2009/05/31 by Katsuaki Asano, K. Asano, T. Terasawa · 82 citations
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Electron #Emission spectrum #Fermi Gamma-ray Space Telescope #Fermi acceleration #Galaxy #Gamma-ray burst #Gamma-ray bursts and supernovae #Luminosity #Monte Carlo method #Nuclear physics #Optics #Particle acceleration #Photon #Physics #Plasma #Pulsars and Gravitational Waves Research #Spectral index #Spectral line #Synchrotron #astro-ph.HE
paper · pdf · doi:10.1088/0004-637x/705/2/1714
published in The Astrophysical Journal 705(2), 1714-1720 (IOP Publishing) · 21 pages, 7 figures. Accepted for publication in The Astrophysical Journal
arxiv created 2009/10/16 · openalex publication_date 2009/10/26 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We propose a new mechanism for the prompt emission of gamma-ray burst. In our model, electrons are continuously accelerated in the post-shock region via plasma turbulence. Using the Monte Carlo technique, we mimic the second-order Fermi acceleration due to plasma turbulence and obtain photon spectra. Since the acceleration balances with the synchrotron cooling, the observed low-energy spectral index is naturally explained. The resultant spectra can be consistent with observed spectra at least below ∼1 MeV. The model also predicts delayed GeV–TeV emission due to inverse Compton and broad pulse profile of optical emission in some cases. Although nontrivial assumptions are required to reproduce MeV–GeV power-law spectra, the model implies the possibility of explaining various kinds of luminosity correlations.