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Turbulent kinetic energy in the energy balance of a solar flare View all abstracts by submitter

Eduard Kontar   Submitted: 2017-04-01 08:49

The energy released in solar flares derives from a reconfiguration of magnetic fields to a lower energy state, and is manifested in several forms, including bulk kinetic energy of the coronal mass ejection, acceleration of electrons and ions, and enhanced thermal energy that is ultimately radiated away across the electromagnetic spectrum from optical to X-rays. Using an unprecedented set of coordinated observations, from a suite of instruments, we here report on a hitherto largely overlooked energy component - the kinetic energy associated with small-scale turbulent mass motions. We show that the spatial location of, and timing of the peak in, turbulent kinetic energy together provide persuasive evidence that turbulent energy may play a key role in the transfer of energy in solar flares. Although the kinetic energy of turbulent motions accounts, at any given time, for only ~ (0.5-1)% of the energy released, its relatively rapid (~1-10 s) energization and dissipation causes the associated throughput of energy (i.e., power) to rival that of major components of the released energy in solar flares, and thus presumably in other astrophysical acceleration sites.

Authors: Kontar, E. P.; Perez, J. E.; Harra, L. K.; Kuznetsov, A. A.; Emslie, A. G.; Jeffrey, N. L. S.; Bian, N. H.; Dennis, B. R.
Projects: None,Hinode/EIS,RHESSI,SDO-AIA,SDO-HMI

Publication Status: to be published in Physical Review Letters
Last Modified: 2017-04-02 19:06
Go to main E-Print page  Triggering Process of the X1.0 Three-ribbon Flare in the Great Active Region NOAA 12192  Magnetic Helicity Estimations in Models and Observations of the Solar Magnetic Field. Part III: Twist Number Method  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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