Astronomy and Astrophysics – Astronomy
Scientific paper
May 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21630301l&link_type=abstract
American Astronomical Society, AAS Meeting #216, #303.01; Bulletin of the American Astronomical Society, Vol. 41, p.850
Astronomy and Astrophysics
Astronomy
Scientific paper
The mechanisms responsible for heating the Sun's corona and accelerating the solar wind are still being actively investigated. However, it is largely accepted that photospheric motions provide the energy source and that the magnetic field must play a key role in the process. Three-dimensional MHD models have traditionally used an empirical prescription for coronal heating (e.g., Lionello et al. 2009), together with WKB Alfven wave acceleration of the solar wind. Recently, attention has been focused on wave turbulence driven models (e.g., Cranmer et al. 2007; Cranmer 2010) in which the heating and solar wind acceleration by Alfven waves are included self-consistently. We will demonstrate the initial implementation of this idea in an MHD model based on turbulent cascade heating in the closed-field regions (Rappazzo et al. 2007, 2008), and Alfven wave turbulent dissipation in open field regions (Verdini & Velli 2007, 2010).
Linker Jon A.
Lionello Roberto
Mikic Zoran
Riley Pete
Velli M. M.
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