On dissipative effects in solar prominences

Free access article

Issue		A&A Volume 410, Number 2, November I 2003


Page(s)		L17 - L19
Section		Letters
DOI		http://dx.doi.org/10.1051/0004-6361:20031401

A&A 410, L17-L19 (2003)
DOI: 10.1051/0004-6361:20031401

Letter

On dissipative effects in solar prominences

I. Ballai

Space & Atmosphere Research Center, Dept. of Applied Mathematics, University of Sheffield, Hicks Building, Hounsfield Road, Sheffield, S3 7RH, England, UK
(Received 8 July 2003 / Accepted 11 September 2003)

Abstract
The present paper aims to discuss the possible dissipative mechanisms acting in a coronal prominence. These mechanism are discussed within the context of spatial damping of linear compressional waves. The obtained results show that the dominant mechanism is thermal radiation provided the supposition of optically thin prominence is valid. Damping due to thermal conduction is a viable attenuation mechanism provided the wavelength of the waves is short.

Key words: Sun: atmosphere -- prominences -- evolution -- magnetic fields -- magnetohydrodynamics -- numerical

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