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Properties of the prominence magnetic field and plasma distributions as obtained from 3D whole-prominence fine structure modeling
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SYSNO ASEP 0469491 Document Type J - Journal Article R&D Document Type Journal Article Subsidiary J Článek ve WOS Title Properties of the prominence magnetic field and plasma distributions as obtained from 3D whole-prominence fine structure modeling Author(s) Gunár, Stanislav (ASU-R) RID, ORCID
Mackay, D. H. (GB)Source Title Astronomy & Astrophysics. - : EDP Sciences - ISSN 0004-6361
Roč. 592, August (2016), A60/1-A60/10Number of pages 10 s. Publication form Online - E Language eng - English Country FR - France Keywords Sun ; filaments ; prominences Subject RIV BN - Astronomy, Celestial Mechanics, Astrophysics OECD category Astronomy (including astrophysics,space science) R&D Projects GA16-17586S GA ČR - Czech Science Foundation (CSF) Institutional support ASU-R - RVO:67985815 UT WOS 000384722600053 EID SCOPUS 84979992237 DOI https://doi.org/10.1051/0004-6361/201527704 Annotation We analyze distributions of the magnetic field strength and prominence plasma (temperature, pressure, plasma beta, and mass) using the 3D whole-prominence fine structure model. We show that in the modeled prominence, the variations of the magnetic field strength and its orientation are insignificant on scales comparable to the smallest dimensions of the observed prominence fine structures. We also show the ability of the 3D whole-prominence fine structure model to reveal the distribution of the prominence plasma with respect to its temperature within the prominence volume. This provides new insights into the composition of the prominence-corona transition region. We further demonstrate that the values of the plasma beta are small throughout the majority of the modeled prominences when realistic photospheric magnetic flux distributions and prominence plasma parameters are assumed. While this is generally true, we also find that in the region with the deepest magnetic dips, the plasma beta may increase towards unity. Finally, we show that the mass of the modeled prominence plasma is in good agreement with the mass of observed non-eruptive prominences. Workplace Astronomical Institute Contact Anežka Melichárková, bibl@asu.cas.cz, Tel.: 323 620 326 Year of Publishing 2017
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