2001/02/03 by C. L. Bianco, Carlo Luciano Bianco, R. Ruffini +2 · 40 citations
Physics and Astronomy · #Afterglow #Astrophysics #Astrophysics and Cosmic Phenomena #Atomic physics #Detector #Gamma-ray burst #Gamma-ray bursts and supernovae #Nuclear physics #Optics #Physics #Plasma #Pulsars and Gravitational Waves Research #Pulse (music) #astro-ph
paper · pdf · doi:10.1051/0004-6361:20000556
published in Astronomy and Astrophysics 368(2), 377-390 (EDP Sciences) · 14 pages, 18 figures, to appear in Astronomy & Astrophysics
arxiv created 2001/02/03 · openalex publication_date 2001/03/01 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
In the framework of the model that uses black holes endowed with electromagnetic structure (EMBH) as the energy source, we study how an elementary spike appears to the detectors. We consider the simplest possible case of a pulse produced by a pure e+e- pair-electro-magnetic plasma, the PEM pulse, in the absence of any baryonic matter. The resulting time profiles show a Fast-Rise-Exponential-Decay shape, followed by a power-law tail. This is obtained without any special fitting procedure, but only by fixing the energetics of the process taking place in a given EMBH of selected mass, varying in the range from 10 to 103 and considering the relativistic effects to be expected in an electron-positron plasma gradually reaching transparency. Special attention is given to the contributions from all regimes with Lorentz γ factor varying from to in a few hundreds of the PEM pulse travel time. Although the main goal of this paper is to obtain the elementary spike intensity as a function of the arrival time, and its observed duration, some qualitative considerations are also presented regarding the expected spectrum and on its departure from the thermal one. The results of this paper will be comparable, when data will become available, with a subfamily of particularly short GRBs not followed by any afterglow. They can also be propedeutical to the study of longer bursts in presence of baryonic matter currently observed in GRBs.