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Propagation and damping of Alfven waves in low solar atmosphere SCIE SCOPUS

Title
Propagation and damping of Alfven waves in low solar atmosphere
Authors
Ryu, Chang-MoCong Tuan Huynh
Date Issued
2017-10
Publisher
WILEY-BLACKWELL
Abstract
Propagation and damping of Alfven waves in the inner solar corona are studied using a 2D magnetohydrodynamics (MHD) simulation code with realistic density and temperature profiles in a uniform background magnetic field. A linear wave is launched by ascribing a sinusoidal fluid motion at about 1000 km from the surface of the Sun, which is shown to generate Alfvenic wave motions along the height. The 2D MHD simulation shows that for B-0 approximate to 3G, Alfven waves of about 10(-2) Hz with an infinite horizontal length-scale can penetrate into the corona, transferring about 90 per cent their energies. This raises the possibility that the wave can be dissipated by various physical processes. The results show that the propagating wave can effectively damp via viscosity in the lower region of the corona, if a horizontal scale of granular size is incorporated.
Keywords
MAGNETIC-FIELD; WIND
URI
https://oasis.postech.ac.kr/handle/2014.oak/92012
DOI
10.1093/mnras/stx1425
ISSN
0035-8711
Article Type
Article
Citation
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, vol. 471, no. 2, page. 2237 - 2241, 2017-10
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