Solar radio bursts provide powerful diagnostics of the coronal magnetic field, density inhomogeneities, and turbulence. These bursts, classified from types I through IV based on their origin and spectral signatures, are all produced via plasma emission processes driven by non-thermal electrons. As such, radio bursts not only trace local magnetized plasma conditions but also carry imprints of the coronal density structures through which the radiation propagates.
Among these, type II bursts are of particular interest as they signify shock waves, often driven by energetic solar eruptions such as coronal mass ejections (CMEs) and flares. Their association with CMEs makes type II bursts highly relevant for space-weather studies. These emissions allow us to probe both shock properties and the surrounding plasma environment, while their polarization signatures offer a direct diagnostic of CME-entrained magnetic fields.
In this talk, I will present results from a detailed polarimetric imaging study of a type II burst observed with the Murchison Widefield Array (MWA), complemented by comparisons with numerical simulations. While the main focus will be on imaging analyses of type II bursts, I will also discuss our ongoing efforts to develop tools and techniques that enable such studies.
Exploring the Magnetized Corona with (Type-II) Solar Radio Burst
Jeudi 4 septembre 2025
de
11:00 à
12:00
Salles de réunion - Bat 14 - Salle de réunion 103a
