Characteristics of the flare acceleration region derived from simultaneous hard X-ray and radio observations

TL;DR

This study combines X-ray and radio observations to determine the spatial properties of the solar flare acceleration region, revealing its height and size and their relation to electron spectral characteristics.

Contribution

It provides a novel analytical and numerical relationship linking type III burst starting frequencies to acceleration region properties, based on simultaneous multi-wavelength observations.

Findings

Estimated acceleration region height around 50 Mm

Acceleration region size approximately 10 Mm

Electrons accelerated above the soft X-ray loop-top

Abstract

We investigate the type III radio bursts and X-ray signatures of accelerated electrons in a well observed solar flare in order to find the spatial properties of the acceleration region. Combining simultaneous RHESSI hard X-ray flare data and radio data from Phoenix-2 and the Nan\c{c}ay radioheliograph, the outward transport of flare accelerated electrons is analyzed. The observations show that the starting frequencies of type III bursts are anti-correlated with the HXR spectral index of solar flare accelerated electrons. We demonstrate both analytically and numerically that the type III burst starting location is dependent upon the accelerated electron spectral index and the spatial acceleration region size, but weakly dependent on the density of energetic electrons for relatively intense electron beams. Using this relationship and the observed anti-correlation, we estimate the height and vertical extent of the acceleration region, giving values of around 50 Mm and 10 Mm respectively. The inferred acceleration height and size suggests that electrons are accelerated well above the soft X-ray loop-top, which could be consistent with the electron acceleration between 40 Mm and 60 Mm above the flaring loop.