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Damping of Non-Isothermal Hot Coronal Loop Oscillations

Luna-Cardozo, M., Erdelyi, R. and Mendoza-Briceno, C.A. (2008) Damping of Non-Isothermal Hot Coronal Loop Oscillations. In: Erdelyi, R. and Mendoza-Briceno, C.A., (eds.) Waves & Oscillations in the Solar Atmosphere: Heating and Magneto-Seismology. Waves & Oscillations in the Solar Atmosphere: Heating and Magneto-Seismology: IAU Symposium 247, September 17-22, 2007, Porlamar, Isla de Margarita, Venezuela. Proceedings of the International Astronomical Union , 3 (s247). Cambridge University Press , Cambridge , pp. 316-319. ISBN 978-0-52187-4694

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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.

Item Type: Proceedings Paper
Institution: The University of Sheffield
Academic Units: The University of Sheffield > Faculty of Science (Sheffield) > School of Mathematics and Statistics (Sheffield)
Depositing User: Mrs Megan Hobbs
Date Deposited: 16 Mar 2010 17:56
Last Modified: 16 Nov 2015 11:48
Published Version: http://dx.doi.org/10.1017/S1743921308015020
Status: Published
Publisher: Cambridge University Press
Identification Number: 10.1017/S1743921308015020
URI: http://eprints.whiterose.ac.uk/id/eprint/10583

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