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Tenuous wind bubbles, which are formed by the spin-down activity of centralcompact remnants, are relevant in some models of fast radio bursts (FRBs) andsuper-luminous supernovae. We study their high-energy signatures, focusing onthe role of pair-enriched bubbles produced by young magnetars, rapidly-rotatingneutron stars, and magnetized white dwarfs. (i) First, we study the nebularproperties and the conditions allowing for escape of high-energy gamma-rays andradio 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 radioemission from the quasi-steady nebula itself may be bright enough to bedetected especially at sub-mm frequencies, which is relevant as a possiblecounterpart of pulsar-driven SNe and FRBs. (ii) Second, we consider the fate ofbursting emission in the nebulae. We suggest that an impulsive burst may leadto a highly relativistic flow, which would interact with the nebula. If theshocked nebula is still relativistic, pre-existing non-thermal particles in thenebula can be significantly boosted by the forward shock, leading toshort-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 toafterglow 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 thesubsequent afterglow emission may be seen by radio telescopes such as VLA. (iv)Finally, we discuss several implications specific to FRBs, includingconstraints on the emission regions and limits on soft gamma-ray counterparts.

monthly notices of the royal astronomical society

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