Turbulence And Wave Dissipation In The Chromosphere, Corona, And Solar Wind

Details Turbulence And Wave Dissipation In The Chromosphere, Corona, And Solar Wind Turbulence And Wave Dissipation In The Chromosphere, Corona, And Solar Wind

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.2101c&link_type=abstract

American Astronomical Society, SPD meeting #37, #21.01; Bulletin of the American Astronomical Society, Vol. 38, p.249

Astronomy and Astrophysics

Astronomy

1

Scientific paper

The continually evolving convection below the solar photospheregives rise to a wide spectrum of acoustic and magneticfluctuations that propagate out into the heliosphere.In this talk I will review the various ways that waves,shocks, and turbulent eddies are expected to interact withthe mean plasma conditions of the outer solar atmosphere.For open magnetic flux tubes, the heating of the chromosphereand corona, as well as the acceleration of the solar wind,can be understood from the standpoint of wave dissipation andturbulent cascade.For example, the importance of magnetohydrodynamic turbulence inthe extended corona has been affirmed by the surprisingmeasurements of the UVCS instrument on SOHO that heavy ions areheated to hundreds of times the temperatures of protons andelectrons, indicating collisionless Alfven wave dissipation.Complete theoretical models are difficult to construct, though,because many of the proposed physical processes act on amultiplicity of spatial scales (from centimeters to solar radii)with feedback effects not yet well understood.Despite these difficulties, progress has been made toward the goalof producing models that predict the plasma properties everywhereabove the solar surface using only lower boundary conditions atthe photosphere.

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