Three-Fluid 2.5-dimensional Magnetohydrodynamic Model of the Effective Temperature in Coronal Holes

Details Three-Fluid 2.5-dimensional Magnetohydrodynamic Model of the Effective Temperature in Coronal Holes Three-Fluid 2.5-dimensional Magnetohydrodynamic Model of the Effective Temperature in Coronal Holes

Jun 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001apj...553..935o&link_type=abstract

The Astrophysical Journal, Volume 553, Issue 2, pp. 935-940.

Astronomy and Astrophysics

Astronomy

16

Magnetohydrodynamics: Mhd, Sun: Corona, Sun: Magnetic Fields, Waves

Scientific paper

Recent SOHO Ultraviolet Coronagraph Spectrometer (UVCS) observations show that protons and minor ions are hot (Tp>106 K, Ti>107 K) and anisotropic in coronal holes. A possible cause of the large perpendicular motions is unresolved Alfvénic fluctuations in the solar wind. Using the three-fluid 2.5-dimensional MHD model, we have shown that the unresolved Alfvénic fluctuations lead to apparent proton temperature and anisotropy consistent with UVCS observations. However, Alfvén waves with realistic amplitudes cannot reproduce the O5+ perpendicular temperature and anisotropy deduced from UVCS observations. This suggests that the minor ions are heated by a different mechanism than protons.

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