AI 中文总结
研究 GRB 211211A 瞬时辐射，在轻子辐射框架内用 LeHaMoC计算模型并经马尔可夫链蒙特卡罗拟合，成功再现其10 keV到10 MeV辐射，揭示发射区物理及粒子分布演化，还预测了TeV能量辐射及高多普勒因子情况。
AI 中文摘要
GRB 211211A 是一个源于致密天体合并的长持续时间伽马射线暴。本文在轻子辐射框架内对 GRB 211211A 的时间分辨瞬时辐射光谱进行建模。目标是推断发射区域的物理性质，研究辐射粒子分布的时间演化，并预测 TeV 能量下的瞬时辐射。通过马尔可夫链蒙特卡罗方法对用 LeHaMoC 计算的时间分辨数值光谱能量分布模型进行拟合。计算包括同步辐射和自吸收、逆康普顿散射以及光子 - 光子对产生。结果表明 10 keV 到 10 MeV 之间的瞬时辐射可由相对论电子的同步辐射成功再现，爆发开始一分钟内的光谱演化反映发射区域不同物理条件。最佳拟合模型显示前 8 秒倾向快速冷却解，随后转变为慢速冷却解。同步自康普顿辐射延伸到 TeV 能量。此次爆发观测到的短时间变化需要整个爆发演化过程中具有非常高的多普勒因子（约 1000 - 2500）。
英文摘要
GRB 211211A is a long duration gamma-ray burst with a compact object merger origin. In this work, we model the time-resolved prompt-emission spectra of GRB 211211A within a leptonic radiation framework. Our goal is to infer the physical properties of the emitting region, study the temporal evolution of the radiating particle distribution, and make predictions for prompt emission at TeV energies. We perform Markov Chain Monte Carlo fitting of the time-resolved numerical spectral energy distribution (SED) models computed with the time-dependent non-thermal radiation code LeHaMoC. Our calculations include synchrotron emission and self-absorption, inverse Compton scattering including cooling in the Klein-Nishina regime, and photon-photon pair production. We find that the prompt emission of GRB 211211A between 10 keV and 10 MeV can be successfully reproduced by synchrotron radiation from a population of relativistic electrons. The spectral evolution during the first minute of the burst reflects different physical conditions in the emitting region. Our best-fit models favor fast-cooling solutions for the first 8 s, followed by a transition to slow-cooling solutions at later times. The accompanying synchrotron self-Compton emission extends to TeV energies, with predicted fluxes that would be detectable by CTAO for a burst similar to GRB 211211A, provided a sufficiently rapid response to a Fermi-GBM trigger or if the burst occurs within the CTAO field of view. The observed short variability of this burst requires very high Doppler factors ($\sim1000-2500$) throughout the burst evolution. Such extreme Doppler factors are difficult to reconcile with the jet Lorentz factor inferred from afterglow modeling unless the prompt-emitting regions are themselves moving relativistically with respect to the jet plasma.
Comments16 pages, 11 figures, submitted to A&A
