Coronal Heating by Surface Alfven Wave Damping: Implementation in MHD Modeling and Connection to Observations

Details Coronal Heating by Surface Alfven Wave Damping: Implementation in MHD Modeling and Connection to Observations Coronal Heating by Surface Alfven Wave Damping: Implementation in MHD Modeling and Connection to Observations

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh42a..07e&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH42A-07

Astronomy and Astrophysics

Astrophysics

[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7959] Space Weather / Models

Scientific paper

We present results from the development of a solar wind model driven by Alfven waves with realistic damping mechanisms. We self-consistently introduce surface Alfven wave damping, which is characterized by transverse gradients in density. The plasma gradients set up a resonant layer, in which the waves dissipate energy to the wind. First, we applied surface Alfven wave damping in a solar wind model driven by a flat wave spectrum (van der Holst et al. 2010), and demonstrated its effect at the boundary of open and closed magnetic fields (Evans et al. 2010). Here we apply surface wave damping to a model which allows a Kolmogorov-type spectrum of Alfven waves to evolve in frequency space (Oran et al. 2010). We consider waves with frequencies lower than those damped in the chromosphere, and on the order of those dominating the heliosphere (0.0001 to 100 Hz). We provide wave dissipation as a function of frequency. We connect our modeling results to recent observations, including an estimation of resonant absorption damping by Verth, Terradas & Goossens (2010) and density and temperature distributions using differential emission measure tomography by Vasquez, Frazin & Manchester (2010), which we present as both direct and indirect evidence that this dissipation mechanism occurs and is important in the lower corona.

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