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

Authors
Verdini, A.; Velli, M.; Matthaeus, W. H.; Oughton, S.; Dmitruk, Pablo Ariel
Publication Year
2010
Language
English
Format
article
Status
Published version
Description
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. © 2010. The American Astronomical Society. All rights reserved..
Fil: Verdini, A.. Observatoire Royale de Belgique; Bélgica
Fil: Velli, M.. Università degli Studi di Firenze; Italia
Fil: Matthaeus, W. H.. University Of Delaware; Estados Unidos
Fil: Oughton, S.. University Of Waikato; Nueva Zelanda
Fil: Dmitruk, Pablo Ariel. Universidad de Buenos Aires; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Física de Buenos Aires. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Física de Buenos Aires; Argentina
Subject
MHD
SOLAR WIND
TURBULENCE
WAVES
Astronomía
Ciencias Físicas
CIENCIAS NATURALES Y EXACTAS
Access level
Open access
License
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repository
CONICET Digital (CONICET)
Institution
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identifier
oai:ri.conicet.gov.ar:11336/59121