2002/01/18 by Roberto Aloisio, Pasquale Blasi
Engineering · Physics and Astronomy · #Astrophysics and Cosmic Phenomena #Background radiation #Charged particle #Computational physics #Cosmic ray #Cyclotron #Cyclotron radiation #Electron #Energy spectrum #Ion #Nuclear physics #Particle Accelerators and Free-Electron Lasers #Physics #Pulsars and Gravitational Waves Research #Quantum electrodynamics #Quantum mechanics #Radiation #Synchrotron #Synchrotron radiation #astro-ph
paper · pdf · doi:10.1016/s0927-6505(02)00102-0
published in Astroparticle Physics 18(2), 195-203 (Elsevier BV) · to be published in Astroparticle Physics
arxiv created 2002/01/18 · openalex publication_date 2002/10/01 · arxiv updated 2009/12/01 · openalex created_date 2022/10/02 · openalex updated_date 2025/11/06
The standard calculations of the synchrotron emission from charged particles in magnetic fields does not apply when the energy losses of the particles are so severe that their energy is appreciably degraded during one Larmor rotation. In these conditions, the intensity and spectrum of the emitted radiation depend on the observation time Tobs: the standard result is recovered only in the limit Tobs≪ Tloss, where Tloss is the time for synchrotron losses. In this case the effects of the radiation backreaction cannot be detected by the observer. We calculate the emitted power of the radiation in the most general case, naturally including both the cases in which the backreaction is relevant and the standard case, where the usual result is recovered. Finally we propose several scenarios of astrophysical interest in which the effects of the backreaction cannot and should not be ignored.