Particle acceleration in helical magnetic fields in solar corona

Astronomy Unit Seminars
Dr Mykola Gordovskyy (U. Manchester)
David Tsiklauri
October 24th, 2014 at 14:30
GO Jones Room 610

Twisted magnetic fields should be ubiquitous in the solar corona. Emerging twisted ropes as well as complex photospheric motions provide continuous influx of the magnetic helicity. Twisted coronal fields, in turn, contain excess magnetic energy, which can be released, causing solar flares and other explosive phenomena. It has been shown recently, that reconnection in helical magnetic structures results in particle acceleration distributed within large volume, including the lower corona and chromosphere. Hence, the magnetic reconnection and particle acceleration scenario involving magnetic helicity can be a viable alternative to the standard flare model, where particles are accelerated in a small volume located in the upper corona.

I will discuss recent progress in modelling the energy release and particle acceleration in twisted coronal loops. I will focus on various observational implications of particle acceleration in helical magnetic structures, particularly on spatial distributions of thermal and non-thermal emission, and their comparison with observational data.