2017/03/31 by Christopher Thompson
Physics and Astronomy · #Astrophysics #Astrophysics and Cosmic Phenomena #Atomic physics #Electron #Gamma-ray bursts and supernovae #Lorentz factor #Lorentz transformation #Magnetic field #Nuclear physics #Optics #Physics #Radio Astronomy Observations and Technology #Scattering #Superluminal motion #Thomson scattering #astro-ph.HE #hep-ph
paper · pdf · doi:10.3847/1538-4357/aa7845
25 pages, 16 figures, Astrophysical Journal, in press
arxiv created 2017/06/06 · openalex publication_date 2017/08/01 · arxiv updated 2017/08/09 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Abstract This paper considers electromagnetic transients of a modest total energy ( erg) and small initial size ( cm). They could be produced during collisions between relativistic field structures (e.g., macroscopic magnetic dipoles) that formed around or before cosmic electroweak symmetry breaking. The outflowing energy has a dominant electromagnetic component; a subdominant thermal component (temperature GeV) supplies inertia in the form of residual . A thin shell forms, expanding subluminally and attaining a Lorentz factor before decelerating. Drag is supplied by the reflection of an ambient magnetic field and deflection of ambient free electrons. Emission of low-frequency (GHz–THz) superluminal waves takes place through three channels: (i) reflection of the ambient magnetic field; (ii) direct linear conversion of the embedded magnetic field into a superluminal mode; and (iii) excitation outside the shell by corrugation of its surface. The escaping electromagnetic pulse is very narrow (a few wavelengths), so the width of the detected transient is dominated by propagation effects. GHz radio transients are emitted from (i) the dark matter halos of galaxies and (ii) the near-horizon regions of supermassive black holes that formed via direct gas collapse and now accrete slowly. Brighter and much narrower 0.01–1 THz pulses are predicted at a rate at least comparable to fast radio bursts, experiencing weaker scattering and absorption. The same explosions also accelerate protons up to eV, and heavier nuclei up to 10 20–21 eV.