期刊
ASTRONOMY & ASTROPHYSICS
卷 551, 期 -, 页码 -出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201220617
关键词
magnetohydrodynamics (MHD); Sun: atmosphere; Sun: corona; Sun: magnetic topology; Sun: oscillations; waves
资金
- STFC
- Royal Society
- Royal Society Leverhulme Trust
- STFC grant
- Spanish Ministerio de Educacion y Ciencia through a Ramon y Cajal grant
- MICINN/MINECO
- FEDER Funds [AYA2011-22846]
- CAIB through Grups Competitius scheme
- FEDER Funds
- SFC (SRIF)
- STFC [ST/K000950/1, ST/H008799/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/K000950/1, ST/H008799/1] Funding Source: researchfish
Aims. We investigate the spatial damping of propagating kink waves in an inhomogeneous plasma. In the limit of a thin tube surrounded by a thin transition layer, an analytical formulation for kink waves driven in from the bottom boundary of the corona is presented. Methods. The spatial form for the damping of the kink mode was investigated using various analytical approximations. When the density ratio between the internal density and the external density is not too large, a simple differential-integral equation was used. Approximate analytical solutions to this equation are presented. Results. For the first time, the form of the spatial damping of the kink mode is shown analytically to be Gaussian in nature near the driven boundary. For several wavelengths, the amplitude of the kink mode is proportional to (1+exp(-z(2)/L-g(2)))/2, where L-g(2) = 16/epsilon kappa(2)k(2). Although the actual value of 16 in L-g depends on the particular form of the driver, this form is very general and its dependence on the other parameters does not change. For large distances, the damping profile appears to be roughly linear exponential decay. This is shown analytically by a series expansion when the inhomogeneous layer width is small enough.
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