Abstract
We investigate the global energetics and energy closure of various physical processes that are energetically important in solar flares and coronal mass ejections (CMEs), which includes: magnetic energies, thermal energies, nonthermal energies (particle acceleration), direct and indirect plasma heating processes, kinetic CME energies, gravitational CME energies, aerodynamic drag of CMEs, solar energetic particle events, EUV and soft X-ray radiation, white-light, and bolometric energies. Statistics on these forms of energies is obtained from 400 GOES M- and X-class events during the first 3.5 years of the Solar Dynamics Observatory (SDO) mission. A primary test addressed in this study is the closure of the various energies, such as the equivalence of the dissipated magnetic energies and the primary dissipated are energies (accelerated particles, direct heating, CME acceleration), which faciliate the energy of secondary processes (plasma heating, shock acceleration) and interactions with the solar wind (aerodynamic drag). Our study demonstrates energy closure in the statistical average, while individual events may have considerable uncertainties, requiring improved nonlinear force-free field models, and particle acceleration models with observationally constrained low-energy cutoffs.
Highlights
The energy flow in solar flares and coronal mass ejections (CMEs) passes through several processes, which are depicted in the diagram of Fig. 1
There are three primary energy dissipation processes that follow after a magnetic instability, typically a magnetic reconnection process, spawning (i) the acceleration of nonthermal particles (e.g., reviews by [3,4,5,6,7], with electron energy Ent,e and ion energy Ent,i, providing (ii) direct heating in the magnetic reconnection region, Edir (e.g., [8,9,10]); these are often accompanied by (iii) an eruptive process, which can be a complete eruption of a CME or filament, or a semi-eruptive energy release, known as “failed eruption”, in the case of a confined flare (e.g., Torok and Kliem [11])
Nonthermal particles are accelerated along bi-directional trajectories that lead out of the magnetic reconnection region, where most particles precipitate down to the chromosphere, heat the chromospheric plasma and drive evaporation of the heated plasma up into the corona (e.g., Antonucci and Dennis [12]), while other particles escape into interplanetary space
Summary
The energy flow in solar flares and coronal mass ejections (CMEs) passes through several processes, which are depicted in the diagram of Fig. 1. Primary test addressed in this study is the closure of the various energies, such as the equivalence of the dissipated magnetic energies and the primary dissipated flare energies (accelerated particles, direct heating, CME acceleration), which faciliate the energy of secondary processes (plasma heating, shock acceleration) and interactions with the solar wind (aerodynamic drag).
Sign-in/Register to view highlights & summary Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
