0470592 - ASÚ 2017 RIV DE eng J - Článek v odborném periodiku
Balthasar, H. - Gömöry, P. - Gonzalez Manrique, S. J. - Kuckein, C. - Kavka, J. - Kučera, A. - Schwartz, P. - Vašková, R. - Berkefeld, T. - Collados Vera, M. - Denker, C. - Feller, A. - Hofmann, A. - Lagg, A. - Nicklas, H. - Orozco Suárez, D. - Pastor Yabar, A. - Schlichenmaier, R. - Schmidt, D. - Schmidt, W. - Sigwarth, M. - Sobotka, Michal - Solanki, S.K. - Soltau, D. - Staude, J. - Strassmeier, K.G. - Volkmer, R. - von der Lühe, O. - Waldmann, T.A.
Spectropolarimetric observations of an arch filament system with the GREGOR solar telescope.
Astronomische Nachrichten. Roč. 337, č. 10 (2016), s. 1050-1056. ISSN 0004-6337. E-ISSN 1521-3994.
[Dynamic Sun - Exploring the Many Facets of Solar Eruptive Events. Potsdam, 26.10.2015-29.10.2015]
Institucionální podpora: RVO:67985815
Klíčová slova: Sun * filaments * photosphere
Kód oboru RIV: BN - Astronomie a nebeská mechanika, astrofyzika
Impakt faktor: 0.916, rok: 2016 ; AIS: 0.439, rok: 2016
DOI: https://doi.org/10.1002/asna.201612432

Arch filament systems occur in active sunspot groups, where a fibril structure connects areas of opposite magnetic polarity, in contrast to active region filaments that follow the polarity inversion line. We used the GREGOR Infrared Spectrograph (GRIS) to obtain the full Stokes vector in the spectral lines SiI lambda 1082.7 nm, He I lambda 1083.0 nm, and Ca I lambda 1083.9 nm. We focus on the near-infrared calcium line to investigate the photospheric magnetic field and velocities, and use the line core intensities and velocities of the helium line to study the chromospheric plasma. The individual fibrils of the arch filament system connect the sunspot with patches of magnetic polarity opposite to that of the spot. These patches do not necessarily coincide with pores, where the magnetic field is strongest. Instead, areas are preferred not far from the polarity inversion line. These areas exhibit photospheric downflows of moderate velocity, but significantly higher downflows of up to 30 km s(-1) in the chromospheric helium line. Our findings can be explained with new emerging flux where the matter flows downward along the field lines of rising flux tubes, in agreement with earlier results.
Trvalý link: http://hdl.handle.net/11104/0268186