Physics
Scientific paper
Jun 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006soph..236..137k&link_type=abstract
Solar Physics, Volume 236, Issue 1, pp.137-153
Physics
7
Scientific paper
The damping of MHD waves in solar coronal magnetic field is studied taking into account thermal conduction and compressive viscosity as dissipative mechanisms. We consider viscous homogeneous unbounded solar coronal plasma permeated by a uniform magnetic field. A general fifth-order dispersion relation for MHD waves has been derived and solved numerically for different solar coronal regimes. The dispersion relation results three wave modes: slow, fast, and thermal modes. Damping time and damping per periods for slow- and fast-mode waves determined from dispersion relation show that the slow-mode waves are heavily damped in comparison with fast-mode waves in prominences, prominence-corona transition regions (PCTR), and corona. In PCTRs and coronal active regions, wave instabilities appear for considered heating mechanisms. For same heating mechanisms in different prominences the behavior of damping time and damping per period changes significantly from small to large wavenumbers. In all PCTRs and corona, damping time always decreases linearly with increase in wavenumber indicate sharp damping of slow- and fast-mode waves.
Kumar Nagendra
Kumar Pradeep P.
No associations
LandOfFree
Viscous Damping of Non-Adiabatic MHD Waves in an Unbounded Solar Coronal Plasma 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 Viscous Damping of Non-Adiabatic MHD Waves in an Unbounded Solar Coronal Plasma, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Viscous Damping of Non-Adiabatic MHD Waves in an Unbounded Solar Coronal Plasma will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1327419