Show simple item record

dc.contributor.author Morgan, Huw
dc.contributor.author Habbal, Shadia Rifai
dc.date.accessioned 2007-10-04T15:24:43Z
dc.date.available 2007-10-04T15:24:43Z
dc.date.issued 2007-03
dc.identifier.citation Morgan , H & Habbal , S R 2007 , ' An empirical 3D model of the large-scale coronal structure based on the distribution of Hα filaments on the solar disk ' Astronomy and Astrophysics , vol 464 , no. 1 , pp. 357-365 . , 10.1051/0004-6361:20066482 en
dc.identifier.issn 0004-6361
dc.identifier.other PURE: 72616
dc.identifier.other dspace: 2160/336
dc.identifier.uri http://hdl.handle.net/2160/336
dc.identifier.uri http://www.aanda.org/ en
dc.description Morgan, H.; Habbal, S. R., An empirical 3D model of the large-scale coronal structure based on the distribution of Hα filaments on the solar disk, Astronomy and Astrophysics, Volume 464, Issue 1, March II 2007, pp.357-365 en
dc.description.abstract Despite the wealth of solar data currently available, the explicit connection between coronal streamers and features on the solar disk remains unresolved. Aims: To reproduce the large-scale coronal structure starting from the solar surface, an empirical three-dimensional (3D) model is used to test the assumption that such structure, namely streamers, is a consequence of twisted high-density sheets originating from prominences (or, equivalently, filaments) at the base of the corona. Methods: A 3D model is created whereby high-density sheets are placed above filaments on the solar disk, which twist and merge with height into a final radial configuration constrained by the oberved position of streamers stalks higher up in the corona. The observational constraints are provided by white light observations from the LASCO/C2 data during the declining phase of solar activity, spanning the end of Carrington Rotation (CR) 2005 and the start of CR 2006, i.e. July-August 2003, and the position of filaments from the corresponding Hα synoptic maps of the Paris-Meudon Observatory. Results: The 3D model thus derived yields a reasonable agreement with the observed large-scale coronal structure, in particular the shape of large helmet streamers. Conclusions: .These results give confidence in the underlying assumption that large helmet streamers can be the result of the convergence of two or more sheet-like structures originating from a distribution of filaments on the solar disk. The model supports the view that streamers, during that time of the solar cycle, are often associated with multiple current sheets. en
dc.format.extent 9 en
dc.language.iso eng
dc.relation.ispartof Astronomy and Astrophysics en
dc.title An empirical 3D model of the large-scale coronal structure based on the distribution of Hα filaments on the solar disk en
dc.type Text en
dc.type.publicationtype Article (Journal) en
dc.identifier.doi http://dx.doi.org/10.1051/0004-6361:20066482
dc.contributor.institution Institute of Mathematics & Physics (ADT) en
dc.contributor.institution Mathematics and Physics en
dc.description.status Peer reviewed en


Files in this item

Aside from theses and in the absence of a specific licence document on an item page, all works in Cadair are accessible under the CC BY-NC-ND Licence. AU theses and dissertations held on Cadair are made available for the purposes of private study and non-commercial research and brief extracts may be reproduced under fair dealing for the purpose of criticism or review. If you have any queries in relation to the re-use of material on Cadair, contact is@aber.ac.uk.

This item appears in the following Collection(s)

Show simple item record

Search Cadair


Advanced Search

Browse

Statistics