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Tracking Downflows from the Chromosphere to the Photosphere in a Solar Arch Filament System
González Manrique,Sergio Javier1; Kuckein,Christoph2; Pastor Yabar,Adur3; Diercke,Andrea2,4; Collados,Manuel5; G?m?ry,Peter1; Zhong,Sihui6,7; Hou,Yijun6,7; Denker,Carsten2
2020-02-10
Source PublicationThe Astrophysical Journal
ISSN0004-637X
Volume890Issue:1
AbstractAbstract We study the dynamics of plasma along the legs of an arch filament system (AFS) from the chromosphere to the photosphere, observed with high-cadence spectroscopic data from two ground-based solar telescopes: the GREGOR telescope (Tenerife) using the GREGOR Infrared Spectrograph in the He i 10830?? range and the Swedish Solar Telescope (La Palma) using the CRisp Imaging Spectro-Polarimeter to observe the Ca ii 8542?? and Fe i 6173?? spectral lines. The temporal evolution of the draining of the plasma was followed along the legs of a single arch filament from the chromosphere to the photosphere. The average Doppler velocities inferred at the upper chromosphere from the He i 10830?? triplet reach velocities up to 20–24?km?s?1, and in the lower chromosphere and upper photosphere the Doppler velocities reach up to 11?km?s?1 and 1.5?km?s?1 in the case of the Ca ii 8542?? and Si i 10827?? spectral lines, respectively. The evolution of the Doppler velocities at different layers of the solar atmosphere (chromosphere and upper photosphere) shows that they follow the same line-of-sight (LOS) velocity pattern, which confirms the observational evidence that the plasma drains toward the photosphere as proposed in models of AFSs. The Doppler velocity maps inferred from the lower photospheric Ca i 10839?? or Fe i 6173?? spectral lines do not show the same LOS velocity pattern. Thus, there is no evidence that the plasma reaches the lower photosphere. The observations and the nonlinear force-free field (NLFFF) extrapolations demonstrate that the magnetic field loops of the AFS rise with time. We found flow asymmetries at different footpoints of the AFS. The NLFFF values of the magnetic field strength help us to explain these flow asymmetries.
KeywordSolar chromosphere Solar photosphere Observational astronomy Astronomy data analysis High resolution spectroscopy
DOI10.3847/1538-4357/ab6cee
Language英语
WOS IDIOP:0004-637X-890-1-ab6cee
PublisherThe American Astronomical Society
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Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/53975
Collection中国科学院国家天文台
Affiliation1.Astronomical Institute, Slovak Academy of Sciences, 05960 Tatranská Lomnica, Slovak Republic; smanrique@ta3.sk
2.Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany
3.Leibniz-Institut für Sonnenphysik (KIS), Sch?neckstra?e 6, D-79104, Freiburg, Germany
4.Universit?t Potsdam, Institut für Physik und Astronomie, Karl-Liebknecht-Str. 24-25, D-14476 Potsdam, Germany
5.Instituto de Astrofísica de Canarias, c/Vía Láctea s/n, E-38205 La Laguna, Tenerife, Spain
6.CAS Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People’s Republic of China
7.University of Chinese Academy of Sciences, Beijing 100049, People’s Republic of China
Recommended Citation
GB/T 7714
González Manrique,Sergio Javier,Kuckein,Christoph,Pastor Yabar,Adur,et al. Tracking Downflows from the Chromosphere to the Photosphere in a Solar Arch Filament System[J]. The Astrophysical Journal,2020,890(1).
APA González Manrique,Sergio Javier.,Kuckein,Christoph.,Pastor Yabar,Adur.,Diercke,Andrea.,Collados,Manuel.,...&Denker,Carsten.(2020).Tracking Downflows from the Chromosphere to the Photosphere in a Solar Arch Filament System.The Astrophysical Journal,890(1).
MLA González Manrique,Sergio Javier,et al."Tracking Downflows from the Chromosphere to the Photosphere in a Solar Arch Filament System".The Astrophysical Journal 890.1(2020).
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