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FILAMENT CHANNEL STRUCTURES IN A Si IV LINE RELATED TO A 3D MAGNETIC MODEL
 

Summary: FILAMENT CHANNEL STRUCTURES IN A Si IV LINE RELATED TO A
3D MAGNETIC MODEL
T. A. KUCERA1,, G. AULANIER2, B. SCHMIEDER2,, N. MEIN2 and J.-C. VIAL3
1Code 682.3, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, U.S.A.
2Observatoire de Paris, section Meudon, DASOP, URA 2080 (CNRS), F-92195 Meudon Principal
Cedex, France
3Intstitut d'Astrophysique Spatiale, Unité mixte CNRS-Université Paris XI, Bâtiment 121,
F-91405 Orsay Cedex, France
(Received 30 October 1998; accepted 29 December 1998)
Abstract. A recent 3D magnetic model of filament support (Aulanier and Démoulin, 1998) has
shown that specific morphologies derived from the model, based on SOHO/MDI magnetograms,
match quite well with the observations of a filament observed in H and Ca II lines with the German
telescope VTT in Tenerife on 25 September 1996 (Aulanier et al., 1998, 1999a). Some predictions
of this model concern the filament channel. To continue the comparison of model and data, we have
investigated the same filament region observed in ultraviolet by the SOHO spectrometers SUMER
and CDS. The elongated EUV fine structures in the filament channel observed in the Si IV 1393.76 Å
line by SUMER have similar orientations and locations to features predicted by the model of Aulanier
et al. (1999a). These regions are near the bases of field lines which tangentially join to the pho-
tosphere in so called `bald patches' and are parts of large arcades above the filament channel. In
addition, we consider the Si IV Doppler shifts in these structures and compare them to what might

  

Source: Aulanier, Guillaume - Observatoire de Paris

 

Collections: Physics