Solar Physics

, Volume 289, Issue 11, pp 4173–4208 | Cite as

An Ensemble Study of a January 2010 Coronal Mass Ejection (CME): Connecting a Non-obvious Solar Source with Its ICME/Magnetic Cloud

  • D. F. Webb
  • M. M. Bisi
  • C. A. de Koning
  • C. J. Farrugia
  • B. V. Jackson
  • L. K. Jian
  • N. Lugaz
  • K. Marubashi
  • C. Möstl
  • E. P. Romashets
  • B. E. Wood
  • H.-S. Yu
Article

Abstract

A distinct magnetic cloud (MC) was observed in-situ at the Solar TErrestrial RElations Observatory (STEREO)-B on 20 – 21 January 2010. About three days earlier, on 17 January, a bright flare and coronal mass ejection (CME) were clearly observed by STEREO-B, which suggests that this was the progenitor of the MC. However, the in-situ speed of the event, several earlier weaker events, heliospheric imaging, and a longitude mismatch with the STEREO-B spacecraft made this interpretation unlikely. We searched for other possible solar eruptions that could have caused the MC and found a faint filament eruption and the associated CME on 14 – 15 January as the likely solar source event. We were able to confirm this source by using coronal imaging from the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI)/EUVI and COR and Solar and Heliospheric Observatory (SOHO)/Large Angle and Spectrometric Coronograph (LASCO) telescopes and heliospheric imaging from the Solar Mass Ejection Imager (SMEI) and the STEREO/Heliospheric Imager instruments. We use several empirical models to understand the three-dimensional geometry and propagation of the CME, analyze the in-situ characteristics of the associated ICME, and investigate the characteristics of the MC by comparing four independent flux-rope model fits with the launch observations and magnetic-field orientations. The geometry and orientations of the CME from the heliospheric-density reconstructions and the in-situ modeling are remarkably consistent. Lastly, this event demonstrates that a careful analysis of all aspects of the development and evolution of a CME is necessary to correctly identify the solar counterpart of an ICME/MC.

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Copyright information

© Springer Science+Business Media Dordrecht 2014

Authors and Affiliations

  • D. F. Webb
    • 1
  • M. M. Bisi
    • 2
  • C. A. de Koning
    • 3
  • C. J. Farrugia
    • 4
  • B. V. Jackson
    • 5
  • L. K. Jian
    • 6
    • 7
  • N. Lugaz
    • 4
  • K. Marubashi
    • 8
    • 9
  • C. Möstl
    • 11
    • 10
  • E. P. Romashets
    • 12
  • B. E. Wood
    • 13
  • H.-S. Yu
    • 5
  1. 1.ISRBoston CollegeChestnut HillUSA
  2. 2.RAL Space Science & Technology Facilities CouncilRutherford Appleton LaboratoryHarwell OxfordUK
  3. 3.NOAA Space Weather Prediction Center and University of ColoradoCIRESBoulderUSA
  4. 4.Space Science Center & Department of PhysicsUniversity of New HampshireDurhamUSA
  5. 5.Center for Astrophysics and Space ScienceUniversity of California, San DiegoLa JollaUSA
  6. 6.Heliophysics Science Division, Code 672NASA Goddard Space Flight CenterGreenbeltUSA
  7. 7.Department of AstronomyUniversity of MarylandCollege ParkUSA
  8. 8.Korea Astronomy and Space Science InstituteDaejeonKorea
  9. 9.SayamaJapan
  10. 10.Institute of PhysicsUniversity of GrazGrazAustria
  11. 11.Space Research InstituteAustrian Academy of SciencesGrazAustria
  12. 12.Lone Star CollegeHoustonUSA
  13. 13.Space Science DivisionNaval Research LaboratoryWashingtonUSA

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