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The effect of a magnetic field on the damping of slow magnetosonic waves in the solar corona
The influence of the magnetic field strength and the associated plasma
parameter β (beta) on the dynamics of slow magnetosonic (MS) waves
in plasma loops of the solar corona was studied. It has
been demonstrated that the feedback effect of the thermal imbalance
induced by MS waves with these waves makes it possible to explain the
observed anomalously low Q factor of the waves of this type without
involving anomalously high values of the thermal conductivity and viscosity
coefficients. The results of this study are a theoretical basis for
diagnosing key parameters of the Solar corona plasma, such as the magnetic
field and the corona heating function by magnetohydrodynamic seismology
using observations of solar and stellar flares both in the radio
range, in particular with the RATAN-600 SAO RAS telescope after
implementation of the guidance mode and with the help of SAO RAS optical
telescopes. A separate significant result is the establishment of the
application field of the infinite magnetic field approximation which greatly
simplifies theoretical modeling of dynamic and thermal processes in plasma
loops of the Solar corona.
Authors:
V.M. Nakariakov (SAO RAS) in cooperation with Duckenfield T.J.
(the University of Warwick, Great Britain), Kolotkov D.Ju. (the University
of Warwick, Great Britain), ISTP SB RAS)
Published:
1. Duckenfield T.J., Kolotkov D.Y., Nakariakov V.M., The effect of
the magnetic field on the damping of slow waves in the solar corona,
2021, Astron. Astrophys., 646, A155, DOI:10.1051/0004-6361/202039791.
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