A burst in a wind bubble and the impact on baryonic ejecta: high-energy gamma-ray flashes and afterglows from fast radio bursts and pulsar-driven supernova remnants
A burst in a wind bubble and the impact on baryonic ejecta: high-energy gamma-ray flashes and afterglows from fast radio bursts and pulsar-driven supernova remnants
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DOI：
10.1093/mnras/stw1328
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发表时间：
2016-03
影响因子：
4.8
通讯作者：
K. Murase;K. Kashiyama;P. Mészáros
中科院分区：
文献类型：
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作者：
K. Murase;K. Kashiyama;P. Mészáros
细小的风泡是由中心致密残余物的自旋下降活动形成的，与快速射电爆发（FRB）和超亮超新星的一些模型有关。我们研究它们的高能特征，重点关注年轻磁星、快速旋转的中子星和磁化白矮星产生的成对富集气泡的作用。 (i) 首先，我们研究了星云的特性以及高能伽马射线和无线电波逃逸的条件，表明年龄 >10-100 年的星云有可能逃逸。在快速旋转的中子星场景中，我们发现来自准稳态星云本身的射电发射可能足够明亮，尤其是在亚毫米频率下，这可能是脉冲星驱动的超新星和快速射电暴的对应物。 (ii) 其次，我们考虑星云中爆发发射的命运。我们认为脉冲爆发可能会导致高度相对论性的流动，从而与星云相互作用。如果受到冲击的星云仍然是相对论性的，则星云中预先存在的非热粒子可能会因前向冲击而显着增强，从而导致短时（可能是毫秒或更长）的高能伽马射线闪光。反向冲击时可能的耗散也可能导致伽马射线发射。 (iii) 在此类耀斑之后，与重子喷射物的相互作用可能会导致持续数天至数周的余辉发射。在磁星场景中，这种气泡爆裂模型导致人们期望 HAWC 和 CTA 可以检测到附近（<10-100 Mpc）的高能伽马射线闪光，并且 VLA 等射电望远镜可以看到随后的余辉发射。 (iv) 最后，我们讨论了快速射电暴的几个具体含义，包括对发射区域的限制和对软伽马射线对应物的限制。
Tenuous wind bubbles, which are formed by the spin-down activity of central compact remnants, are relevant in some models of fast radio bursts (FRBs) and super-luminous supernovae. We study their high-energy signatures, focusing on the role of pair-enriched bubbles produced by young magnetars, rapidly-rotating neutron stars, and magnetized white dwarfs. (i) First, we study the nebular properties and the conditions allowing for escape of high-energy gamma-rays and radio waves, showing that their escape is possible for nebulae with ages of >10-100 yr. In the rapidly-rotating neutron star scenario, we find that radio emission from the quasi-steady nebula itself may be bright enough to be detected especially at sub-mm frequencies, which is relevant as a possible counterpart of pulsar-driven SNe and FRBs. (ii) Second, we consider the fate of bursting emission in the nebulae. We suggest that an impulsive burst may lead to a highly relativistic flow, which would interact with the nebula. If the shocked nebula is still relativistic, pre-existing non-thermal particles in the nebula can be significantly boosted by the forward shock, leading to short-duration (maybe millisecond or longer) high-energy gamma-ray flashes. Possible dissipation at the reverse shock may also lead to gamma-ray emission. (iii) After such flares, interactions with the baryonic ejecta may lead to afterglow emission with a duration of days to weeks. In the magnetar scenario, this burst-in-bubble model leads to the expectation that nearby (<10-100 Mpc) high-energy gamma-ray flashes may be detected by HAWC and CTA, and the subsequent afterglow emission may be seen by radio telescopes such as VLA. (iv) Finally, we discuss several implications specific to FRBs, including constraints on the emission regions and limits on soft gamma-ray counterparts.