Volume 541, May 2012
|Number of page(s)||11|
|Published online||10 May 2012|
High spatial resolution VAULT H-Lyα observations and multiwavelength analysis of an active region filament⋆
1 Institut d’Astrophysique Spatiale, UMR 8617, Université Paris 11, 91405 Orsay Cedex, France
2 Naval Research Laboratory, 4555 Overlook avenue SW, Washington, DC 20375, USA
3 Big Bear Solar Observatory of New Jersey Institute of Technology, 40386 North Shore Lane, Big Bear City, CA92314-9672, USA
Received: 14 October 2011
Accepted: 9 March 2012
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.
Key words: Sun: filaments, prominences / Sun: UV radiation / opacity
Appendix A is available in electronic form at http://www.aanda.org
© ESO, 2012
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.