A Model for Radio Emission from Solar Coronal Shocks

Abstract

Solar coronal shocks are very common phenomena in the solar atmosphere and are believed to be the drivers of solar type II radio bursts. However, the microphysical nature of these emissions is still an open problem. This paper proposes that electron cyclotron maser (ECM) emission is responsible for the generation of radiations from the coronal shocks. In the present model, an energetic ion beam accelerated by the shock excites first Alfvén wave (AW) and then the excited AW leads to the formation of a density-depleted duct along the foreshock boundary of the shock. In this density-depleted duct, the energetic electron beam produced via the shock acceleration can effectively excite radio emission by the ECM instability. Our results show that this model may have potential application to solar type II radio bursts.

arXiv comment18 pages, 4 figures, accepted for publication in APJ

References in corpus (7)

• Direct Detection of a CME-Associated Shock in LASCO White Light Images
• Quantitative Measurements of CME-driven Shocks from LASCO Observations
• Observations and Interpretation of a Low Coronal Shock Wave Observed in the EUV by the SDO/AIA
• Coronal Magnetic Field Measurement from EUV Images made by the Solar Dynamics Observatory
• The Strength and Radial Profile of Coronal Magnetic Field from the Standoff Distance of a CME-driven Shock
• Off-limb Solar Coronal Wavefronts From SDO/AIA EUV Observations - Implications For Particle Production
• On the relationship of shock waves to flares and coronal mass ejections

Cited by in corpus (4)

• Cyclotron maser emission from power-law electrons with strong pitch-angle anisotropy
• Quantifying the Magnetic Structure of a Coronal Shock Producing a Type II Radio Burst
• Electron Cyclotron Maser Emissions from Evolving Fast Electron Beams
• A Parametric Investigation on the Cyclotron Maser Instability Driven by Ring-beam Electrons with Intrinsic Alfvén Waves