Self-heating and its possible relationship to chromospheric heating in slowly rotating stars
arXiv:0909.5400 · doi:10.1111/j.1365-2966.2009.16159.x
Abstract
The efficiency of nonmodal self-heating by acoustic wave perturbations is examined. Considering different kinds of kinematically complex velocity patterns we show that nonmodal instabilities arising in these inhomogeneous flows may lead to significant amplification of acoustic waves. Subsequently, the presence of viscous dissipation damps these amplified waves and causes the energy transfer back to the background flow in the form of heat; viz. closes the "self-heating" cycle and contributes to the net heating of the flow patterns and the chromospheric network as a whole. The acoustic self-heating depends only on the presence of kinematically complex flows and dissipation. It is argued that together with other mechanisms of nonlinear nature the self-heating \textit{may be} a probable additinal mechanism of nonmagnetic chromospheric heating in the Sun and other solar-type stars with slow rotation and extended convective regions.
8 pages, 3 figures
References in corpus (5)
- Numerical simulation of the three-dimensional structure and dynamics of the non-magnetic solar chromosphere
- Giant Chromospheric Anemone Jet Observed with Hinode and Comparison with Magnetohydrodynamic Simulations: Evidence of Propagating Alfven Waves and Magnetic Reconnection
- Farley-Buneman Instability in the Solar Chromosphere
- Swirling astrophysical flows - efficient amplifiers of Alfven waves
- Amplification of MHD waves in swirling astrophysical flows