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      A turbulence-driven model for heating and acceleration of the fastwind in coronal holes

      Verdini, A.; Verli, M.; Matthaeus, William H.; Oughton, Sean; Dmitruk, Pablo
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      Oughton 2010 Turbulence.pdf
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      DOI
       10.1088/2041-8205/708/2/L116
      Link
       www.iop.org
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      Citation
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      Verdini, A., Verli, M., Matthaeus, W. H., Oughton, S. & Dmitruk, P. (2010). A turbulence-driven model for heating and acceleration of the fastwind in coronal holes. Astrophysical Journal Letters, 708(2), L116-L120.
      Permanent Research Commons link: https://hdl.handle.net/10289/3647
      Abstract
      A model is presented for generation of fast solar wind in coronal holes, relying on heating that is dominated by turbulent dissipation of MHD fluctuations transported upward in the solar atmosphere. Scale-separated transport equations include large-scale fields, transverse Alfvénic fluctuations, and a small compressive dissipation due to parallel shears near the transition region. The model accounts for proton temperature, density, wind speed, and fluctuation amplitude as observed in remote sensing and in situ satellite data.
      Date
      2010
      Type
      Journal Article
      Publisher
      IOP Publishing Ltd
      Rights
      This is an author’s accepted version of an article published in the journal: Astrophysical Journal Letters. © 2010. The American Astronomical Society.
      Collections
      • Computing and Mathematical Sciences Papers [1455]
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