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Damping of non-isothermal hot coronal loops oscillations

Published online by Cambridge University Press:  01 September 2007

M. Luna-Cardozo ,
R. Erdélyi  and
César A. Mendoza-Briceño
M. Luna-Cardozo
Affiliation:
SP2RC, Department of Applied Mathematics, University of Sheffield, Sheffield S3 7RH, UK emails: m.luna@sheffield.ac.uk; robertus@sheffield.ac.uk
R. Erdélyi
Affiliation:
SP2RC, Department of Applied Mathematics, University of Sheffield, Sheffield S3 7RH, UK emails: m.luna@sheffield.ac.uk; robertus@sheffield.ac.uk
César A. Mendoza-Briceño
Affiliation:
Centro de Física Fundamental CFF, Facultad de Ciencias, Universidad de Los Andes, La Hechicera, Mérida 5101, Venezuela, email: cesar@ula.ve
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Abstract

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Here we investigate longitudinal waves in non-isothermal hot (T ≥ 5.0 MK) coronal loops. Motivated by SOHO SUMER and Yohkoh SXT observations and taking into account gravitational stratification, thermal conduction, compressive viscosity, radiative cooling, and heating, the governing equations of 1D hydrodynamics is solved numerically for standing wave oscillations along a magnetic field line. A semicircular shape is chosen to represent a coronal loop. It was found that the decay time of standing waves decreases with the increase of the initial temperature and the periods of oscillations are affected by the different initial velocities and loop lengths studied by the numerical experiments. The predicted decay times are within the range of values inferred from Doppler-shift oscillations observed by SUMER in hot coronal loops.

Keywords

waveshydrodynamicsSun: CoronaSun: oscillations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S247: Waves & Oscillations in the Solar Atmosphere: Heating and Magneto-Seismology , September 2007 , pp. 316 - 319
Copyright
Copyright © International Astronomical Union 2008

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