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 language | English |
---|---|
Pages (from-to) | 957-961 |
Number of pages | 6 |
Journal | Astronomy & Astrophysics |
Volume | 318 |
Publication status | Published - Feb 1997 |
Keywords
- MHD
- waves
- Sun, corona
- KELVIN-HELMHOLTZ INSTABILITY
- RESONANT ABSORPTION
- SURFACE-WAVES
- ALFVEN WAVES
- LOOPS