Hostname: page-component-586b7cd67f-t7fkt Total loading time: 0 Render date: 2024-11-24T10:58:36.121Z Has data issue: false hasContentIssue false
  • English
  • Français

A filament supported by different magnetic field configurations

Published online by Cambridge University Press:  26 August 2011

Y. Guo ,
B. Schmieder ,
P. Démoulin ,
T. Wiegelmann ,
G. Aulanier ,
T. Török  and
V. Bommier
Y. Guo
Affiliation:
Department of Astronomy, Nanjing University, Nanjing 210093, China email: [email protected] LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France
B. Schmieder
Affiliation:
LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France
P. Démoulin
Affiliation:
LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France
T. Wiegelmann
Affiliation:
Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Strasse 2, 37191 Katlenburg-Lindau, Germany
G. Aulanier
Affiliation:
LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France
T. Török
Affiliation:
LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France
V. Bommier
Affiliation:
LERMA, Observatoire de Paris, CNRS, UPMC, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France
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.

A nonlinear force-free magnetic field extrapolation of vector magnetogram data obtained by THEMIS/MTR on 2005 May 27 suggests the simultaneous existence of different magnetic configurations within one active region filament: one part of the filament is supported by field line dips within a flux rope, while the other part is located in dips within an arcade structure. Although the axial field chirality (dextral) and the magnetic helicity (negative) are the same along the whole filament, the chiralities of the filament barbs at different sections are opposite, i.e., right-bearing in the flux rope part and left-bearing in the arcade part. This argues against past suggestions that different barb chiralities imply different signs of helicity of the underlying magnetic field. This new finding about the chirality of filaments will be useful to associate eruptive filaments and magnetic cloud using the helicity parameter in the Space Weather Science.

Keywords

Sun: coronaSun: filamentsSun: magnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S273: The Physics of Sun and Star Spots , August 2010 , pp. 328 - 332
Copyright
Copyright © International Astronomical Union 2011

References

Antiochos, S. K., Dahlburg, R. B., & Klimchuk, J. A. 1994, Astrophys. J. Lett., 420, L41CrossRefGoogle Scholar
Aulanier, G. & Démoulin, P. 1998, Astron. Astrophys, 329, 1125Google Scholar
Bommier, V., Landi Degl'Innocenti, E., Landolfi, M., & Molodij, G. 2007, Astron. Astrophys, 464, 323CrossRefGoogle Scholar
Georgoulis, M. K. 2005, Astrophys. J. Lett., 629, L69CrossRefGoogle Scholar
Guo, Y., Schmieder, B., Démoulin, P., Wiegelmann, T., Aulanier, G., Tórók, T., & Bommier, V. 2010, Astrophys. J., 714, 343CrossRefGoogle Scholar
Kippenhahn, R. & Schlüter, A. 1957, Zeitschrift fur Astrophysik, 43, 36Google Scholar
Kuckein, C., Centeno, R., Martínez Pillet, V., Casini, R., Manso Sainz, R., & Shimizu, T. 2009, Astron. Astrophys, 501, 1113CrossRefGoogle Scholar
Kuperus, M. & Raadu, M. A. 1974, Astron. Astrophys, 31, 189Google Scholar
Landolfi, M. & Landi Degl'Innocenti, E. 1982, Solar Phys., 78, 355CrossRefGoogle Scholar
Low, B. C. & Lou, Y. Q. 1990, Astrophys. J., 352, 343CrossRefGoogle Scholar
Régnier, S., Amari, T., & Kersalé, E. 2002, Astron. Astrophys, 392, 1119CrossRefGoogle Scholar
Schrijver, C. J., De Rosa, M. L., Title, A. M., & Metcalf, T. R. 2005, Astrophys. J., 628, 501CrossRefGoogle Scholar
Wheatland, M. S., Sturrock, P. A., & Roumeliotis, G. 2000, Astrophys. J., 540, 1150CrossRefGoogle Scholar
Wiegelmann, T. 2004, Solar Phys., 219, 87CrossRefGoogle Scholar