Hostname: page-component-8448b6f56d-c4f8m Total loading time: 0 Render date: 2024-04-19T08:06:29.848Z Has data issue: false hasContentIssue false
  • English
  • Français

Magnetic Reconnection Inflow near the CME/Flare Current Sheet

Published online by Cambridge University Press:  03 June 2005

J. Lin ,
Y.-K. Ko ,
L. Sui ,
J. C. Raymond ,
G. A. Stenborg ,
Y. Jiang ,
S. Zhao  and
S. Mancuso
J. Lin
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA, email: jlin@cfa.harvard.edu
Y.-K. Ko
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA, email: jlin@cfa.harvard.edu
L. Sui
Affiliation:
Department of Physics, Catholic University of America, 620 Michigan Avenue, Washington, DC 20064, USA
J. C. Raymond
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA, email: jlin@cfa.harvard.edu
G. A. Stenborg
Affiliation:
Department of Physics, Catholic University of America, 620 Michigan Avenue, Washington, DC 20064, USA
Y. Jiang
Affiliation:
National Astronomical Observatories of China/Yunnan Observatory, Chinese Academy of Sciences, P. O. Box 110, Kunming, Yunnan 650011, China
S. Zhao
Affiliation:
National Astronomical Observatories of China/Yunnan Observatory, Chinese Academy of Sciences, P. O. Box 110, Kunming, Yunnan 650011, China
S. Mancuso
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA, email: jlin@cfa.harvard.edu INAF/Osservatorio Astronomico di Torino, 20 Strada Osservatorio, 1-10025 Pino Torinese, Italy
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.

This work reports direct observations of the magnetic reconnection site during an eruptive process occurring on November 18, 2003. The event started with a rapid expansion of a few magnetic arcades located over the east limb of the Sun and developed an energetic partial halo coronal mass ejection (CME), a long current sheet and a group of bright flare loops in the wake of the CME. It was observed by several instruments both in space and on ground, including the EUV Imaging Telescope, the Ultraviolet Coronagraph Spectrometer, and the Large Angle and Spectrometric Coronagraph experiment on board the Solar and Heliospheric Observatory, the Reuven Ramaty High Energy Solar Spectroscopic Imager, as well as the Mauna Loa Solar Observatory Mark IV K-coronameter. We combine the data from these instruments to investigate various properties of the eruptive process, including those around the current sheet. The composite of images from different instruments and the corresponding results specify explicitly how the different objects developed by a single eruptive process are related to one another.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Keywords

Sun: coronal mass ejectionsflaresMHD
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS226 , September 2004 , pp. 311 - 313
Copyright
© 2005 International Astronomical Union