论文标题
GRB及时排放的极化及其在Polar的数据中的应用
Polarization of GRB Prompt Emission and its Application to POLAR's Data
论文作者
论文摘要
同步加速器发射极化对磁场构型非常敏感。最近，已经开发出具有混合（SM）磁场在伽马射线爆发（GRB）余旋相中具有混合（SM）磁场的极化。在这里，我们将这些SM模型应用于GRB及时阶段，并将其极化特性与纯粹有序（SO）磁场中的同步加速器发射的偏振特性进行比较。我们发现，在相应的SO模型中，SM模型中的极化特性与这些模型非常相似（例如，在具有排列有序零件（SMA）的混合磁场中发射（SMA）和具有纯粹有序的对齐磁场（SOA）的同步磁场的发射），仅具有较低的极性度（PD）。我们还讨论了模型的统计特性。我们发现，模拟爆发的PDS集中在SOA和同步器在纯粹有序的环形磁场（SOT）中的$ 25 \％$ $ \％$左右，而它们的$ 0 \％$ $ \％$ $ \％$ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ actection $ collition $ yirial copte $ $ actection n.随机磁场的有序磁场。从统计数据中，如果大多数GRB的PDS是非零的，则它有利于SO和SM模型。此外，如果有一些明亮的GRB，其PD较大的GRB比大多数GRB的PD低，则会有利于SOT（SMT）模型。如果所有明亮的GRB与大多数PD都具有可比性的PD，则它有利于SOA（SMA）模型。最后，我们将结果应用于Polar的数据，并发现观察到的爆发的$ \ sim10 \％$ time集成的PDS有利于SMA和SMT型号，而这些爆发的$ξ_b$参数限制为约1.135。
Synchrotron emission polarization is very sensitive to the magnetic field configuration. Recently, polarization of synchrotron emission with a mixed (SM) magnetic field in Gamma-ray burst (GRB) afterglow phase had been developed. Here, we apply these SM models to GRB prompt phase and compare their polarization properties with that of synchrotron emission in purely ordered (SO) magnetic field. We find that the polarization properties in a SM model are very similar to these in a corresponding SO model (e.g., synchrotron emission in a mixed magnetic field with an aligned ordered part (SMA) and synchrotron emission with a purely ordered aligned magnetic field (SOA)), only with a lower polarization degree (PD). We also discuss the statistical properties of the models. We find PDs of the simulated bursts are concentrated around $25\%$ for both SOA and synchrotron emission in a purely ordered toroidal magnetic field (SOT), while they can range from $0\%$ to $25\%$ for SMA and synchrotron emission in a mixed magnetic field with a toroidal ordered part (SMT), depending on $ξ_B$ value, i.e., the ratio of magnetic reduction of the ordered magnetic field over that of random magnetic field. From statistics, if PDs of majority GRBs are non-zero, then it favours SO and SM models. Further, if there are some bright GRBs with a prominently lower PDs than that of the majority GRBs, it favours SOT (SMT) models; if all the bright GRBs have comparable PDs with the majority ones, it favours SOA (SMA) models. Finally, we apply our results to POLAR's data and find that $\sim10\%$ time-integrated PDs of the observed bursts favor SMA and SMT models, and $ξ_B$ parameter of these bursts is constrained to be around 1.135.
