标题： 脉冲星风气泡中的伽马射线暴：拼凑出完整图景 显示英文标题

标题： Gamma-Ray Bursts in Pulsar Wind Bubbles: Putting the Pieces Together

摘要： 我们提出了预期出现在脉冲星风泡（PWBs）内的伽马射线暴（GRBs）的主要观测特征。 这是超新星模型中最自然的结果，在该模型中最初发生一次超新星爆炸，留下一个超大质量中子星，它在时间t_sd内失去旋转能量并坍缩为黑洞，触发伽马射线暴爆炸。 我们发现超新星和伽马射线暴事件之间的时间延迟t_sd是决定系统行为的最重要参数。 我们考虑了后火球辐射、伽马射线暴瞬时辐射以及来自PWB的直接辐射。 描述了不同t_sd值下的观测特征，并将其整合到一个连贯的框架中。 通过对球形PWB的约束条件从PWB发射和后火球观测未被探测到的情况中得出。 对于非常低的t_sd<1小时值，超新星模型退化为坍缩星模型；0.4<t_sd/1年<1是产生一些X射线后火球中看到的铁线所必需的。 然而，我们发现对于球形PWB，这意味着没有可检测到的射电后火球，小喷流断裂时间和非相对论转变时间，与一些这些伽马射线暴的观测结果不符。 这些与观测结果的差异可能通过采用非球形几何来调和。 我们发现，最近在几个X射线后火球中检测到的轻元素线，在小t_sd下预计会占主导地位，而在大t_sd情况下则相反。 最后，我们预测脉冲星风泡光子由后火球相对论电子外部康普顿散射应该在早期后火球期间导致高能发射，这可以解释EGRET在一些伽马射线暴中检测到的GeV光子，并且应该可以通过未来的任务（GLAST）检测到。 显示英文摘要

摘要： We present the main observational features expected for GRBs that occur inside pulsar wind bubbles (PWBs). This is the most natural outcome of supranova model where initially a supernova explosion takes place, leaving a supra-massive NS, which loses its rotational energy over a time t_sd and collapses to a BH, triggering a GRB explosion. We find that the time delay t_sd between the supernova and GRB events is the most important parameter that determines the behavior of the system. We consider the afterglow, prompt GRB and direct emission from the PWB. The observational signatures for different t_sd are described and joined together into one coherent framework. Constraints on the model are derived for a spherical PWB, from the lack of detection of the PWB emission and afterglow observations. For very low values of t_sd<1 hr the supranova model reduces to the collapsar model; 0.4<t_sd/1yr<1 is required to produce the iron lines seen in some X-ray afterglows. However, we find that for a spherical PWB, this implies no detectable radio afterglow, a small jet break time and non-relativistic transition time, in disagreement with observations for some of these GRBs. These discrepancies with the observations may be reconciled by resorting to a non-spherical geometry. We find that light element lines, recently detected in a few X-ray afterglows, are expected to dominate over iron lines for small t_sd, while for large t_sd the situation is reversed. Finally, we predict that external Compton scattering of the PWB photons by the afterglow relativistic electrons, should lead to high energy emission during the early afterglow that may explain the GeV photons detected by EGRET in some GRBs, and should be detectable by future missions (GLAST).