论文标题
敏捷光学对应物的特性是由伽马射线中电子冷却产生的
Properties of the Prompt Optical Counterpart Arising from the Cooling of Electrons in Gamma-Ray Bursts
论文作者
论文摘要
这项工作扩展了同时的努力（Panaitescu＆vestrand 2022），以研究通过相对论性伽马射线爆发（GRB）电子通过辐射（同步器和自发和自发性）的排放和准确损失的相对论伽马射线爆发（GRB）电子的冷却而产生的低能量对应物同步子发射的性能。 我们得出伴随GRB的迅速光学对应物（POC）的主要特征（脉冲持续时间，亮度相对于爆发的亮度，相对于爆发的亮度）。 根据磁场寿命，电子注入的持续时间以及从硬X射线（GRB）到光学发射能的电子传输时间DTO，在GRB脉冲（持续时间DTG）或之后（延迟OC）的GRB脉冲（持续时间）中可能会出现A（true）POC。由GRB电子冷却引起的对应物的特征是，真正的POC脉冲（DTO <dTG）持续到相应的GRB脉冲（DTO 〜DTG），而延迟的OC脉冲（DTO> dTG）持续使用，直到转运时间（DTO 〜DTO）。如果可以测量OC的可变性，那么该OC机制的另一个签名是GRB的可变性仅传递给POC，但对于延迟的OC丢失。在GRB电子冷却模型中，POC应平均比延迟一个（发现与数据一致的延迟）平均变暗，并且更难的Grb低能斜率应更频繁地与调光器POC相关联，低能斜坡的范围与[-1/2,1/2,1/3]中的低能斜率范围相关，并平均产生的（1/2,1/3）的含量（MISJ）（均为1，1/3]的elect colling（MOSJ）（均为1，1/2,,3）。分散表明，硬grb的POC可能比R = 20昏暗，并且难以通过机器人望远镜检测到（除非有另一种机制掩盖了来自冷却电子的发射），并且软grb的POC可以比R = 10的POC更明亮，即像光（Ofs ofs of Sers burs burs burs surbes）一样明亮。
This work extends a contemporaneous effort (Panaitescu & Vestrand 2022) to study the properties of the lower-energy counterpart synchrotron emission produced by the cooling of relativistic Gamma-Ray Burst (GRB) electrons through radiation (synchrotron and self-Compton) emission and adiabatic losses. We derive the major characteristics (pulse duration, lag-time after burst, brightness relative to the burst) of the Prompt Optical Counterpart (POC) accompanying GRBs. Depending on the magnetic field life-time, duration of electron injection, and electron transit-time Dto from hard X-ray (GRB) to optical emitting energies, a (true) POC may appear during the GRB pulse (of duration dtg) or after (delayed OC). The signature of counterparts arising from the cooling of GRB electrons is that true POC pulses (Dto < dtg) last as long as the corresponding GRB pulse (dto ~ dtg) while delayed OC pulses (Dto > dtg) last as long as the transit-time (dto ~ Dto). If OC variability can be measured, then another signature for this OC mechanism is that the GRB variability is "passed" only to POCs but is lost for delayed OCs. Within the GRB electron cooling model for counterparts, POCs should be on average dimmer than delayed one (which is found to be consistent with the data), and harder GRB low-energy slopes bLE should be associated more often with the dimmer POCs The range of low-energy slopes bLE in [-1/2,1/3] produced by electron cooling and the average burst brightness of 1 mJy (with 1 dex dispersion) imply that POCs of hard GRBs can be dimmer than R=20 and difficult to detect by robotic telescopes (unless there is another mechanism that overshines the emission from cooling electrons) and that the POCs of soft GRBs can be brighter than R=10, i.e. as bright as the Optical Flashes (OFs) seen for several bursts.
