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Formation and evolution of an active region filament

Published online by Cambridge University Press:  06 January 2014

Christoph Kuckein ,
Rebeca Centeno  and
Valentín Martínez Pillet
Christoph Kuckein
Affiliation:
Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482, Potsdam, Germany. email: ckuckein@aip.de Instituto de Astrofísica de Canarias (IAC), Vía Láctea s/n, 38205, La Laguna, Tenerife, Spain
Rebeca Centeno
Affiliation:
High Altitude Observatory (NCAR), Boulder, CO 80301, USA
Valentín Martínez Pillet
Affiliation:
National Solar Observatory (NSO), Sunspot, NM 88349, USA
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Abstract

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Several scenarios explaining how filaments are formed can be found in literature. In this paper, we analyzed the observations of an active region filament and critically evaluated the observed properties in the context of current filament formation models. This study is based on multi-height spectropolarimetric observations. The inferred vector magnetic field has been extrapolated starting either from the photosphere or from the chromosphere. The line-of-sight motions of the filament, which was located near disk center, have been analyzed inferring the Doppler velocities. We conclude that a part of the magnetic structure emerged from below the photosphere.

Keywords

Sun: filamentsprominencesSun: photosphereSun: chromosphereSun: magnetic fieldstechniques: polarimetric
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. 40 - 43
Copyright
Copyright © International Astronomical Union 2013 

References

Antiochos, S. K., Dahlburg, R. B., & Klimchuk, J. A. 1994, ApJ 420, L41CrossRefGoogle Scholar
Collados, M., Lagg, A., Díaz García, J. J., et al. 2007, ASP-CS 368, 611Google Scholar
Denker, C., Johannesson, A., Marquette, W., et al. 1999, Solar Phys. 184, 87Google Scholar
Guo, Y., Schmieder, B., Démoulin, P., et al. 2010, ApJ 714, 343Google Scholar
Kuckein, C. 2012, PhD Thesis, Universidad de La Laguna (Tenerife, Spain)Google Scholar
Kuckein, C., Martínez Pillet, V., & Centeno, R. 2012b, A&A 542, A112Google Scholar
Kuckein, C., Martínez Pillet, V., & Centeno, R. 2012a, A&A 539, A131Google Scholar
Kuckein, C., Centeno, R., Martínez Pillet, V., et al. 2009, A&A 501, 1113Google Scholar
Lites, B. W., Low, B. C., Martinez Pillet, V., et al. 1995, ApJ 446, 877CrossRefGoogle Scholar
Okamoto, T. J., Tsuneta, S., Lites, B. W., et al. 2008, ApJ 673, L215Google Scholar
Ruiz Cobo, B. & del Toro Iniesta, J. C. 1992, ApJ 398, 375Google Scholar
Scherrer, P. H., Bogart, R. S., Bush, R. I., et al. 1995, Solar Phys. 162, 129Google Scholar
Socas-Navarro, H. 2001, ASP-CS 236, 487Google Scholar
van Ballegooijen, A. A. & Martens, P. C. H. 1989, ApJ 343, 971Google Scholar
Xu, Z., Lagg, A., Solanki, S., & Liu, Y. 2012, ApJ 749, 138Google Scholar
Yelles Chaouche, L., Kuckein, C., Martínez Pillet, V., & Moreno-Insertis, F. 2012, ApJ 748, 23Google Scholar