期刊
ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
卷 229, 期 1, 页码 -出版社
IOP Publishing Ltd
DOI: 10.3847/1538-4365/aa582f
关键词
Sun: chromosphere; Sun: corona; Sun: magnetic fields; Sun: photosphere
资金
- Max Planck Foundation
- Strategic Innovations Fund of the President of the Max Planck Society (MPG), DLR
- members of the Max Planck Society
- Ministerio de Economia y Competitividad [ESP2013-47349-C6, ESP2014-56169-C6]
- European FEDER funds
- NASA [NNX13AE95G]
- BK21 plus program through the National Research Foundation (NRF) - Ministry of Education of Korea
- DLR [50 OC 1301, WI 3211/4-1]
- UK's Science and Technology Facilities Council via Consolidated [ST/K000950/1, ST/N000609/1]
- GA CR [16-05011S, 16-13277S]
- [RVO:67985815]
- Science and Technology Facilities Council [ST/H001964/1, ST/K000950/1, ST/N000609/1] Funding Source: researchfish
- STFC [ST/K000950/1, ST/N000609/1, ST/H001964/1] Funding Source: UKRI
Magneto-static models may overcome some of the issues facing force-free magnetic field extrapolations. So far they have seen limited use and have faced problems when applied to quiet-Sun data. Here we present a first application to an active region. We use solar vector magnetic field measurements gathered by the IMaX polarimeter during the flight of the SUNRISE balloon-borne solar observatory in 2013 June as boundary conditions for a magneto-static model of the higher solar atmosphere above an active region. The IMaX data are embedded in active region vector magnetograms observed with SDO/HMI. This work continues our magneto-static extrapolation approach, which was applied earlier to a quiet-Sun region observed with SUNRISE I. In an active region the signal-to-noise-ratio in the measured Stokes parameters is considerably higher than in the quiet-Sun and consequently the IMaX measurements of the horizontal photospheric magnetic field allow us to specify the free parameters of the model in a special class of linear magneto-static equilibria. The high spatial resolution of IMaX (110-130 km, pixel size 40 km) enables us to model the non-force-free layer between the photosphere and the mid-chromosphere vertically by about 50 grid points. In our approach we can incorporate some aspects of the mixed beta layer of photosphere and chromosphere, e.g., taking a finite Lorentz force into account, which was not possible with lower-resolution photospheric measurements in the past. The linear model does not, however, permit us to model intrinsic nonlinear structures like strongly localized electric currents.
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