Heating of coronal holes by phase mixing.

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Abstract

A two-dimensional, analytical, self-similar solution to the Alfven wave phase mixing equations is presented for a coronal hole model. The solution shows clearly that the damping of the waves with height follows the scaling predicted by Heyvaerts & Priest 1983 at low heights, before switching to an algebraic decay at large heights. The ohmic dissipation is calculated and it is shown that the maximum dissipation occurs at a height that scales with eta(1/3). However, the total Ohmic dissipation is, of course, independent of the resistivity. Using realistic solar parameters it appears that phase mixing is a viable mechanism for heating the lower corona provided either the frequency of photospheric motions is sufficiently large or the background Alfven velocity is sufficiently small.

Original languageEnglish
Pages (from-to)957-961
Number of pages6
JournalAstronomy & Astrophysics
Volume318
Publication statusPublished - Feb 1997

Keywords

  • MHD
  • waves
  • Sun, corona
  • KELVIN-HELMHOLTZ INSTABILITY
  • RESONANT ABSORPTION
  • SURFACE-WAVES
  • ALFVEN WAVES
  • LOOPS

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