Hostname: page-component-77c89778f8-n9wrp Total loading time: 0 Render date: 2024-07-20T20:38:37.505Z Has data issue: false hasContentIssue false
  • English
  • Français

Featuring dark coronal structures: physical signatures of filaments and coronal holes for automated recognition

Published online by Cambridge University Press:  06 January 2014

Judith Palacios ,
Consuelo Cid ,
Elena Saiz ,
Yolanda Cerrato  and
Antonio Guerrero
Judith Palacios
Affiliation:
Space Reseach Group–Space Weather, Physics Dpt., University of Alcalá University Campus, Sciences Building, P.O. 28871, Alcalá de Henares, Spain email: judith.palacios@uah.es
Consuelo Cid
Affiliation:
Space Reseach Group–Space Weather, Physics Dpt., University of Alcalá University Campus, Sciences Building, P.O. 28871, Alcalá de Henares, Spain email: judith.palacios@uah.es
Elena Saiz
Affiliation:
Space Reseach Group–Space Weather, Physics Dpt., University of Alcalá University Campus, Sciences Building, P.O. 28871, Alcalá de Henares, Spain email: judith.palacios@uah.es
Yolanda Cerrato
Affiliation:
Space Reseach Group–Space Weather, Physics Dpt., University of Alcalá University Campus, Sciences Building, P.O. 28871, Alcalá de Henares, Spain email: judith.palacios@uah.es
Antonio Guerrero
Affiliation:
Space Reseach Group–Space Weather, Physics Dpt., University of Alcalá University Campus, Sciences Building, P.O. 28871, Alcalá de Henares, Spain email: judith.palacios@uah.es
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Filaments may be mistaken for coronal holes when observed in extreme ultraviolet (EUV) images; however, a closer and more careful look reveals that their photometric properties are different. The combination of EUV images with photospheric magnetograms shows some characteristic differences between filaments and coronal holes. We have performed analyses with 7 different SDO/AIA wavelengths (94, 131, 171, 211, 193, 304, 335 Å) and SDO/HMI magnetograms obtained in September 2011 and March 2012 to study coronal holes and filaments from the photometric, magnetic, and also geometric point of view, since projection effects play an important role on the aforementioned traits.

Keywords

Sun: solar filamentsSun: coronal holes
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S300: Nature of Prominences and their role in Space Weather , June 2013 , pp. 517 - 518
Copyright
Copyright © International Astronomical Union 2013 

References

Krista, L. & Gallagher, P., 2009, SolPhys, 256, 87Google Scholar
Krista, L. D., Gallagher, P. T., & Bloomfield, D. S., 2011, ApJ, 731, 26CrossRefGoogle Scholar
O'Dwyer, B., Del Zanna, G., Mason, H. E., Weber, M. A., & Tripathi, D., 2010, A&A, 521, A21Google Scholar
Pesnell, W. D., Thompson, B. J., & Chamberlin, P. C., 2012, SolPhys, 275, 3Google Scholar