论文标题
伽马射线爆发及时发射的光球发射起源的证据
Evidence of Photosphere Emission Origin for Gamma-Ray Burst Prompt Emission
论文作者
论文摘要
五十年后，伽马射线爆发（GRB）提示发射（Photosphere或Synchrotron）的物理起源仍可能存在争议。在这里，首先，我们发现许多观察到的15个长GRB的特征，它们具有最高的及时发射效率$ε_γ$（$ε________{γ} \ gtrsim 80 \％$），强烈支持Photoshere（热）发射起源：（1）$ $ e _ {\ text {p}} \ propto（e _ {\ text {iso}}）^{1/4} $，并且分散体很小； （2）X射线余辉光曲线的简单幂律形状和光余波光曲线中的显着反向冲击信号； （3）按时间集成频谱截止幂律模型最适合的； （4）观察的一致效率（使用$ e _ {\ text {iso}}/e_ {k} $）和Photoshere发射模型的预测（带有$η/γ$）。然后，我们进一步研究了两个杰出样品的长GRB的特征（$ε_{γ} \ gtrsim 50 \％$和$ε_{γ} \ sillesim 50 \％$）。 It is found that the different distributions for $E_{\text{p}}$ and $E_{\text{iso}}$, and the similar observed efficiency (from the X-ray afterglow) and theoretically predicted efficiency (from the prompt emission or the optical afterglow) well follow the prediction of photosphere emission model.另外，基于相同的效率，我们得出了$γ\ propto e _ {\ text {iso}}}^{1/8} e _ {\ text {p}}^{1/2}/（t_ {90}）^{1/4} $ astimate $ umate $γ$的极好的相关性。最后，$ e _ {\ text {p}} $和$ e _ {\ text {iso}} $的不同分布，并且短grbs存在一致的效率。此外，我们对扩展发射（$ε_{γ} \ Lessim 50 \％$）和主脉冲（$ε_{γ} \ gtrsim 50 \％$）进行自然解释。
The physical origin of gamma-ray burst (GRB) prompt emission (photosphere or synchrotron) is still subject to debate after five decades. Here, firstly we find that many observed characteristics of 15 long GRBs, which have the highest prompt emission efficiency $ε_γ$ ($ε_{γ}\gtrsim 80\%$), strongly support the photosphere (thermal) emission origin: (1) the relation between $E_{\text{p}}$ and $E_{\text{iso}}$ is almost $E_{\text{p}}\propto (E_{\text{iso}})^{1/4}$ , and the dispersion is quite small; (2) the simple power-law shape of the X-ray afterglow light curves and the significant reverse shock signals in the optical afterglow light curves; (3) best-fitted by the cutoff power-law model for the time-integrated spectrum; (4) the consistent efficiency from observation (with $E_{\text{iso}}/E_{k}$) and the prediction of photosphere emission model (with $η/Γ$). Then, we further investigate the characteristics of the long GRBs for two distinguished samples ($ε_{γ}\gtrsim 50\%$ and $ε_{γ}\lesssim 50\%$). It is found that the different distributions for $E_{\text{p}}$ and $E_{\text{iso}}$, and the similar observed efficiency (from the X-ray afterglow) and theoretically predicted efficiency (from the prompt emission or the optical afterglow) well follow the prediction of photosphere emission model. Also, based on the same efficiency, we derive an excellent correlation of $Γ\propto E_{\text{iso}}^{1/8}E_{\text{p}}^{1/2}/(T_{90})^{1/4}$ to estimate $Γ$. Finally, the different distributions for $E_{\text{p}}$ and $E_{\text{iso}}$, and the consistent efficiency exist for the short GRBs. Besides, we give a natural explanation of the extended emission ($ε_{γ}\lesssim 50\%$) and the main pulse ($ε_{γ}\gtrsim 50\%$).
