计的$γ$射线频谱进行建模。我们的Leptonic型号预测的通量严重减弱了$> 1美元的TEV，这是由于$γγ$ PAIR的生产带有外层次背景光，因此需要额外的组件，即$ \ gtrsim 10 $ tev。超高能量宇宙射线可以在GRB Blastwave中加速，它们的传播在外层状培养基中诱导电磁级联反应。这种通量的视线组成部分可以解释Lhaaso检测到的$ \ gtrsim 10 $ TEV的发射，需要超高能量宇宙射线中的GRB BlastWave Energy的一小部分。这可能表明GRB中超高能量宇宙射线加速度。
The brightest long gamma-ray burst detected so far by the Swift-BAT and Fermi-GBM telescopes, GRB~221009A, provides an unprecedented opportunity for understanding the high-energy processes in extreme transient phenomena. We find that the conventional leptonic models, synchrotron and synchrotron-self-Compton, for the afterglow emission from this source have difficulties explaining the observation of $\gtrsim 10$ TeV $γ$ rays, by the LHAASO detector, and extending up to 18 TeV energies. We model $γ$-ray spectrum estimated in the energy range 0.1-1 GeV by the Fermi-LAT detector. The flux predicted by our leptonic models is severely attenuated at $> 1$ TeV due to $γγ$ pair production with extragalactic background light, and hence an additional component is required at $\gtrsim 10$ TeV. Ultrahigh-energy cosmic rays can be accelerated in the GRB blastwave, and their propagation induces an electromagnetic cascade in the extragalactic medium. The line of sight component of this flux can explain the emission at $\gtrsim 10$ TeV detected by LHAASO, requiring a fraction of the GRB blastwave energy in ultrahigh-energy cosmic rays. This could be an indication of ultrahigh-energy cosmic-ray acceleration in GRBs.
