Observation of inverse Compton emission from a long γ-ray burst

作者: Peter Veres , PN Bhat , MS Briggs , WH Cleveland , R Hamburg

DOI: 10.1038/S41586-019-1754-6

关键词: StarsGamma-ray burstAstrophysicsExtragalactic background lightSynchrotron radiationAfterglowSpectral componentPhotonSpectral energy distributionPhysics

摘要: Long-duration γ-ray bursts (GRBs) originate from ultra-relativistic jets launched the collapsing cores of dying massive stars. They are characterized by an initial phase bright and highly variable radiation in kiloelectronvolt-to-megaelectronvolt band, which is probably produced within jet lasts milliseconds to minutes, known as prompt emission1,2. Subsequently, interaction with surrounding medium generates shock waves that responsible for afterglow emission, days months occurs over a broad energy range radio gigaelectronvolt bands1-6. The emission generally well explained synchrotron emitted electrons accelerated external shock7-9. Recently, intense long-lasting between 0.2 1 teraelectronvolts was observed GRB 190114C10,11. Here we report multi-frequency observations 190114C, study evolution time across 17 orders magnitude energy, 5 × 10-6 1012 electronvolts. We find broadband spectral distribution double-peaked, teraelectronvolt constituting distinct component power comparable component. This associated satisfactorily inverse Compton up-scattering photons high-energy electrons. conditions required account typical GRBs, supporting possibility commonly GRBs.

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