2014/02/28 by Zhi-Bin Zhang, Si-Wei Kong, Yong-Feng Huang +2 · 15 citations
Physics and Astronomy · #Afterglow #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Galaxy #Gamma-ray burst #Gamma-ray bursts and supernovae #Light curve #Luminosity #Physics #Pulsars and Gravitational Waves Research #Radio telescope #Redshift #Telescope #astro-ph.CO #astro-ph.HE
paper · pdf · doi:10.1088/1674-4527/15/2/008
published in Research in Astronomy and Astrophysics 15(2), 237-251 (IOP Publishing) · 16 pages, 8 figures (2 new figs added), 1 table; accepted by Research in Astronomy and Astrophysics
arxiv created 2014/06/03 · openalex publication_date 2015/01/28 · arxiv updated 2015/06/18 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Using the generic hydrodynamic model of gamma-ray burst (GRB) afterglows, we calculate the radio afterglow light curves of low luminosity, high luminosity, failed and standard GRBs in different observational bands of FAST's energy window. The GRBs are assumed to be located at different distances from us. Our results rank the detectability of GRBs in descending order as high luminosity, standard, failed and low luminosity GRBs. We predict that almost all types of radio afterglows except those of low luminosity GRBs could be observed by a large radio telescope as long as the domains of time and frequency are appropriate. It is important to note that FAST can detect relatively weak radio afterglows at a higher frequency of 2.5 GHz for very high redshift up to z = 15 or even more. Radio afterglows of low luminosity GRBs can only be detected after the completion of the second phase of FAST. FAST is expected to significantly expand the sample of GRB radio afterglows in the near future.