Hostname: page-component-586b7cd67f-2plfb Total loading time: 0 Render date: 2024-11-24T13:38:35.901Z Has data issue: false hasContentIssue false
  • English
  • Français

Effect of Coronal Mass Ejection Interactions on the SOHO/CELIAS/MTOF Measurements

Published online by Cambridge University Press:  03 June 2005

X. Wang ,
P. Wurz ,
P. Bochsler ,
F. Ipavich ,
J. Paquette  and
R.F. Wimmer-Schweingruber
X. Wang
Affiliation:
Physics Institute, University of Bern, 3012 Bern, Switzerland email: [email protected]
P. Wurz
Affiliation:
Physics Institute, University of Bern, 3012 Bern, Switzerland email: [email protected]
P. Bochsler
Affiliation:
Physics Institute, University of Bern, 3012 Bern, Switzerland email: [email protected]
F. Ipavich
Affiliation:
University of Maryland, College Park, MD20742, USA email: [email protected]
J. Paquette
Affiliation:
University of Maryland, College Park, MD20742, USA email: [email protected]
R.F. Wimmer-Schweingruber
Affiliation:
Extraterrestrische Physik, University of Kiel, 24098 Kiel, Germany email: [email protected]
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.

By using the plasma composition data from SOHO/CELIAS/MTOF, charge states data from ACE/SWICS, combining with the remote sensing observations from SOHO/LASCO white-light image and WIND/WAVES radio emission, we describe a coronal mass ejection (CME) observed on 2001 October 19 16:50 UT to show how the effect of CME interaction appears in the in situ measurements. A new narrow shock is formed while the rear CME passing through the core region of the preceding one, which moves faster than the surrounding part and has a new type II radio burst associated with it. Because of its distinguished elemental abundance and unusual low charge states, we connect a density hump observed by MTOF/PM with the preceding CME core. By comparing the relative abundances of minor ions in shock compressive region, ICME region and CME core region with respect to that in upstream slow solar wind, we indicate mass-per-charge dependence of minor thermal ions may be an important imprint of the characteristic velocity of distant acceleration region.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Keywords

shock wavesSun: abundancescoronal mass ejections (CMEs) solar windradio radiation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS226 , September 2004 , pp. 409 - 413
Copyright
© 2005 International Astronomical Union