Solar Physics

, Volume 225, Issue 1, pp 141–155 | Cite as

Re-Evaluation of the Flare–Type II–CME Association

  • A. Shanmugaraju
  • Y.-J. Moon
  • Y.-H. Kim
  • M. Dryer
  • S. Umapathy
Article
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Accepted:

Abstract

We have re-evaluated the association of type II solar radio bursts with flares and/or coronal mass ejections (CMEs) using the year 2000 solar maximum data. For this, we consider 52 type II events whose associations with flares or CMEs were absent or not clearly identified and reported. These events are classified as follows; group I: 11 type IIs for which there are no reports of GOES X-ray flares and CMEs; group II: 12 type IIs for which there are no reports of GOES X-ray flares; and group III: 29 type IIs for which the flare locations are not reported. By carefully re-examining their association from GOES X-ray and Hα, Yohkoh SXT and EIT-EUV data, we attempt to answer the following questions: (i) if there really were no X-ray flares associated with the above 23 type IIs of groups I and II; (ii) whether they can be regarded as backside events whose X-ray emission might have been occulted. From this analysis, we have found that two factors, flare background intensity and flare location, play important roles in the complete reports about flare–type II–CME associations. In the above 23 cases, for more than 50% of the cases in total, the X-ray flares were not noticed and reported, because the background intensity of X-ray flux was high. In the remaining cases, the X-ray intensity might be greatly reduced due to occultation. From the Hα flare data, Yohkoh SXT data and EIT-EUV data, we found that ten cases out of 23 might be frontside events, and the remaining are backside events. While the flare–type II association is found to be nearly 90%, the type II–CME association is roughly around 75%. This analysis might be useful to reduce some ambiguities regarding the association among type IIs, flares and CMEs.

Keywords

Flare Coronal Mass Ejection Radio Burst Solar Maximum Background Intensity 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.
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Copyright information

© Springer Science + Business Media, Inc. 2004

Authors and Affiliations

  • A. Shanmugaraju
    • 1
  • Y.-J. Moon
    • 2
  • Y.-H. Kim
    • 2
  • M. Dryer
    • 3
  • S. Umapathy
    • 4
  1. 1.Department of PhysicsUniversidad de los AndesBogotaColombia
  2. 2.Korea Astronomy ObservatoryDaejeonKorea
  3. 3.NOAA Space Environment CenterBoulderUSA
  4. 4.School of PhysicsMadurai Kamaraj UniversityMaduraiIndia

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