Journal
ASTROPHYSICAL JOURNAL
Volume 788, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/788/1/9
Keywords
magnetohydrodynamics (MHD); Sun : chromosphere; Sun : corona; Sun : oscillations
Categories
Funding
- KU Leuven [GOA/2009-009]
- Interuniversity Attraction Poles Programme initiated by the Belgian Science Policy Office [IAP P7/08]
- Odysseus grant of the FWO Vlaanderen
- Spanish MINECO
- FEDER funds [AYA2011-22846]
- CAIB through the grups competitius scheme
- Spanish Ministry of Economy and Competitiveness through a Juan de la Cierva grant
- Ministry of Education, Culture, and Sport [CEF11-0012]
- UIB Vicerectorat dInvestigaci i Postgrau
- Spanish Ministerio de Educacion y Ciencia through a Ramon y Cajal grant
- MICINN/MINECO
- CAIB through the Grups Competitius scheme
- Leverhulme Trust (UK)
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Magnetohydrodynamic (MHD) kink waves have now been observed to be ubiquitous throughout the solar atmosphere. With modern instruments, they have now been detected in the chromosphere, interface region, and corona. The key purpose of this paper is to show that kink waves do not only involve purely transverse motions of solar magnetic flux tubes, but the velocity field is a spatially and temporally varying sum of both transverse and rotational motion. Taking this fact into account is particularly important for the accurate interpretation of varying Doppler velocity profiles across oscillating structures such as spicules. It has now been shown that, as well as bulk transverse motions, spicules have omnipresent rotational motions. Here we emphasize that caution should be used before interpreting the particular MHD wave mode/s responsible for these rotational motions. The rotational motions are not necessarily signatures of the classic axisymmetric torsional Alfven wave alone, because kink motion itself can also contribute substantially to varying Doppler velocity profiles observed across these structures. In this paper, the displacement field of the kink wave is demonstrated to be a sum of its transverse and rotational components, both for a flux tube with a discontinuous density profile at its boundary, and one with a more realistic density continuum between the internal and external plasma. Furthermore, the Doppler velocity profile of the kink wave is forward modeled to demonstrate that, depending on the line of sight, it can either be quite distinct or very similar to that expected from a torsional Alfven wave.
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