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Title: Application of a solar wind model driven by turbulence dissipation to a 2D magnetic field configuration

Although it is widely accepted that photospheric motions provide the energy source and that the magnetic field must play a key role in the process, the detailed mechanisms responsible for heating the Sun's corona and accelerating the solar wind are still not fully understood. Cranmer et al. developed a sophisticated, one-dimensional (1D), time-steady model of the solar wind with turbulence dissipation. By varying the coronal magnetic field, they obtain, for a single choice of wave properties, a realistic range of slow and fast wind conditions with a sharp latitudinal transition between the two streams. Using a 1D, time-dependent model of the solar wind of Lionello et al., which incorporates turbulent dissipation of Alfvén waves to provide heating and acceleration of the plasma, we have explored a similar configuration, obtaining qualitatively equivalent results. However, our calculations suggest that the rapid transition between slow and fast wind suggested by this 1D model may be disrupted in multidimensional MHD simulations by the requirement of transverse force balance.
Authors:
; ; ;  [1] ;  [2]
  1. Predictive Science, Inc., 9990 Mesa Rim Road, Suite 170, San Diego, CA 92121-3933 (United States)
  2. Department of Earth, Planetary, and Space Sciences, UCLA, 595 Charles E. Young Drive East, Los Angeles, CA 90095-1567 (United States)
Publication Date:
OSTI Identifier:
22370154
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 796; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ALFVEN WAVES; MAGNETIC FIELD CONFIGURATIONS; MAGNETIC FIELDS; MAGNETOHYDRODYNAMICS; ONE-DIMENSIONAL CALCULATIONS; PLASMA; SIMULATION; SOLAR WIND; SUN; TIME DEPENDENCE; TURBULENCE