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Seismological constraints on the solar coronal heating function View all abstracts by submitter

Dmitrii Kolotkov   Submitted: 2020-10-07 02:38

The hot solar corona exists because of the balance between radiative and conductive cooling and some counteracting heating mechanism which remains one of the major puzzles in solar physics. The coronal thermal equilibrium is perturbed by magnetoacoustic waves which are abundantly present in the corona, causing a misbalance between the heating and cooling rates. Due to this misbalance, the wave experiences a back-reaction, either losing or gaining energy from the energy supply that heats the plasma, at the time scales comparable to the wave period. In particular, the plasma can be subject to wave-induced instability or over-stability, depending on the specific choice of the coronal heating function. In the unstable case, the coronal thermal equilibrium would be violently destroyed, which does not allow for the existence of long-lived plasma structures typical for the corona. Based on this, we constrained the coronal heating function using observations of slow magnetoacoustic waves in various coronal plasma structures.

Authors: D. Y. Kolotkov, T. J. Duckenfield, V. M. Nakariakov
Projects: None

Publication Status: Accepted for publication in A&A
Last Modified: 2020-10-07 10:17
Go to main E-Print page  Magnetic Helicity Flux across Solar Active Region Photospheres: I. Hemispheric Sign Preference in Solar Cycle 24  The Coronal Global Evolutionary Model: Using HMI Vector Magnetogram and Doppler Data to Determine Coronal Magnetic Field Evolution  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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