期刊
ASTROPHYSICAL JOURNAL
卷 815, 期 1, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/815/1/10
关键词
methods: numerical; Sun: chromosphere; Sun: corona; Sun: magnetic fields; Sun: photosphere
资金
- Bundesministerium fur Wirtschaft und Technologie through Deutsches Zentrum fur Luft- und Raumfahrt e.V. (DLR) [50 OU 0401]
- Innovationsfonds of the President of the Max Planck Society (MPG)
- Spanish MICINN (European FEDER funds) [ESP2006-13030-C06, AYA2009-14105-C06]
- NASA [NNX08AH38G]
- U.K.'s Science and Technology Facilities Council
- GA CR [13-24782S]
- BK21 plus program through the National Research Foundation (NRF) - Ministry of Education of Korea
- [RVO:67985815]
- STFC [ST/K000950/1] Funding Source: UKRI
Our aim is to model the three-dimensional magnetic field structure of the upper solar atmosphere, including regions of non-negligible plasma beta. We use high-resolution photospheric magnetic field measurements from SUNRISE/IMaX as the boundary condition for a magneto-static magnetic field model. The high resolution of IMaX allows us to resolve the interface region between the photosphere and corona, but modeling this region is challenging for the following reasons. While the coronal magnetic field is thought to be force-free (the Lorentz force vanishes), this is not the case in the mixed plasma beta environment in the photosphere and lower chromosphere. In our model, pressure gradients and gravity forces are self-consistently taken into account and compensate for the non-vanishing Lorentz force. Above a certain height (about 2 Mm) the non-magnetic forces become very weak and consequently the magnetic field becomes almost force-free. Here, we apply a linear approach where the electric current density consists of a superposition of a field-line parallel current and a current perpendicular to the Sun' s gravity field. We illustrate the prospects and limitations of this approach and give an outlook for an extension toward a nonlinear model.
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