Hostname: page-component-77c89778f8-gq7q9 Total loading time: 0 Render date: 2024-07-22T08:22:35.511Z Has data issue: false hasContentIssue false
  • English
  • Français

Vector Magnetic Fields at the Base of Filaments and the Filament Environment

Published online by Cambridge University Press:  12 April 2016

Jingxiu Wang  and
Wei Li
Jingxiu Wang
Affiliation:
Beijing Astronomical Observatory, Chinese Academy of Sciences, Beijing 100080, China
Wei Li
Affiliation:
Beijing Astronomical Observatory, Chinese Academy of Sciences, Beijing 100080, China

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.

Based on an analysis of three active filaments in AR 6891, we find that vector magnetic fields at the base of filaments and the filament environment is characterized by the following: (1) The transverse field is parallel along the magnetic neutral line for most of the filaments. The average transverse field beneath the filaments is more than 400 G. (2) The horizontal gradient of the line-of-sight field crossing the neutral line is, more or less, constant along the major fraction of a filament, but very steep at the two ends. The average gradient is 0.06 G/km. (3) For each of the filaments there is a squeezing magnetic structure which represents an intrusion of a satellite bipole into the main flux system. The neutral line for a squeezing magnetic structure has a large curvature, a strong sheared transverse field of more than 1 KG, and a steep field gradient of approximate 0.3 G/km. (4) The transverse field and field gradient are clearly enhanced before the filament eruption.

Type
Filaments and Their Environment
Information
International Astronomical Union Colloquium , Volume 167: New Perspectives on Solar Prominences , 1998 , pp. 98 - 101
Copyright
Copyright © Astronomical Society of the Pacific 1998

References

Leroy, J-L. 1989, in Dynamics and Structure of Quiescent Solar Prominences, Priest, E.R. (ed.), Kluwer Acad. Publ., Dordrecht, Holland, p. 77 Google Scholar
Tang, F. 1987, Sol. Phys., 107, 233 CrossRefGoogle Scholar
Tandberg-Hanssen, E. 1974, Solar Prominences, D. Reidel, Dordrecht, Holland Google Scholar
Wang, J., Shi, Z., Wang, H. and Lü, Y. 1996, ApJ, 456, 861 CrossRefGoogle Scholar