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

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dc.contributor.authorVerdini, A.
dc.contributor.authorVerli, M.
dc.contributor.authorMatthaeus, William H.
dc.contributor.authorOughton, Sean
dc.contributor.authorDmitruk, Pablo
dc.date.accessioned2010-02-26T03:52:43Z
dc.date.available2010-02-26T03:52:43Z
dc.date.issued2010
dc.description.abstractA 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.en
dc.format.mimetypeapplication/pdf
dc.identifier.citationVerdini, 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.en
dc.identifier.doi10.1088/2041-8205/708/2/L116en
dc.identifier.urihttps://hdl.handle.net/10289/3647
dc.language.isoen
dc.publisherIOP Publishing Ltden_NZ
dc.relation.isPartOfAstrophysical Journal Lettersen_NZ
dc.relation.urihttp://www.iop.org/EJ/abstract/2041-8205/708/2/L116en
dc.rightsThis is an author’s accepted version of an article published in the journal: Astrophysical Journal Letters. © 2010. The American Astronomical Society.en
dc.subjectMHDen
dc.subjectsolar winden
dc.subjectturbulenceen
dc.subjectwavesen
dc.titleA turbulence-driven model for heating and acceleration of the fastwind in coronal holesen
dc.typeJournal Articleen
pubs.begin-page116en_NZ
pubs.elements-id34744
pubs.end-pageL120en_NZ
pubs.issue2en_NZ
pubs.volume708en_NZ
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