1 / 15

Solar Erupting Filaments and Magnetic Field Configurations of IP Magnetic Clouds

Solar Erupting Filaments and Magnetic Field Configurations of IP Magnetic Clouds. Yuming Wang 1, 2 & Jie Zhang 1 (Presenting) 1 George Mason University 2 University of Science & Technology of China. Paper by Wang, et al., ApJ, 651, 2006. GMU 10-2006.

carina
Télécharger la présentation

Solar Erupting Filaments and Magnetic Field Configurations of IP Magnetic Clouds

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Solar Erupting Filaments and Magnetic Field Configurations of IP Magnetic Clouds Yuming Wang1, 2 & Jie Zhang1 (Presenting) 1George Mason University 2University of Science & Technology of China Paper by Wang, et al., ApJ, 651, 2006 GMU 10-2006

  2. It is generally believed that the axial orientation of MCs is parallel to the long axis of filaments. [e.g., Bothmer and Schwenn 1994; Bothmer and Rust 1997; Marubashi 1997; McAllister et al. 2001; Yurchyshyn et al. 2001; Jing et al. 2004; Rust et al. 2005.] N Flux rope Sun + ¯ E W S

  3. Here, we further take the curvature of filament axis into account, when compared with MC axis • Three filament-MC events are analyzed. The selection of filaments satisfies the following criteria: • The filament and its orientation is well observed in Halphaimages , i.e., large and dark enough • There is no complex filament system in the source region.

  4. August 9, 2000 event

  5. ~2.5 days later

  6. October 9, 2000 event

  7. ~3.5 days later

  8. November 18, 2003 event

  9. ~2 days later

  10. 70~90° Leading front Consistent with the central part of the filament Inconsistent 47°

  11. Why is the axis of MCs not consistent with that of filaments for some events? • A CME is a large scale phenomenon, in which filament itself (seen in Halpha) is only a small part of the eruptive magnetic structure [e.g., Harrison & Lyons 2000; Plunkett et al. 2001]. • A MC is also a large scale structure. The in-situ observation only see a line through the 3-D MC. • A CME may rotate when it moves outward [e.g., Fan & Gibson 2004; Torok & Kliem 2005]. • Error in fitting the observations of magnetic clouds • When the filament is curved, what portion correspond to the axis of MC?

More Related