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Solar Physics

, 294:139 | Cite as

Development of a Fast CME and Properties of a Related Interplanetary Transient

  • V. V. GrechnevEmail author
  • A. A. Kochanov
  • A. M. Uralov
  • V. A. Slemzin
  • D. G. Rodkin
  • F. F. Goryaev
  • V. I. Kiselev
  • I. I. Myshyakov
Article

Abstract

We study the development of a coronal mass ejection (CME) caused by a prominence eruption on 24 February 2011 and properties of a related interplanetary CME (ICME). The prominence destabilized, accelerated, and produced an M3.5 flare, a fast CME, and a shock wave. The eruption at the east limb was observed in quadrature by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO) and by the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) instrument suite on board the Solar-Terrestrial Relations Observatory (STEREO). The ICME produced by the SOL2011-02-24 event was measured in situ on STEREO-B two days later. The diagnostics made from multi-wavelength SDO/AIA images reveals a pre-eruptive heating of the prominence to about 7 MK and its subsequent heating during the eruption by flare-accelerated particles to about 10 MK. The hot plasma was detected in the related ICME as an enhancement in the ionic charge state of Fe, whose evolution was reproduced in the modeling. The analysis of the solar source region allows for predicting the variations of magnetic components in the ICME, while the flux-rope rotation by about \(40^{\circ }\) was indicated by observations. The magnetic-cloud propagation appears to be ballistic.

Keywords

Coronal mass ejections Heating, in flares Magnetic fields, interplanetary Prominences, active Solar wind, disturbances X-ray bursts 

Notes

Acknowledgements

We thank D.V. Prosovetsky, Yu.S. Shugay, B.V. Somov, and A.V. Kiselev for their assistance and discussions. We are indebted to the co-authors of the Grechnev et al. (2015) article that provided the basis for the present work. We thank the anonymous reviewer for valuable remarks.

V. Slemzin and D. Rodkin (Sections 2, 3.3, and 4.2) were funded by the Russian Science Foundation (RSF) under grant 17-12-01567. V. Grechnev, A. Kochanov, A. Uralov, V. Kiselev, and I. Myshyakov (Sections 3.1, 3.2, 3.4 – 3.6, 4.1, 4.3, and the Appendix) were funded by the RSF under grant 18-12-00172.

We thank the NASA/SDO and the AIA and HMI science teams; the NASA’s STEREO/SECCHI science and instrument teams; the teams operating RHESSI, SOHO/LASCO, S/WAVES, and the GOES satellites for the data used here. SOHO is a project of international cooperation between ESA and NASA. We are grateful to the team maintaining the CME Catalog at the CDAW Data Center by NASA and the Catholic University of America in cooperation with the Naval Research Laboratory. We thank the team that created and maintains the online archive of the WSA – ENLIL + Cone Model and the team that created the online Drag-Based Model.

Disclosure of Potential Conflicts of Interest

The authors declare that they have no conflicts of interest.

Supplementary material

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Copyright information

© Springer Nature B.V. 2019

Authors and Affiliations

  1. 1.Institute of Solar-Terrestrial Physics SB RASIrkutskRussia
  2. 2.P. N. Lebedev Physical Institute RASMoscowRussia

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