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Bipolar Magnetic Structures Driven by Stratified Turbulence with a Coronal Envelope

Warnecke, Jörn (author)
KTH,Stockholms universitet,Institutionen för astronomi,Nordiska institutet för teoretisk fysik (Nordita),Nordic Institute for Theoretical Physics NORDITA
Rivero Losada, Illa (author)
KTH,Stockholms universitet,Institutionen för astronomi,Nordiska institutet för teoretisk fysik (Nordita),Nordic Institute for Theoretical Physics NORDITA
Brandenburg, Axel (author)
KTH,Stockholms universitet,Institutionen för astronomi,Nordiska institutet för teoretisk fysik (Nordita),Nordic Institute for Theoretical Physics NORDITA
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Kleeorin, Nathan (author)
KTH,Stockholms universitet,Nordiska institutet för teoretisk fysik (Nordita),Ben-Gurion University of the Negev, Israel; N. I. Lobachevsky State University of Nizhny Novgorod, Russia,Nordic Institute for Theoretical Physics NORDITA
Rogachevskii, Igor (author)
KTH,Stockholms universitet,Nordiska institutet för teoretisk fysik (Nordita),Ben-Gurion University of the Negev, Israel; N. I. Lobachevsky State University of Nizhny Novgorod, Russia,Nordic Institute for Theoretical Physics NORDITA
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 (creator_code:org_t)
2013
2013
English.
In: Astrophysical Journal Letters. - 2041-8205 .- 2041-8213. ; 777:2
  • Journal article (peer-reviewed)
Abstract Subject headings
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  • We report the spontaneous formation of bipolar magnetic structures in direct numerical simulations of stratified forced turbulence with an outer coronal envelope. The turbulence is forced with transverse random waves only in the lower (turbulent) part of the domain. Our initial magnetic field is either uniform in the entire domain or confined to the turbulent layer. After about 1-2 turbulent diffusion times, a bipolar magnetic region of vertical field develops with two coherent circular structures that live during one turbulent diffusion time, and then decay during 0.5 turbulent diffusion times. The resulting magnetic field strengths inside the bipolar region are comparable to the equipartition value with respect to the turbulent kinetic energy. The bipolar magnetic region forms a loop-like structure in the upper coronal layer. We associate the magnetic structure formation with the negative effective magnetic pressure instability in the two-layer model.

Subject headings

NATURVETENSKAP  -- Fysik -- Astronomi, astrofysik och kosmologi (hsv//swe)
NATURAL SCIENCES  -- Physical Sciences -- Astronomy, Astrophysics and Cosmology (hsv//eng)

Keyword

magnetohydrodynamics (MHD)
starspots
Sun: corona
sunspots
turbulence
Astronomy
astronomi

Publication and Content Type

ref (subject category)
art (subject category)

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