Properties of the HPS‐ICME‐CIR Interaction Event of 9–10 September 2011

Duraid A Mohammed Al-Shakarchi, Huw Morgan

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During September 09‐10, 2011 the ACE, Wind and SOHO spacecraft measured the complex interaction between an interplanetary coronal mass ejection (ICME) and a co‐rotating interaction region (CIR) associated with the heliospheric sector boundary. Except for a few short periods, the suprathermal electrons are unidirectional, suggesting the ICME magnetic field has opened through interchange reconnection. Signatures of interaction are distributed throughout the event suggesting that the structures have become entangled, or embedded. Since the ICME speed is relatively low, the strong forward shock must be caused by the ICME‐CIR interaction. Other interesting features are the upstream heating flux discontinuity, the very high proton density in the frontal boundary of the heliospheric plasma sheet and the forward shock, the significant speed elevation within the sheath, the distortion of Bz in the magnetic cloud, the indistinct location of the stream interface, the unidirectional domination of the suprathermal electrons and the reverse shock at the CIR rear boundary. There is an unusual delay between the proton density and temperature profiles. Furthermore, large differences in proton speed and forward shock density measured between L1 spacecraft indicates high variation at small spatial scales. A few days earlier, STEREO B recorded the undisturbed CIR, which shows that (i) some general features of the CIR are preserved (ii) the CIR is compressed by a factor of ∼4 by the ICME and (iii) a magnetic exhausted region at the front of the CIR is a continuous feature and is not formed due to the ICME interaction
Original languageEnglish
Pages (from-to)2535-2556
Number of pages22
JournalJournal of Geophysical Research: Space Physics
Issue number4
Early online date26 Apr 2018
Publication statusPublished - 16 May 2018


  • interplanetary coronal mass ejection ICME
  • corotating interaction region CIR
  • ICME-CIR interaction
  • solar wind plasma
  • interchange reconnection
  • heliospheric plasma sheet


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