Computer Science
Scientific paper
Aug 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...3e..17v&link_type=abstract
Solar Active Regions and 3D Magnetic Structure, 26th meeting of the IAU, Joint Discussion 3, 16-17 August, 2006, Prague, Czech R
Computer Science
Scientific paper
One of the most interesting phenomena appearances on the Sun is the high temperature of the solar corona, which reaches 10^6 K (compared with 5×10^3 K at the level of the photosphere). To maintain such a high temperature and compensate for radiative cooling, the constant inflow of energy is needed. The necessary energy is considered to be carried by Alfvén waves. Alfvén waves also play an important role in the heating of the solar wind and in transporting energy from the Sun to the Earth. However, MHD Alfvén waves are weakly damping and there is the problem of the transformation of energy from waves to plasma particles. Therefore, solar corona heating by Alfvén waves can be connected with transformation of longwaved Alfvén waves to shortwaved kinetic Alfvén waves. Kinetic Alfvén waves are rapid damped waves and can effectively transfer energy to plasma particles. The nonlinear mechanism of Alfvén wave transformation to kinetic Alfvén waves and magnetoacoustic waves in the solar corona plasma with small plasma parameter b<<1 is investigated. The parametric instability, where Alfvén wave is the pump wave, is considered as the generation mechanism. Using a two-fluid model and Maxwell's equation, we derive a nonlinear dispersion relation governing this three-wave interaction processes, the instability growth rate and the time of instability development. Our theoretical investigations show that the decay of Alfvén waves into kinetic Alfvén and magnetoacoustic waves can cause to a solar corona heating.
Voitsekhovska A. D.
Yukhimuk A. K.
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