论文标题
同步加速器自及余粒闭合关系和费米 - 拉特检测到伽马射线爆发
Synchrotron Self-Compton Afterglow Closure Relations and Fermi-LAT Detected Gamma-Ray Bursts
论文作者
论文摘要
费米大面积望远镜（Fermi-LAT）协作报告了第二伽玛射线爆发目录（2FLGC），该目录包括29次爆发的子集，光子能量超过10 GEV。尽管标准的同步器向前震模模型成功地解释了伽马射线爆发（GRB）恒星观测值，但在这种情况下，几乎无法描述来自这些瞬态事件的10 GEV的能量光子。我们介绍了绝热和辐射场景中的同步加速器自compton（SSC）余潮模型的封闭关系（CRS），当中央发动机将连续的能量注入BlastWave中，以研究2FLGC中这些爆发的光谱和时间指数的演变。我们将SSC余辉模型在恒星和星际介质中演变，而CRS则是辐射参数，能量注入指数和电子光谱指数的函数，价格为$ 1 <p <2 $和$ 2 \ 2 \ leq p $。我们选择了在2FLGC中使用简单或损坏的功率定律建模的所有GRB。我们发现，即使那些需要中间密度剖面（例如GRB 130427A）或用于放大磁场的总能量（例如，$ \ \ varepsilon_b $），SSC模型的CR可以满足在同步加速器场景中无法解释的大量突发的大部分。当冷却频谱中断对应于grb Afterglow的典型值时，SSC模型中此参数的值（$ \ varepsilon_b \ of 10^{ - 5} -5} - 10^{ - 4} $）对应于Fermi-lat频段。分析表明，对于没有能量注入的情况，ISM是首选的，而对于能量注入方案而言，ISM是恒星风介质。
The Fermi Large Area Telescope (Fermi-LAT) Collaboration reported the Second Gamma-ray Burst Catalog (2FLGC), which comprises a subset of 29 bursts with photon energies above 10 GeV. Although the standard synchrotron forward-shock model has successfully explained the Gamma-ray burst (GRB) afterglow observations, energetic photons higher than 10 GeV from these transient events can hardly be described in this scenario. We present the closure relations (CRs) of synchrotron self-Compton (SSC) afterglow model in the adiabatic and radiative scenario and when the central engine injects continuous energy into the blastwave to study the evolution of the spectral and temporal indexes of those bursts reported in 2FLGC. We consider the SSC afterglow model evolving in stellar-wind and interstellar medium, and the CRs as a function of the radiative parameter, the energy injection index, and the electron spectral index for $1<p<2$ and $ 2\leq p$. We select all GRBs that have been modeled with both a simple or a broken power law in the 2FLGC. We found that the CRs of the SSC model can satisfy a significant fraction of burst that cannot be interpreted in the synchrotron scenario, even though those that require an intermediate density profile (e.g., GRB 130427A) or an atypical fraction of total energy given to amplify the magnetic field ($\varepsilon_B$). The value of this parameter in the SSC model ranges ($\varepsilon_B\approx 10^{-5} - 10^{-4}$) when the cooling spectral break corresponds to the Fermi-LAT band for typical values of GRB afterglow. The analysis shows that ISM is preferred for the scenario without energy injection and the stellar wind medium for an energy injection scenario.
