REGISTRATION
PERSONAL INFORMATION
| Submission Time: | 2017-07-10 01:33:47 UTC |
| Email: | sjjang@kasi.re.kr |
| First Name: | Soojeong |
| Middle Name: | |
| Last Name: | Jang |
| Name as it appears on badge : | Soojeong Jang |
| Affiliation: | School of Space Research, Kyung Hee University |
| Nationality: | Korea |
| Degree: | Graduate Student |
| Preferred Working Group 1st Choice: | WG 1 (Data) |
| Preferred Working Group 2nd Choice: | WG 4 (Event Campaign) |
PRESENTATION
| Title : | Two distict types of CME-flare relationships based on SOHO and STEREO |
| Abstract | |
| In this paper we present two distinct types of CME-flare relationships according to their observing time differences using 107 events from 2010 to 2013. The observing time difference, ∆T, is defined as flare peak time minus CME first appearance time at STEREO COR1 field of view. There are 41 events for group A (∆T<0) and 66 events for group B (∆T≤0). We compare CME 3D parameters (speed and kinetic energy) based on multi-spacecraft data (SOHO and STEREO A&B) and their associated flare properties (peak flux, fluence and duration). Our main results are as follows. First, there are better relationships between CME and flare parameters for group B than that of group A. Especially, CME 3D kinetic energy for group B is well-correlated with flare fluence with the correlation coefficient of 0.67, which is much stronger than that (cc=0.31) of group A. Second, the events belonging to group A have short flare durations less than 1 hour (mean=21mins), while the events for group B have longer durations up to 4 hours (mean=81mins). Third, the mean value of height at peak speed for group B is 4.05 Rs, which is noticeably higher than that of group A (1.89 Rs). This is well correlated with CME acceleration duration (cc=0.75). A higher height at peak speed and a longer acceleration duration of CME for group B could be explained by that magnetic reconnections for group B continuously occur for a longer time than those for group A. | |
LUNCH
List
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