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Evolution of the 5 January 2005 CMEs associated with eruptive filaments in inner heliosphere

Published online by Cambridge University Press:  06 January 2014

Rahul Sharma ,
Nandita Srivastava ,
Bernard V. Jackson ,
D. Chakrabarty ,
Nolan Luckett ,
Hsiu-Shan Yu ,
Qiang Hu  and
Christian Möstl
Rahul Sharma
Affiliation:
3, Indra Nagar, North Sunderwas, Udaipur, India. email: sharmarahul20@googlemail.com
Nandita Srivastava
Affiliation:
Udaipur Solar Observatory, Physical Research Laboratory, Udaipur, India.
Bernard V. Jackson
Affiliation:
Center for Astrophysics and Space Sciences, University of California at San Diego, CA, USA.
D. Chakrabarty
Affiliation:
Space and Atmospheric Sciences Division, Physical Research Laboratory, Ahmedabad, India.
Nolan Luckett
Affiliation:
Center for Astrophysics and Space Sciences, University of California at San Diego, CA, USA.
Hsiu-Shan Yu
Affiliation:
Center for Astrophysics and Space Sciences, University of California at San Diego, CA, USA.
Qiang Hu
Affiliation:
Department of Physics, The University of Alabama in Huntsville, Huntsville, AL, USA. Center for Space Plasma and Aeronomic Research, The University of Alabama in Huntsville, Huntsville, AL, USA.
Christian Möstl
Affiliation:
Space Sciences Laboratory, University of California, Berkeley, CA, USA. Kanzelhöhe Observatory-IGAM, Institute of Physics, University of Graz, Graz, Austria. Space Research Institute, Austrian Academy of Sciences, A-8042 Graz, Austria.
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Abstract

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On 5 January 2005, SoHO/LASCO observed two CMEs associated with eruptive filaments with different initial velocities and acceleration. The second CME accelerates much faster than the previous and the resulting interaction has been revealed in in-situ spacecraft measurements by the presence of magnetic holes at the border of the two distinct magnetic clouds. At their interface region, these magnetic clouds have embedded filament plasma that shows complex magnetic structures with a distinct magnetic flux rope configuration; these have been modeled by the Grad - Shafranov reconstruction technique. The geomagnetic consequences of these structures have been associated with substorms in recovery phase of a storm and detailed analysis is presented in Sharma et al. (2013). In the present paper, we highlight the comparison of shape and extent of two filament plasma remnants in magnetic clouds as revealed by three - dimensional (3D) reconstruction and analysis from the Solar Mass Ejection Imager (SMEI) data. The results provide an overview of the two eruptive filaments on 5 January 2005 and their interplanetary propagation.

Keywords

Solar filamentsICMEsgeomagnetic stormssubstorms
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S300: Nature of Prominences and their role in Space Weather , June 2013 , pp. 491 - 492
Copyright
Copyright © International Astronomical Union 2013