| Name: Ajaz Mir |
| Affiliation: Department of Physics, Islamic University of Science & Technology, Awantipora, J&K |
| Conference ID: ASI2026_799 |
| Title: Kinetic Modelling of Solar Radio Bursts Generated by Beam–Plasma Interactions |
| Abstract Type: Poster |
| Abstract Category: High Energy Phenomena, Fundamental Physics and Astronomy |
| Author(s) and Co-Author(s) with Affiliation: Ajaz Mir(Islamic University of Science & Technology, Awantipora-192122, India), Anshu Kumari(Udaipur Solar Observatory, Udaipur-313001, India) |
| Abstract: Solar radio bursts play a pivotal role in advancing both fundamental plasma physics and space-weather predictions. These emissions are produced by energetic electron beams and shock structures propagating through the solar corona. They encode rich information about nonlinear kinetic processes whose detailed microphysics remain only partially understood. Although magnetohydrodynamic (MHD) models successfully reproduce the large-scale evolution of coronal shocks, mass ejections, and magnetic-field reconfiguration, they are intrinsically limited in their ability to capture the kinetic instabilities, wave–particle interactions, and coherent wave processes responsible for radio emission.
Particle-In-Cell (PIC) simulations provide a powerful framework to bridge this gap by self-consistently resolving beam–plasma interactions, Langmuir turbulence, nonlinear wave–wave coupling, and mode-conversion processes that are widely regarded as the physical origin of Type II and Type III solar radio bursts. In this work, we present preliminary PIC simulation findings demonstrating that the onset of solar radio emission is primarily governed by beam–plasma instabilities. Energetic electrons drive strong Langmuir wave activity, which subsequently undergoes nonlinear coupling, including interactions with backscattered Langmuir modes. These processes lead to the generation of slowly and rapidly drifting electromagnetic emissions that closely resemble the spectral characteristics of observed Type II and Type III radio bursts.
The temporal evolution and frequency drift of the emitted radiation are identified through power-spectral analysis, while their nonlinear and coherent properties are quantified using bispectral diagnostics. Together, these analyses provide compelling evidence that solar radio bursts originate from fundamentally kinetic processes that are inaccessible to fluid-based descriptions.
|
