Published January 10, 2010 | Version v1
Journal article Metadata-only

A TURBULENCE-DRIVEN MODEL FOR HEATING AND ACCELERATION OF THE FAST WIND IN CORONAL HOLES

Creators

  • 1. Observatoire Royale de Belgique, 3 Avenue Circulaire, 1180, Bruxelles (Belgium)
  • 2. Dipart. di Astronomia e Scienza dello Spazio, Univ. di Firenze, Largo E. Fermi 3, 50125, Firenze (Italy)
  • 3. Department of Physics and Astronomy, University of Delaware, DE 19716 (United States)
  • 4. Department of Mathematics, University of Waikato, Hamilton (New Zealand)
  • 5. Depart. Fisica, Facultad de Ciencias Exactas y Naturales, Univ. de Buenos Aires-Conicet (Argentina)

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 Alfvenic 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.

Availability note (English)

Available from http://dx.doi.org/10.1088/2041-8205/708/2/L116

Additional details

Identifiers

DOI
10.1088/2041-8205/708/2/L116;

Publishing Information

Journal Title
Astrophysical Journal Letters
Journal Volume
708
Journal Issue
2
Journal Page Range
p. L116-L120
ISSN
2041-8205

INIS

Country of Publication
United States
Country of Input or Organization
International Atomic Energy Agency (IAEA)
INIS RN
41046198
Subject category
S79: ASTROPHYSICS, COSMOLOGY AND ASTRONOMY;
Descriptors DEI
MAGNETOHYDRODYNAMICS; PROTON TEMPERATURE; REMOTE SENSING; SATELLITES; SOLAR ATMOSPHERE; SOLAR WIND; TRANSPORT THEORY; TURBULENCE
Descriptors DEC
ATMOSPHERES; FLUID MECHANICS; HYDRODYNAMICS; MECHANICS; SOLAR ACTIVITY; STELLAR ACTIVITY; STELLAR ATMOSPHERES; STELLAR WINDS