论文标题
GRB非常高能量排放190114c的质子同步加速器起源
Proton Synchrotron Origin of the Very High Energy Emission of GRB 190114C
论文作者
论文摘要
我们在这里考虑质子合成的模型，以解释能量带中Grb 190114c余辉的魔术观察$ 0.2-1 $ 〜TEV，而X射线光谱则通过电子合成支出发射来解释。考虑到粒子加速过程的不确定性，我们考虑了模型的几种变化，并表明它们都很好地匹配了数据。我们发现，不确定模型参数的值是合理的：{isotropic}爆炸能量$ \ sim 10^{54.5} $ 〜ERG，环境密度$ \ sim 10-100〜 {\ rm cm^{ - 3}} $，以及对电子/质子质量加速对高能量律师的加速级数。所有这些值直接源自观察到的TEV和X射线通量。该模型还要求将质子加速到观测到的能量高达几美元$ 10^{20} $ 〜EV。此外，假设喷气间断是在$ 10^6 $ 〜s之后进行的，则可以使爆发的光束校正的能量为$ \ \ \ \ 10^{53} $ 〜ERG，这是比平常高的数量级，由于电子的一小部分加速。我们的建模与从光学到X射线以及粒子加速度的数值模型的所有频段的较晚时间数据一致。因此，我们的结果证明了质子同步发射与GRB在余波阶段中GRB的高能量观察的相关性。
We consider here a proton-synchrotron model to explain the MAGIC observation of GRB 190114C afterglow in the energy band $0.2 - 1$~TeV, while the X-ray spectra are explained by electron-synchrotron emission. Given the uncertainty of the particle acceleration process, we consider several variations of the model, and show that they all match the data very well. We find that the values of the uncertain model parameters are reasonable: {isotropic} explosion energy $\sim 10^{54.5}$~erg, ambient density $\sim 10-100~{\rm cm^{-3}}$, and fraction of electrons/protons accelerated to a high energy power law of a few per-cents. All these values are directly derived from the observed TeV and X-ray fluxes. The model also requires that protons be accelerated to observed energies as high as a few $10^{20}$~eV. Further, assuming that the jet break takes place after $10^6$~s gives the beaming-corrected energy of the burst to be $\approx 10^{53}$~erg, which is one to two orders of magnitude higher than usually inferred, because of the small fraction of electrons accelerated. Our modeling is consistent with both late time data at all bands, from optical to X-rays, and with numerical models of particle acceleration. Our results thus demonstrate the relevance of proton-synchrotron emission to the high energy observations of GRBs during their afterglow phase.
