The Dynamical Influence Of The Transition Region And Chromosphere On The Heating Of Coronal Loops By Resonant Absorption Of Alfvén Waves

Details The Dynamical Influence Of The Transition Region And Chromosphere On The Heating Of Coronal Loops By Resonant Absorption Of Alfvén Waves The Dynamical Influence Of The Transition Region And Chromosphere On The Heating Of Coronal Loops By Resonant Absorption Of Alfvén Waves

Oct 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999esasp.446..167b&link_type=abstract

8th SOHO Workshop: Plasma Dynamics and Diagnostics in the Solar Transition Region and Corona. Proceedings of the Conference hel

Astronomy and Astrophysics

Astrophysics

2

Scientific paper

We present a numerical MHD study of coronal heating by resonant absorption of Alfvén waves using models that include an extended chromosphere and dynamical transition region. The calculations are done with the Versatile Advection Code (VAC) and assume axisymmetric loop configurations. Linear polarized, monochromatic Alfvén waves are launched at the bottom of our extended chromosphere. The efficiency of heating by resonant absorption of these waves in the corona is measured by the ratio of Ohmic dissipation over the incoming Poyting flux at the bottom of our chromosphere (averaged over a driving period). The efficiency turns out to be much smaller than in loop models that do not take the chromospheric and transition region coupling into account. For our model, the efficiency is typically of the order of 10% in contrast with values over 90% in models without the coupling taken into account. The difference can be described in terms of efficient nonlinear generation of compressive motions in the chromosphere and transition region, the change of the coronal cavity length as a consequence of the continuous motion of the transition region (due to the the Alfvén wave pressure and compressive motions), and coronal cavity leakage due to a finite Alfvén speed ratio between corona and chromosphere. The compressive waves and motions lead to density variations that should be observable. To proove that, our model results are used to simulate some coronal and transition region CDS EUV line observations as well as broad band EIT observations. The results are used to give an explanation of EUV coronal brightenings in terms of mass motions.

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