Solar Coronal Heating via Alfven Wave Turbulence

Journal Article · Thu Mar 25 00:00:00 EDT 2010 · AIP Conference Proceedings

DOI:https://doi.org/10.1063/1.3395910· OSTI ID:21371726

Bigot, B ^[1]; Galtier, S ^[2]; Politano, H ^[3]

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1. Space Science Center, University of New Hampshire, Durham, NH 03824 (United States)
2. Institut d'Astrophysique Spatiale, Universite Paris-Sud, batiment 121, 91405 Orsay (France)
3. Universite de Nice-Sophia Antipolis, CNRS UMR 6202, Observatoire de la Cote d'Azur, BP 4229, 06304 Nice Cedex 4 (France)

A short review is given about the self-consistent MHD model of solar coronal heating recently proposed by Bigot et al.(2008) in which the dynamical effect of the background magnetic field along a coronal structure is taken into account through exact results from Alfven wave turbulence. The main properties of the model are given as well as the heating rate and the microturbulent velocity obtained in the case of coronal loops. The conclusion is that Alfven wave turbulence may produce an efficient background heating for the solar corona.

• OSTI ID: 21371726
• Journal Information: AIP Conference Proceedings, Vol. 1216, Issue 1; Conference: 12. international solar wind conference, Saint-Malo (France), 21-26 Jun 2009; Other Information: DOI: 10.1063/1.3395910; (c) 2010 American Institute of Physics; ISSN 0094-243X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ALFVEN WAVES
ASTROPHYSICS
HEATING RATE
MAGNETIC FIELDS
MAGNETOHYDRODYNAMICS
PLASMA
PLASMA HEATING
REVIEWS
SOLAR CORONA
TURBULENCE
VELOCITY
ATMOSPHERES
DOCUMENT TYPES
FLUID MECHANICS
HEATING
HYDRODYNAMICS
HYDROMAGNETIC WAVES
MECHANICS
PHYSICS
SOLAR ATMOSPHERE
STELLAR ATMOSPHERES
STELLAR CORONAE