2017/01/17 by Vadim R. Munirov, Nathaniel J. Fisch, N. J. Fisch
Physics and Astronomy · #Astro and Planetary Science #Astrophysics #Classical mechanics #Computational physics #Dynamo #Dynamo theory #Ionosphere and magnetosphere dynamics #Kinetic energy #Magnetic field #Mechanics #Nuclear physics #Optics #Physics #Plasma #Quantum electrodynamics #Quantum mechanics #Radiative transfer #Solar and Space Plasma Dynamics #Solar dynamo #astro-ph.GA #physics.plasm-ph
paper · pdf · doi:10.1103/physreve.95.013205
published as Physical Review E 95, 013205 (2017) · 6 pages, 4 figures, published in Physical Review E
openalex publication_date 2017/01/17 · arxiv created 2017/09/21 · arxiv updated 2017/09/22 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Magnetic fields in rotating and radiating astrophysical plasma can be produced due to a radiative interaction between plasma layers moving relative to each other. The efficiency of current drive, and with it the associated dynamo effect, is considered in a number of limits. It is shown here, however, that predictions for these generated magnetic fields can be significantly higher when kinetic effects, previously neglected, are taken into account.