D-day 0 C O N T A C T S
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.


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