Introduction

Hard X-ray emission of solar flares can enable insights into the non-thermal energetic particle properties created during these irruptive events. Depending on the coronal densities and plasma properties, a part of the non-thermal electron population can be trapped at the loop-top. Theory suggest
that the coronal region at the loop-top is
the main acceleration site for electrons,At high energies, the bright footpoint emission from the flare loops prevents a detailed analysis of the usually weaker loop-top source due to the limited dynamic range of instruments like RHESSI. Thus, flares close to the solar limb, where the footpoints are  occulted,  are interesting events to study because they can reveal the loop-top emission. Here, we report on recent findings of a statistical study of such events, comprising  
The so-called Neupert effect is an empirically observed correlation in solar flares, which relates the changes (i.e. the time derivative) in the soft X-ray (SXR) flux to the temporal hard X-ray (HXR) variations. It is usually assumed that the HXRs originate in strong footpoint emissions from accelerated electron beams hitting the transition region and chromosphere. This in turn can lead to heating processes, increasing the overall SXR and extreme ultraviolet (EUV) emission.

Flare Selection