Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...390..297h&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 390, no. 1, May 1, 1992, p. 297-308.
Astronomy and Astrophysics
Astrophysics
77
Magnetohydrodynamic Turbulence, Plasma Heating, Solar Corona, Turbulence Models, Heat Flux, Hydrodynamic Equations, Magnetohydrodynamic Flow, Photosphere
Scientific paper
The rate of solar coronal heating induced by the slow random motions of the dense photosphere is calculated in the framework of an essentially parameter-free model. This model assumes that these motions maintain the corona in a state of small-scale MHD turbulence. The associated dissipative effects then allow a large-scale stationary state to be established. The solution for the macroscopic coronal flow and the heating flux is first obtained assuming the effective (turbulent) dissipation coefficients to be known. In a second step these coefficients are calculated by the self-consistency argument that they should result from the level of turbulence associated with this very heating flux. For the sake of tractability the derivation is restricted to a two-dimensional situation where boundary flows are translationally symmetric. The resulting value of the heating rate and the predicted level of microturbulent velocity compare satisfactorily with the observational data.
Heyvaerts Jean
Priest Eric R.
No associations
LandOfFree
A self-consistent turbulent model for solar coronal heating does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with A self-consistent turbulent model for solar coronal heating, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and A self-consistent turbulent model for solar coronal heating will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1514320