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Direct Observation of Low Coronal Breakout: Does Breakout Precede or Follow Solar Eruption?

Direct Observation of Low Coronal Breakout: Does Breakout Precede or Follow Solar Eruption?. Su-Chan Bong 1 , Y.-J. Moon 1 , K.-S. Cho 1 , Yeon-Han Kim 1 , Y. D. Park 1 , G. S. Choe 2 1 KASI 2 PPPL. CME Initiation. Breakout Model. (Lynch et al. 2004). 1998-03-22 Event. Red: NoRH 17GHz

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Direct Observation of Low Coronal Breakout: Does Breakout Precede or Follow Solar Eruption?

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  1. Direct Observation of Low Coronal Breakout: Does Breakout Precede or Follow Solar Eruption? Su-Chan Bong1, Y.-J. Moon1, K.-S. Cho1, Yeon-Han Kim1, Y. D. Park1, G. S. Choe2 1KASI 2PPPL

  2. CME Initiation

  3. Breakout Model (Lynch et al. 2004)

  4. 1998-03-22 Event • Red: NoRH 17GHz • Green: LASCO C1 FeIV • Blue: Yohkoh SXT AlMg

  5. Images of C1 and SXT C1 SXT

  6. CME & X-Ray Loop Height

  7. Summary of Incidents • 19:00-23:24 Slow rise of Fe XIV (C1) and X-ray loops • 23:24-23:57 Start of Fe XIV (C1) loop fast eruption • 23:33-00:08 Start of X-ray (SXT) loop fast eruption and brightening • 00:11 Start of microwave (NoRH) brightening • 00:21-00:52 Fe XIV (C1) field opening • 00:49 Microwave (NoRH) brightening maximum • 01:10 X-ray (SXT) brightening maximum • 03:50 End of microwave (NoRH) brightening • 03:53-10:00 Fe XIV (C1) open field narrowing

  8. Connectivity after the Event

  9. Connectivity during the Event

  10. CME & X-Ray Loop Height

  11. Speed and Acceleration Second acceleration Initial acceleration

  12. Conformality

  13. Flare

  14. Open Field Range

  15. Large Scale Structure

  16. Four Phase Eruption • Slow rise • The coronal loop and the underlying core slowly rise • Probably due to the increase of magnetic shear or emergence of new flux • Initial acceleration • The coronal loop and the core are accelerated up to ~200 km s-1 with a peak acceleration of 100 m s-2 • May be related to a near-surface activity (such as pre-eruptive reconnection) • Non-conformal • Breakout and second acceleration • The magnetic field apparently opens up in the field of view • The CME is accelerated up to 500 km s-1 with a peak acceleration of ~300 m s-2 • Propagation • The CME proceeds in the interplanetary space along with solar wind.

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