TY - JOUR
T1 - High spatial resolution VAULT H-Ly α observations and multiwavelength analysis of an active region filament
AU - Vial, J. C.
AU - Olivier, K.
AU - Philippon, A. A.
AU - Vourlidas, A.
AU - Yurchyshyn, Vasyl
N1 - Funding Information:
Jean-Claude Vial acknowledges the ISSI support in the frame of the “Spectroscopy and Imaging of Quiescent and Eruptive Prominences from Space” working team, headed by N. Labrosse, and is grateful to V. Abramenko, who helped us with special BBSO files, to L. Golub, for the TRACE image, and to P. Schwartz, who provided the filament model. The authors thank the anonymous referee, who helped them to improve the paper. The work of A. Vourlidas was supported by various NASA grants to the Naval Research Laboratory.
PY - 2012
Y1 - 2012
N2 - Context. The search for the fine structure of prominences has received considerable new attention thanks to the Swedish Solar Telescope (SST) Hα pictures that provide an unsurpassed spatial resolution. Recently, it has been shown that the filaments' coronal environment, at least for quiescent filaments, is perturbed by either cool absorbing material (in the EUV) or an "emissivity blocking" (actually a lack of transition region and coronal material). Aims. The aim is to assess the fine structure in an active region filament and to determine the nature of the EUV absorption or lack of emission phenomena, using the very optically thick line H-Lyα, formed at a temperature higher than Hα. Methods. We performed a multiwavelength study where high-resolution imaging in the H-Lyα line (VAULT) was analysed and compared with observations of an active region filament in Hα (BBSO) and EUV lines (EIT and TRACE). Results. As for the SST data, small-scale structures were detected at a typical scale of about one to two arcseconds with, for some cuts, an indication of fine scales down to 0.4 arcsec in the optically thick H-Lyα line. The filament intensity relative to the intensity of the (active) region it is embedded in is about 0.2 in H-Lyα. This ratio (Lymanα ratio intensity or "LRI") is the lowest value compared to other lines, e.g. Hα. The filament environment was also investigated and evidence of an UV extension was found. The comparison of spatial cuts in different lines across the filament shows evidence of strong absorption, and consequently of cool plasma on one side of the filament, but not on the other (that side is obscured by the filament itself). Conclusions. The absence of very fine structure in H-Lyα compared to Hα is explained by the formation temperature of the H-Lyα line (∼20 000 K), where the transition regions of the thin threads begin to merge. From the detection of H-Lyα absorption on the observable side of the filament side, we derive the presence of absorbing (cool) material and possibly also of emissivity blocking (or coronal void). This poses the question whether these absorption effects are typical of active region filaments.
AB - Context. The search for the fine structure of prominences has received considerable new attention thanks to the Swedish Solar Telescope (SST) Hα pictures that provide an unsurpassed spatial resolution. Recently, it has been shown that the filaments' coronal environment, at least for quiescent filaments, is perturbed by either cool absorbing material (in the EUV) or an "emissivity blocking" (actually a lack of transition region and coronal material). Aims. The aim is to assess the fine structure in an active region filament and to determine the nature of the EUV absorption or lack of emission phenomena, using the very optically thick line H-Lyα, formed at a temperature higher than Hα. Methods. We performed a multiwavelength study where high-resolution imaging in the H-Lyα line (VAULT) was analysed and compared with observations of an active region filament in Hα (BBSO) and EUV lines (EIT and TRACE). Results. As for the SST data, small-scale structures were detected at a typical scale of about one to two arcseconds with, for some cuts, an indication of fine scales down to 0.4 arcsec in the optically thick H-Lyα line. The filament intensity relative to the intensity of the (active) region it is embedded in is about 0.2 in H-Lyα. This ratio (Lymanα ratio intensity or "LRI") is the lowest value compared to other lines, e.g. Hα. The filament environment was also investigated and evidence of an UV extension was found. The comparison of spatial cuts in different lines across the filament shows evidence of strong absorption, and consequently of cool plasma on one side of the filament, but not on the other (that side is obscured by the filament itself). Conclusions. The absence of very fine structure in H-Lyα compared to Hα is explained by the formation temperature of the H-Lyα line (∼20 000 K), where the transition regions of the thin threads begin to merge. From the detection of H-Lyα absorption on the observable side of the filament side, we derive the presence of absorbing (cool) material and possibly also of emissivity blocking (or coronal void). This poses the question whether these absorption effects are typical of active region filaments.
KW - Opacity
KW - Sun: UV radiation
KW - Sun: filaments, prominences
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U2 - 10.1051/0004-6361/201118275
DO - 10.1051/0004-6361/201118275
M3 - Article
AN - SCOPUS:84860719115
SN - 0004-6361
VL - 541
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A108
ER -