2008/07/28 by Rongrong Xue, R. R. Xue, Yi-Zhong Fan +3
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysics #Electron #Gamma ray #Gamma-ray burst #Gamma-ray bursts and supernovae #Ion #Lorentz factor #Lorentz transformation #Neutron #Nuclear physics #Physics #Pulsars and Gravitational Waves Research #RADIUS #Range (aeronautics) #astro-ph #earthquake and tectonic studies
paper · pdf · doi:10.1111/j.1365-2966.2008.13578.x
published as Mon.Not.Roy.Astron.Soc.389:321,2008 · 5 pages, 2 figures
openalex publication_date 2008/07/28 · arxiv created 2008/10/17 · arxiv updated 2010/04/21 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
In the neutron-rich internal shocks model for γ-ray bursts (GRBs), the Lorentz factors (LFs) of ion shells are variable, and so are the LFs of accompanying neutron shells. For slow neutron shells with a typical LF of approximate tens, the typical β-decay radius is ∼1014–1015 cm. As GRBs last long enough [T90 > 14(1 +z) s], one earlier but slower ejected neutron shell will be swept successively by later ejected ion shells in the range ∼1013–1015 cm, where slow neutrons have decayed significantly. Part of the thermal energy released in the interaction will be given to the electrons. These accelerated electrons will mainly be cooled by the prompt soft γ-rays and give rise to GeV emission. This kind of GeV emission is particularly important for some very long GRBs and is detectable for the upcoming satellite Gamma-Ray Large Area Space Telescope (GLAST).