Solar Physics

, 294:73 | Cite as

Observations of a Flare-Generated Blast Wave in a Pseudo Coronal Mass Ejection Event

  • V. G. Eselevich
  • M. V. Eselevich
  • I. V. ZimovetsEmail author


We present an analysis of the event near the east limb, SOL2014-03-06T09:23, in which a pseudo coronal mass ejection (CME) was detected by the Large Angle and Spectrometric Coronagraph (LASCO) C2 instrument and indicated as “Poor Event; Only C2” in the Solar and Heliospheric Observatory (SOHO) LASCO CME Catalog. The analysis was performed based on two main methods: 1) investigation of the difference brightness profiles along specific directions in the solar corona using the EUV observations by the Atmospheric Imaging Assembly (AIA) instrument onboard the Solar Dynamics Observatory (SDO); 2) investigation of the spatially-resolved observations of the type II radio bursts made with the Nançay Radioheliograph. Based on the analysis performed we argue that the observed pseudo-CME could be a blast wave caused by impulsive flare energy release in the low corona. We also argue that, in the limited height range of \({\approx}\,0.2 \mathrm{R_{\odot }}\,\mbox{--}\,0.5 \mathrm{R}_{\odot}\), the front of this blast wave could steepen into a shock front.


Flares, waves Radio bursts, type II Waves, shock 



The authors thank the SDO/AIA, RSTN at Learmonth, ORFEES, NRH, RHESSI, PROBA2/LYRA, GOES, SOHO/LASCO, and SOHO LASCO CME Catalog teams, whose data were used in this study. We thank the radio monitoring service at LESIA (Observatoire de Paris; ) to provide value-added data that have been used for this study. The CME catalog is generated and maintained at the CDAW Data Center by NASA and The Catholic University of America in cooperation with the Naval Research Laboratory. SOHO is a project of international cooperation between ESA and NASA. We are grateful to the anonymous reviewer for the useful and constructive comments which helped to improve the quality of the manuscript. We are also grateful to Dr. C.R. Goddard (University of Warwick, UK) for help with correcting the language. The work was supported by Theme 16.2 PLASMA “Conducting basic research in the field of space plasma physics, solar-terrestrial connections and magnetosphere physics”, State registration number 0120.0 602992 (No 0028-2014-0002) of the Ministry of Science and Higher Education of the Russian Federation.

Disclosure of Potential Conflicts of Interest

The authors declare that they have no conflicts of interest.


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Copyright information

© Springer Nature B.V. 2019

Authors and Affiliations

  1. 1.Institute of Solar-Terrestrial Physics of Siberian Branch of Russian Academy of SciencesIrkutskRussia
  2. 2.Space Research Institute (IKI) of Russian Academy of SciencesMoscowRussia
  3. 3.State Key Laboratory of Space WeatherNational Space Science Center (NSSC) of Chinese Academy of SciencesBeijingChina
  4. 4.International Space Science Institute – Beijing (ISSI-BJ)BeijingChina

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