Physics
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sp51c04e&link_type=abstract
American Geophysical Union, Spring Meeting 2001, abstract #SP51C-04 INVITED
Physics
7509 Corona, 7524 Magnetic Fields, 7835 Magnetic Reconnection, 7863 Turbulence
Scientific paper
We present reduced MHD turbulence scenarios for coronal heating in a coronal loop using the 2D cross section approximation (Einaudi and Velli 1999) and the complete boundary value problem 3D simulations. 2D runs are carried out for longer times and greater resolution with different types of forcing, allowing the exploration of the dependence of the heating rates, statistical properties and scalings with the nature of the photospheric forcing. 3D runs are carried out using only some selected photospheric forcings. It is found that line-tying partially inhibits the inverse cascade which dominates the 2D approximation. In 3D the overall behavior of the system is sensitive to the 3 time-scales present in the system, namely propagation time along the loop, dynamical transverse time and photospheric forcing correlation time. Coronal heating scaling laws are reviewed in the light of simulation results
Betta Rita
Einaudi Giorgio
Velli M. M.
No associations
LandOfFree
Coronal Heating via MHD Turbulence 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 Coronal Heating via MHD Turbulence, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Coronal Heating via MHD Turbulence will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1279563