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P-mode induced convective collapse in vertical expanding magnetic flux tubes?

Published online by Cambridge University Press:  12 September 2017

D. Utz Open the ORCID record for D. Utz [Opens in a new window] ,
T. Van Doorsselaere ,
N. Magyar ,
M. Bárta  and
J. I. Campos Rozo Open the ORCID record for J. I. Campos Rozo [Opens in a new window]
D. Utz
Affiliation:
IGAM, Institute of Physics, Karl-Franzens University Graz, Universitätsplatz 5II, AT-8010, Graz, Austria email: [email protected] Centre for mathematical Plasma Astrophysics, KU Leuven, Celestijnenlaan 200B, bus 2400, B-3001, Leuven, Belgium email: [email protected]
T. Van Doorsselaere
Affiliation:
Centre for mathematical Plasma Astrophysics, KU Leuven, Celestijnenlaan 200B, bus 2400, B-3001, Leuven, Belgium email: [email protected]
N. Magyar
Affiliation:
Centre for mathematical Plasma Astrophysics, KU Leuven, Celestijnenlaan 200B, bus 2400, B-3001, Leuven, Belgium email: [email protected]
M. Bárta
Affiliation:
Astronomical Observatory of the Czech Academy of Sciences, Friccova 298, Cz-251 65, Ondrejov, Czech Republic email: [email protected]
J. I. Campos Rozo
Affiliation:
National Astronomical Observatory of Colombia, National University of Colombia, Carrera 30 #45-03 ed. 413, Bogota, Colombia email: [email protected]
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Abstract

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Small-scale kG strong magnetic field elements in the solar photosphere are often identified as so-called magnetic bright points (MBPs). In principle these MBPs represent the cross-section of a vertical, strong, magnetic flux tube which is expanding with height in the solar atmosphere. As these magnetic elements represent possible MHD wave guides, a significant interest has been already paid to them from the viewpoint of observations and simulations. In this work we would like to shed more light on a possible scenario for the creation of such strong magnetic field concentrations. The accepted standard scenario involves the convective collapse process. In this ongoing work we will show indications that this convective collapse process may become triggered by sufficiently strong pressure disturbances. However, it is highly unlikely that p-mode waves can be of such a strength.

Keywords

magnetic flux tubesMHD-simulationconvective collapsep-mode waves
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S327: Fine Structure and Dynamics of the Solar Atmosphere , October 2016 , pp. 86 - 93
Copyright
Copyright © International Astronomical Union 2017 

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