Shock-wave radio probing of solar wind sources in coronal magnetic fields

Abstract

The Space Weather effects in the near-Earth environment as well as in atmospheres of other terrestrial planets arise by corpuscular radiation from the Sun, known as the solar wind. The solar magnetic fields govern the solar corona structure. Magnetic-field strength values in the solar wind sources - key information for modeling and forecasting the Space Weather climate - are derived from various solar space- and ground-based observations, but, so far not accounting for specific types of radio bursts. These are "fractured" type II radio bursts attributed to collisions of shock waves with coronal structures emitting the solar wind. Here, we report about radio observations of two "fractured" type II bursts to demonstrate a novel tool for probing of magnetic field variations in the solar wind sources. These results have direct impact on interpretations of this class of bursts and contribute to the current studies of the solar wind emitters.

References in corpus (6)

• A Review of Solar Type III Radio Bursts
• Turbulence-Driven Coronal Heating and Improvements to Empirical Forecasting of the Solar Wind
• First Observation of a Type II Solar Radio Burst Transitioning Between a Stationary and Drifting State
• Coronal Pseudo-Streamer and Bipolar Streamer Observed by SOHO/UVCS in March 2008
• Solar type II radio bursts associated with CME expansions as shown by EUV waves
• The Broken Lane of a Type II Radio Burst Caused by Collision of a Coronal Shock with a Flare Current Sheet

Cited by in corpus (2)

• Solar coronal density turbulence and magnetic field strength at the source regions of two successive metric type II radio bursts
• Radio, X-ray, and EUV signatures of internal and external reconnection of an erupting flux rope