 |
| Titel |
Radial evolution of intermittent heat flux in solar coronal holes |
| VerfasserIn |
S. A. Markovskii, J. V. Hollweg |
| Medientyp |
Artikel
|
| Sprache |
Englisch
|
| ISSN |
1023-5809
|
| Digitales Dokument |
URL |
| Erschienen |
In: Nonlinear Processes in Geophysics ; 11, no. 4 ; Nr. 11, no. 4 (2004-11-08), S.485-494 |
| Datensatznummer |
250009329
|
| Publikation (Nr.) |
 copernicus.org/npg-11-485-2004.pdf |
|
|
|
|
|
| Zusammenfassung |
| Recently, we suggested that the source of ion heating in solar coronal holes
is small-scale reconnection events (microflares) at the coronal base. The
microflares launch intermittent heat flux up into the corona exciting ion
cyclotron waves through a plasma microinstability. The ions are heated by
these waves during the microflare bursts and then evolve with no energy input
between the bursts. The overall coronal heating by this mechanism is a summed
effect of all microflare bursts during the expansion time of the solar wind
and adiabatic cooling between the microflares. The intermittent heat flux
produced by the microflares was modeled as electron beams with constant speed
and temperature for simplicity. In this paper, we consider a more
sophisticated model of the heat flux taking into account the action of the
mirror force and the charge separation electric field on the beam particles.
We show that the radial evolution of the heat flux is determined mainly by
the beam expansion along the magnetic field roughly at the root mean square
velocity of the beam particles, while the variation of the beam bulk speed
and thermal energy is less important. |
| |
|
| Teil von |
|
|
|
|
|
|
|
|