2020/05/31 by Rachid Ouyed, Denis Leahy, D. A. Leahy +1 · 4 citations
Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Ejecta #Galaxy #Galaxy cluster #Gamma-ray bursts and supernovae #Neutron star #Nuclear physics #Physics #Plasma #Pulsars and Gravitational Waves Research #Stars #Supernova #astro-ph.HE #physics.plasm-ph
paper · pdf · doi:10.1093/mnras/staa3511
published in Monthly Notices of the Royal Astronomical Society 500(4), 4414-4421 (Oxford University Press) · MNRAS version (see https://academic.oup.com/mnras/article-abstract/500/4/4414/5979827?redirectedFrom=PDF). Converted to a main paper (first 9 pages) + supplementary material [a total of 50 pages including 16 tables and 11 figures]. The QN FRB simulator can be run online at: http://www.quarknova.ca/FRBSimulator/
openalex created_date 2020/05/29 · openalex publication_date 2020/11/11 · arxiv created 2021/03/19 · arxiv updated 2021/03/23 · openalex updated_date 2026/08/05
ABSTRACT We show that old isolated neutron stars in groups and clusters of galaxies experiencing a Quark-Nova phase (QN: an explosive transition to a quark star) may be the source of fast radio bursts (FRBs). Each of the millions of fragments of the ultrarelativistic QN ejecta provides a collisionless plasma for which the ambient medium (galactic/halo, the intragroup/intracluster medium) acts as a relativistic plasma beam. The Buneman and the Weibel instabilities, successively induced by the beam in the fragment, generate particle bunching and observed coherent emission at GHz frequency with a corresponding fluence in the Jy ms range. The duration, frequency drift, and the rate are in agreement with observed properties of FRBs. Repeats (on time-scales of minutes to months) are due to seeing multiple fragments each beaming at a different direction and coming in at different times. Single (non-repeating) FRBs occur when only emission from the primary fragment is within the detector’s sensitivity. Key properties of FRB 121102 (its years of activity) and of FRB 180916.J0158+65 (its ∼16 d period) are recovered. The spatial and temporal coincidence between SGR 1935+2154 and FRB 200428 finds an explanation in our model. We give testable predictions.