Abstract
Based on photospheric vector magnetograms obtained at Huairou Solar Observing Station (HSOS), non-potential characteristics of the magnetic field beneath the filament in active region NOAA 9077 are investigated. We focus on the structure and evolution of the magnetic field from 00:08 UT to 10:25 UT of 14 July before the Bastille event. Particular attention is paid to transverse field strength, shear degree and horizontal gradient of the line-of-sight magnetic field around the filament and filament channel. The following characteristics are found. (1) The magnetic non-potentiality has an obviously non-uniform distribution. The shear degree of the transverse field (Hagyard et al., 1984) is very large, up to 75° in some sites beneath the filament, such as the initial brightening site in TRACE 1600 Å images and the breaking site of the filament. The transverse field and the horizontal gradient of the line-of-sight field are very large in some parts corresponding to the hottest and continuously brightening portions. (2) The mean strength and mean shear angle of the transverse field and mean horizontal gradient of the line-of-sight field have obviously dropped in most parts beneath the filament for two hours before the filament eruption and onset of the X5.7/3B flare. After comparing simultaneous UV and EUV images, Hβ filtergrams and Dopplergrams at solar atmosphere, we suggest that magnetic cancellation is likely to quickly transport the magnetic energy and complexity into the higher atmosphere in these two hours. This leads to magnetic instability in the filament and eventually causes the eruption of filament and onset of the flare.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
Ai, G. and Hu, Y.: 1986, Publ. Beijing Astron. Obs. 8, 1.
Deng, Y. Y., Wang, J. X., Yan, Y. H., and Zhang, J.: 2001, Solar Phys. 204, 11.
Hagyard, M. J.: 1997, in Solar-Terrestrial Prediction V, p. 527.
Hagyard, M., Smith, J., Teuber, D., and West, E.: 1984, Solar Phys. 91, 115.
Hagyard, M. J., Venkatakrishnan, P., and Smith, J. B., Jr.: 1990, Astrophys. J. Suppl. Ser. 73, 159.
Handy, B. N. et al.: 1999, Solar Phys. 187, 229.
Kosovichev, A. G. and Zharkova, V. V.: 2001, Astrophys. J. 550, L105.
Leroy, J.-L. 1989, in E. R. Priest (ed.), Dynamics and Structure of Quiescent Solar Prominences, Kluwer Academic Publishers, Dordrecht, Holland, p. 77.
Liu, Y. and Zhang, H. Q.: 2001, Astron. Astrophys. 372, 1019L.
Lü, Y., Wang, J., and Wang, H.: 1993, Solar Phys. 148, 119.
Martin, S. F. and Livi, S.: 1992, in Z. Švestka, B. V. Jackson, and M. E. Machado (eds.), Lecture Notes in Physics 399, 33.
Sakurai, T., Shibata, K., Ichimoto, K., Tsuneta, S., and Acton, L.: 1992, Publ. Astron. Soc. Japan 44, L123.
Schrijver, C. J. and Title, A. M.: 2001, Solar Phys. 200, CD-ROM
Wang, H., Ewell M., and Zirin H.: 1994, Astrophys. J. 424, 436.
Wang, J. and Li, W.: 1998, in D. Webb, D. Rust, and B. Schmieder (eds.), 'New Perspectives on Solar Prominences', IAU Colloquium 167, 98.
Wang, J. and Shi, Z.: 1993, Solar Phys. 143, 119.
Wang, J., Shi, Z., Wang, H., and Lü, Y.: 1996, Astrophys. J. 456, 861.
Zhang, J., Wang, J., Deng, Y., and Wu, D.: 2001, Astrophys. J. 548, L99.
Zirin, H. and Tanaka, K.: 1973, Solar Phys. 32, 173.
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Tian, L., Wang, J. & Wu, D. Non-Potentiality of the Magnetic Field Beneath the Eruptive Filament in the Bastille Event. Solar Physics 209, 375–389 (2002). https://doi.org/10.1023/A:1021201817701
Published:
Issue Date:
DOI: https://doi.org/10.1023/A:1021201817701