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Alfven waves and turbulence in the solar atmosphere and solar wind

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dc.contributor.author Verdini, Andrea
dc.contributor.author Velli, Marco
dc.date.accessioned 2008-09-23T22:25:11Z
dc.date.available 2008-09-23T22:25:11Z
dc.date.issued 2007-06-10
dc.identifier.citation The Astrophysical Journal, 662:669-676, 2007 June 10 en_US
dc.identifier.clearanceno 04-0876
dc.identifier.uri http://hdl.handle.net/2014/40967
dc.description.abstract We solve the problem of propagation and dissipation of Alfvenic 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 timedependent variability of the lower atmospheric layer is introduced. en_US
dc.description.sponsorship NASA/JPL en_US
dc.language.iso en_US en_US
dc.publisher American Astronomical Society en_US
dc.subject solar wind en_US
dc.subject turbulence en_US
dc.subject waves en_US
dc.title Alfven waves and turbulence in the solar atmosphere and solar wind en_US
dc.type Article en_US


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