2010/10/20 by Christoph Kuckein, C. Kuckein, Kuckein, Christoph +6
Physics and Astronomy · #FOS: Physical sciences #Solar and Space Plasma Dynamics #Solar and Stellar Astrophysics (astro-ph.SR) #astro-ph.SR
paper · pdf · doi:10.48550/arxiv.1010.4260
4 pages, to appear in the ASP Conference Proceedings of the "Solar Polarization Workshop 6"
arxiv created 2010/10/20 · openalex publication_date 2010/10/20 · arxiv updated 2010/10/21 · openalex created_date 2022/10/06 · openalex updated_date 2026/07/28
Using spectropolarimetric data of an Active Region (AR) filament we have carried out inversions in order to infer vector magnetic fields in the photosphere (Si I line) and in the chromosphere (He I line). Our filament lies above the polarity inversion line (PIL) situated close to disk center and presents strong Zeeman-like signatures in both photospheric and chromospheric lines. Pore-like formations with both polarities are identified in the continuum under the PIL. The azimuth ambiguity is solved at both heights using the AZAM code. A comparison between the photospheric and chromospheric vector magnetic fields revealed that they are well aligned in some areas of the filament. However, especially at chromospheric heights, the magnetic field is mostly aligned with the dark threads of the filament. Velocity signatures indicating upflows of field lines are found at both heights. The combination of all these findings strongly suggests an emerging flux rope scenario.