Turbulence and Particle Acceleration in Solar Flares
Abstract
Solar eruptive events produce flares in the corona and coronal mass ejections (CMEs). Particles are accelerated both in the coronal reconnection sites and in the CME driven shocks. Traditionally, investigations of the radiation producing particles (RPPs) at the flare has been the main focus of the solar physics while the focus of the helispheric has been the study of the solar energetic particles (SEPs) and accelerated in the CME-shock environment. However, there are several observations (from RHESSI hard X-ray, ground based microwave, and Fermi gamma-ray) indicating a close connection between these two processes. This connection will be the focus of this talk.I will review these observations and describe models that explain these connection. I will show the role of RPPs escaping the upwards along open field lines as seeds for re-acceleration at the CME, and the role of CME accelerated SEPs, escaping from the shock downstream to the Sun, in production of long duration >100 MeV gamma-rays. An important aspect, which plays a central role in this scenario, is the processes of escape of accelerated particles up and down from flare site and from downstream and upstream of the CME.
- Publication:
-
AGU Fall Meeting Abstracts
- Pub Date:
- December 2019
- Bibcode:
- 2019AGUFMSH33D3413P
- Keywords:
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- 7829 Kinetic waves and instabilities;
- SPACE PLASMA PHYSICS;
- 7835 Magnetic reconnection;
- SPACE PLASMA PHYSICS;
- 7836 MHD waves and instabilities;
- SPACE PLASMA PHYSICS;
- 7863 Turbulence;
- SPACE PLASMA PHYSICS