Alfvén waves and turbulence in the solar atmosphere and solar wind
- Creators
- Verdini, Andrea
- Velli, Marco
Abstract
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.
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.Attached Files
Published - VERapj07.pdf
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Additional details
- Eprint ID
- 13905
- Resolver ID
- CaltechAUTHORS:20090409-113000863
- Created
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2009-04-09Created from EPrint's datestamp field
- Updated
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2021-11-08Created from EPrint's last_modified field