Dynamical generation of macroscale magnetic fields and fast flows in a four-component astrophysical plasma

Abstract

We explore the possibility of the generation or amplification of macroscale magnetic fields and flows in a four-component astrophysical dusty plasma composed of mobile massless electrons and positrons, inertial positive ions and negatively charged static dust particles. The investigation demonstrates that when microscopic turbulent ambient plasma energy is predominantly kinetic, a straight dynamo (DY) mechanism is feasible. Conversely, a unified reverse-dynamo/dynamo (RDY/DY) mechanism is possible when the microscopic turbulent ambient plasma energy is primarily magnetic. Additionally, the evolution of Alfvén Mach numbers at the macro- and microscale are significantly affected by plasma species densities and invariant helicities. The potential implications of the present study for astrophysical settings are also highlighted.

References in corpus (10)

• On the Origin of Cosmic Magnetic Fields
• The Galactic Positron Annihilation Radiation & The Propagation of Positrons in the Interstellar Medium
• Modeling astrophysical outflows via the unified Dynamo-Reverse Dynamo mechanism
• A Magnetic Alpha-Omega Dynamo in Active Galactic Nuclei Disks: II. Magnetic Field Generation, Theories and Simulations
• Reversed dynamo at small scales and large magnetic Prandtl number
• Dust ion acoustic solitary structures in presence of nonthermally distributed electrons and positrons
• Constraints on dynamo action in plasmas
• A Magnetic Alpha-Omega Dynamo in Active Galactic Nuclei Disks: I. The Hydrodynamics of Star-Disk Collisions and Keplerian Flow
• Generation of a Fireball in AGN Hot Plasmas
• Macro-scale fast flow and magnetic field generation in 2-temperature relativistic electron-ion plasmas of astrophysical objects