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Heating of coronal active regions

Published online by Cambridge University Press:  26 August 2011

Daniel O. Gómez
Daniel O. Gómez*
Affiliation:
Instituto de Astronomía y Física del Espacio, C.C. 67 - Suc. 28, (1428) Buenos Aires, Argentina - email: gomez@iafe.uba.ar Departamento de Física, Facultad de Ciencias Exactas y Naturales (UBA), Ciudad Universitaria, (1428) Buenos Aires, Argentina
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Abstract

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Recent observations of coronal loops in solar active regions show that their heating must be a truly dynamic process. Even though it seems clear that the energy source is the magnetic field that confines the coronal plasma, the details of how it dissipates are still a matter of debate. In this presentation we review the theoretical models of coronal heating, which have been traditionally clasified as DC or AC depending on the electrodynamic response of the loops to the photospheric driving motions.

Also, we show results from numerical simulations of the internal dynamics of coronal loops within the framework of the reduced MHD approximation. These simulations indicate that the application of a stationary velocity field at the photospheric boundary leads to a turbulent stationary regime after several photospheric turnover times. Once this turbulent regime is set, both DC and AC stresses dissipate at faster rates as a result of a direct energy cascade.

Keywords

Sun: coronaSun: X-raysmagnetic fielsMHDturbulence
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S273: The Physics of Sun and Star Spots , August 2010 , pp. 44 - 50
Copyright
Copyright © International Astronomical Union 2011

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