Is Cyclotron Maser Emission in Solar Flares Driven by a Horseshoe Distribution?

TL;DR

This paper investigates whether horseshoe electron distributions drive cyclotron maser emission in solar flare spike bursts, proposing a model involving electron acceleration, low plasma density cavities, and implications for electron supply in hard X-ray bursts.

Contribution

It introduces a 1D model linking electron acceleration to horseshoe distributions and coronal density cavities, extending ECME theory to solar flare spike bursts.

Findings

Horseshoe distributions can form in solar flare conditions.

Coronal density cavities facilitate ECME escape.

The model addresses the electron supply problem in hard X-ray bursts.

Abstract

Since the early 1980s, decimetric spike bursts have been attributed to electron cyclotron maser emission (ECME) by the electrons that produce hard X-ray bursts as they precipitate into the chromosphere in the impulsive phase of a solar flare. Spike bursts are regarded as analogous to the auroral kilometric radiation (AKR), which is associated with the precipitation of auroral electrons in a geomagnetic substorm. Originally, a loss-cone-driven version of ECME, developed for AKR, was applied to spike bursts, but it is now widely accepted that a different, horseshoe-driven, version of EMCE applies to AKR. We explore the implications of the assumption that horseshoe-driven ECME also applies to spike bursts. We develop a 1D model for the acceleration of the electrons by a parallel electric field, and show that under plausible assumptions it leads to a horseshoe distribution of electrons in a solar flare. A second requirement for horseshoe-driven ECME is an extremely low plasma density, referred to as a density cavity. We argue that a coronal density cavity should develop in association with a hard X-ray burst, and that such a density cavity can overcome a long-standing problem with the escape of ECME through the second-harmonic absorption layer. Both the horseshoe distribution and the associated coronal density cavity are highly localized, and could not be resolved in the statistically large number of local precipitation regions needed to explain a hard X-ray burst. The model highlights the "number problem" in the supply of the electrons needed to explain a hard X-ray burst.