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Electric Current Filamentation Induced by 3D Plasma Flows in the Solar Corona
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SYSNO ASEP 0479460 Document Type J - Journal Article R&D Document Type Journal Article Subsidiary J Článek ve WOS Title Electric Current Filamentation Induced by 3D Plasma Flows in the Solar Corona Author(s) Nickeler, Dieter Horst (ASU-R) RID, ORCID
Wiegelmann, T. (DE)
Karlický, Marian (ASU-R) RID, ORCID
Kraus, Michaela (ASU-R) RID, ORCIDSource Title Astrophysical Journal - ISSN 0004-637X
Roč. 837, č. 2 (2017), 104/1-104/11Number of pages 11 s. Publication form Print - P Language eng - English Country US - United States Keywords magnetohydrodynamics ; Sun ; corona Subject RIV BN - Astronomy, Celestial Mechanics, Astrophysics OECD category Astronomy (including astrophysics,space science) R&D Projects GA16-05011S GA ČR - Czech Science Foundation (CSF) GA16-13277S GA ČR - Czech Science Foundation (CSF) Institutional support ASU-R - RVO:67985815 UT WOS 000401172400002 EID SCOPUS 85015943757 DOI 10.3847/1538-4357/aa6043 Annotation Many magnetic structures in the solar atmosphere evolve rather slowly, so they can be assumed as (quasi-) static or (quasi-) stationary and represented via magnetohydrostatic (MHS) or stationary magnetohydrodynamic (MHD) equilibria, respectively. While exact 3D solutions would be desired, they are extremely difficult to find in stationary MHD. We construct solutions with magnetic and flow vector fields that have three components depending on all three coordinates. We show that the noncanonical transformation method produces quasi-3D solutions of stationary MHD by mapping 2D or 2.5D MHS equilibria to corresponding stationary MHD states, that is, states that display the same field-line structure as the original MHS equilibria. These stationary MHD states exist on magnetic flux surfaces of the original 2D MHS states. Although the flux surfaces and therefore also the equilibria have a 2D character, these stationary MHD states depend on all three coordinates and display highly complex currents. The existence of geometrically complex 3D currents within symmetric field-line structures provides the basis for efficient dissipation of the magnetic energy in the solar corona by ohmic heating. We also discuss the possibility of maintaining an important subset of nonlinear MHS states, namely force-free fields, by stationary flows. We find that force-free fields with nonlinear flows only arise under severe restrictions of the field-line geometry and of the magnetic flux density distribution. Workplace Astronomical Institute Contact Radka Svašková, bibl@asu.cas.cz, Tel.: 323 620 326 Year of Publishing 2018
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