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Alfvén waves and turbulence in the solar atmosphere and solar wind

Verdini, Andrea and Velli, Marco (2007) Alfvén waves and turbulence in the solar atmosphere and solar wind. Astrophysical Journal, 662 (1). pp. 669-676. ISSN 0004-637X. doi:10.1086/510710.

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We solve the problem of propagation and dissipation of Alfvénic turbulence in a model solar atmosphere consisting of a static photosphere and chromosphere, transition region, and open corona and solar wind using a phenomenological model for the turbulent dissipation based on wave reflection. We show that most of the dissipation for a given wave-frequency spectrum occurs in the lower corona, and the overall rms amplitude of the fluctuations evolves in a way consistent with observations. The frequency spectrum for a Kolmogorov-like slope is not found to change dramatically from the photosphere to the solar wind; however, it does preserve signatures of transmission throughout the lower atmospheric layers, namely, oscillations in the spectrum at high frequencies reminiscent of the resonances found in the linear case. These may disappear once more realistic couplings for the nonlinear terms are introduced or if time-dependent variability of the lower atmospheric layer is introduced.

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Additional Information:© 2007 American Astronomical Society. Print publication: Issue 1 (2007 June 10); received 2006 August 5; accepted for publication 2006 November 3 We would like to thank the IPAM program "Grand Challenge Problems in Computational Astrophysics" at UCLA, where this work was completed. We also thank S. Oughton and W. H. Matthaeus for useful discussion.
Subject Keywords:MHD; solar wind; turbulence; waves
Issue or Number:1
Record Number:CaltechAUTHORS:20090409-113000863
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:13905
Deposited By: Jason Perez
Deposited On:09 Apr 2009 23:22
Last Modified:08 Nov 2021 22:41

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