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

Autores
Verdini, A.; Velli, M.; Matthaeus, W.H.; Oughton, S.; <div class="autor_fcen" id="2615">Dmitruk, P.</div>
Año de publicación
2010
Idioma
inglés
Tipo de recurso
artículo
Estado
Versión publicada
Descripción
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:Dmitruk, P. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.
Fuente
Astrophys. J. Lett. 2010;708(2 PART 2):L116-L120
Materia
MHD
Solar wind
Turbulence
Waves
Nivel de accesibilidad
Acceso abierto
Licencia
http://creativecommons.org/licenses/by/2.5/ar
Repositorio
Biblioteca Digital (UBA-FCEN)
Institución
Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
OAI Identificador
snrd:HASH4ee68a18fe5a7307991447