A Near-simultaneous Observation of X-ray Plasma Ejection, Coronal Mass Ejection, and Type II Radio Burst

Details A Near-simultaneous Observation of X-ray Plasma Ejection, Coronal Mass Ejection, and Type II Radio Burst A Near-simultaneous Observation of X-ray Plasma Ejection, Coronal Mass Ejection, and Type II Radio Burst

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...3e..85k&link_type=abstract

Solar Active Regions and 3D Magnetic Structure, 26th meeting of the IAU, Joint Discussion 3, 16-17 August, 2006, Prague, Czech R

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We report on the first near-simultaneous observation of X-ray plasma ejection (XPE), type II solar radio burst, and coronal mass ejection (CME) on 1999 October 26. First, an XPE was observed from 21:12 UT to 21:23 UT in the Yohkoh/ SXT field of view (1.1 to 1.4 solar radii). The XPE was initially accelerated and then constantly propagated with a speed of about 350 km/s. Second, a type II solar radio burst was observed at 21:30 UT by the Culgoora solar radio spectrograph. The burst started at the height of about 1.5 solar radii which is estimated from its starting frequency assuming the one-fold Newkirk coronal density model. From the frequency drift rate of the burst, the propagation speed is estimated to be about 400 km/s. Third, the associated CME was observed by the Mauna Loa Mk 4 coronameter (1.2 to 2.8 solar radii). The CME front was identified at 21:20 UT and its speed was 500 km/s (around 2 solar radii) at the type II starting time. By comparing these three phenomena, we found that (1) there is a remarkable difference (0.4 solar radii) between the CME front and the XPE front at 21:23 UT, (2) the type II formation height is not consistent with the CME front but with the trajectory extrapolated from the XPE front, (3) three speeds are comparable with one another. Regarding the type II origin, our results suggest two possibilities: coronal shock generation by the XPE front or the CME flank.

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