AAS 200th meeting, Albuquerque, NM, June 2002
Session 65. The Magnetic Structure of CMEs
SPD Topical Session Oral, Wednesday, June 5, 2002, 2:30-4:00pm, 4:15-6:00pm, Ruidoso/Pecos

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[65.09] Evidence from Coronal Observations of Magnetic Field Structure in CMEs

N. Gopalswamy (NASA Goddard Space Flight Center)

The magnetic nature of coronal mass ejections has been inferred from the fact that they originate from closed magnetic field regions on the Sun such as active regions and filament regions. Although we have no direct measurement of the magnetic fields of CMEs, we can obtain useful information on the magnetic structure of CMEs from coronal observations at various wavelengths. The CME is a multithermal structure with temperatures ranging from a few kilokelvin to several megakelvin, so we need multi-wavelength observations to get a global picture of CMEs. A wide range of ground and space based instruments routinely observe CMEs. We present several examples of CMEs observed in X-ray, white light, EUV and radio wavelengths that help us understand the magnetic structure of CMEs.

If you would like more information about this abstract, please follow the link to http://online.itp.ucsb.edu/online/solar_c02/gopalswamy/. This link was provided by the author. When you follow it, you will leave the Web site for this meeting; to return, you should use the Back comand on your browser.

The author(s) of this abstract have provided an email address for comments about the abstract: gopals@fugee.gsfc.nasa.gov

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Bulletin of the American Astronomical Society, 34
© 2002. The American Astronomical Soceity.