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Title: Two Distinct Types of CME-flare Relationships Based on SOHO and STEREO Observations

Abstract

In this paper, we present two distinct types of coronal mass ejection (CME)-flare relationships according to their observing time differences using 107 events from 2010 to 2013. The observing time difference, Δ T , is defined as flare peak time minus CME first appearance time at Solar Terrestrial Relations Observatory ( STEREO ) COR1 field of view. There are 41 events for group A (Δ T < 0) and 66 events for group B (Δ T ≥ 0). We compare CME 3D parameters (speed and kinetic energy) based on multi-spacecraft data ( SOlar and Heliospheric Observatory ( SOHO ) and STEREO A and 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. In particular, 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 of less than 1 hr (mean = 21 minutes), while the events for group B have longermore » durations up to 4 hr (mean = 81 minutes). 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 the 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 the fact that magnetic reconnections for group B continuously occur for a longer time than those for group A.« less

Authors:
;  [1]; ; ;  [2]
  1. School of Space Research, Kyung Hee University, Yongin (Korea, Republic of)
  2. Korea Astronomy and Space Science Institute, Daejeon (Korea, Republic of)
Publication Date:
OSTI Identifier:
22663126
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 845; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ACCELERATION; COMPARATIVE EVALUATIONS; CORRELATIONS; MAGNETIC RECONNECTION; MASS; SOLAR FLARES; SPACE VEHICLES; SUN; VELOCITY

Citation Formats

Jang, Soojeong, Moon, Yong-Jae, Kim, Rok-Soon, Kim, Sujin, and Lee, Jae-Ok, E-mail: moonyj@khu.ac.kr. Two Distinct Types of CME-flare Relationships Based on SOHO and STEREO Observations. United States: N. p., 2017. Web. doi:10.3847/1538-4357/AA82B4.
Jang, Soojeong, Moon, Yong-Jae, Kim, Rok-Soon, Kim, Sujin, & Lee, Jae-Ok, E-mail: moonyj@khu.ac.kr. Two Distinct Types of CME-flare Relationships Based on SOHO and STEREO Observations. United States. doi:10.3847/1538-4357/AA82B4.
Jang, Soojeong, Moon, Yong-Jae, Kim, Rok-Soon, Kim, Sujin, and Lee, Jae-Ok, E-mail: moonyj@khu.ac.kr. Sun . "Two Distinct Types of CME-flare Relationships Based on SOHO and STEREO Observations". United States. doi:10.3847/1538-4357/AA82B4.
@article{osti_22663126,
title = {Two Distinct Types of CME-flare Relationships Based on SOHO and STEREO Observations},
author = {Jang, Soojeong and Moon, Yong-Jae and Kim, Rok-Soon and Kim, Sujin and Lee, Jae-Ok, E-mail: moonyj@khu.ac.kr},
abstractNote = {In this paper, we present two distinct types of coronal mass ejection (CME)-flare relationships according to their observing time differences using 107 events from 2010 to 2013. The observing time difference, Δ T , is defined as flare peak time minus CME first appearance time at Solar Terrestrial Relations Observatory ( STEREO ) COR1 field of view. There are 41 events for group A (Δ T < 0) and 66 events for group B (Δ T ≥ 0). We compare CME 3D parameters (speed and kinetic energy) based on multi-spacecraft data ( SOlar and Heliospheric Observatory ( SOHO ) and STEREO A and 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. In particular, 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 of less than 1 hr (mean = 21 minutes), while the events for group B have longer durations up to 4 hr (mean = 81 minutes). 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 the 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 the fact that magnetic reconnections for group B continuously occur for a longer time than those for group A.},
doi = {10.3847/1538-4357/AA82B4},
journal = {Astrophysical Journal},
number = 2,
volume = 845,
place = {United States},
year = {Sun Aug 20 00:00:00 EDT 2017},
month = {Sun Aug 20 00:00:00 EDT 2017}
}