Data Access
Table 1 of Cho et al. 2003 JGR paper. Method:
CMEs are selected which have temporal and spatial proximity to the type II events in Table 1 of Fry et al (2003). C2 appearance time, PA, and speed from SOHO/LASCO CME catalog are used (http://cdaw.gsfc.nasa.gov/CME_list/). They say: "The procedure for examining the arrival time predictions of ICMEs and IP shocks for the near-simultaneous events are summarized as follows:
(1) From the 173 type II events of Fry et al. [2003], we choose a total of 101 CMEs that are within a threshold window (~90 min).
(2) We select 89 events from this group by comparing the position angles and the coordinate information of the associated flares.
(3) We apply the adopted prediction models (the ensemble of shock propagation models and the empirical CME propagation models) to the selected events. Then we look for IP shocks that appear near the predicted times. For this, we examine the IP shocks identified by Fry et al. [2003] who used the NOAA/SEC 1-min resolution ACE and/or Wind plasma and field data, searching for simultaneous jumps in velocity, density, temperature, and total magnetic field magnitude according to the Rankine-Hugoniot relations. As a result, we identified 38 IP shocks.
(4) We then search for ICMEs associated with the 38 IP shocks. For the identification of ICMEs, we look for MC and EJ from in situ magnetic field-plasma measurements and particle detection of ACE (available at http://www.srl.caltech.edu/ACE/ASC/level2/index.html). According to Burlaga [1995] and Berdichevsky et al. [2002], a MC is defined as a large flux-rope structure of an almost cylindrical shape with low plasma beta (<0.6), enhanced magnetic field strength (>10 nT), and a large and smooth rotation of the magnetic field direction. In the case of EJs, which are not flux ropes and have disordered magnetic fields, smooth rotation may not be present. We also refer to previously identified sources of ICMEs [Gopalswamy et al., 2001; Cane and Richardson, 2003] and the Magnetic Cloud Table (available at http://lepmfi.gsfc.nasa.gov/mfi/mag_cloud_pub1p.html)."
Version:2.6.0
Table 1 of Cho et al. 2003 JGR paper. Method:
CMEs are selected which have temporal and spatial proximity to the type II events in Table 1 of Fry et al (2003). C2 appearance time, PA, and speed from SOHO/LASCO CME catalog are used (http://cdaw.gsfc.nasa.gov/CME_list/). They say: "The procedure for examining the arrival time predictions of ICMEs and IP shocks for the near-simultaneous events are summarized as follows:
(1) From the 173 type II events of Fry et al. [2003], we choose a total of 101 CMEs that are within a threshold window (~90 min).
(2) We select 89 events from this group by comparing the position angles and the coordinate information of the associated flares.
(3) We apply the adopted prediction models (the ensemble of shock propagation models and the empirical CME propagation models) to the selected events. Then we look for IP shocks that appear near the predicted times. For this, we examine the IP shocks identified by Fry et al. [2003] who used the NOAA/SEC 1-min resolution ACE and/or Wind plasma and field data, searching for simultaneous jumps in velocity, density, temperature, and total magnetic field magnitude according to the Rankine-Hugoniot relations. As a result, we identified 38 IP shocks.
(4) We then search for ICMEs associated with the 38 IP shocks. For the identification of ICMEs, we look for MC and EJ from in situ magnetic field-plasma measurements and particle detection of ACE (available at http://www.srl.caltech.edu/ACE/ASC/level2/index.html). According to Burlaga [1995] and Berdichevsky et al. [2002], a MC is defined as a large flux-rope structure of an almost cylindrical shape with low plasma beta (<0.6), enhanced magnetic field strength (>10 nT), and a large and smooth rotation of the magnetic field direction. In the case of EJs, which are not flux ropes and have disordered magnetic fields, smooth rotation may not be present. We also refer to previously identified sources of ICMEs [Gopalswamy et al., 2001; Cane and Richardson, 2003] and the Magnetic Cloud Table (available at http://lepmfi.gsfc.nasa.gov/mfi/mag_cloud_pub1p.html)."
| Role | Person | StartDate | StopDate | Note | |
|---|---|---|---|---|---|
| 1. | Author | spase://SMWG/Person/Kyung-Seok.Cho |
Paper published in Journal of Geophysical Research describing the method of CME/ICME selection
Event number is taken from the metric type II/flare events of Fry et al. 2003
UT time of first CME appearance in the LASCO C2 image (yymmdd/hhmm)
Position angle of the CME in the plane of the sky. PA is measured counterclockwise in degrees from solar north. "Halo" denotes events which extend fully around the occulting disk
CME velocity as determined by a linear fit from the LASCO C2 and C3 images
Mean speed of the type II radio burst
Difference in time between the first C2 appearance of the CME and the starting time of the Type II radio burst, respectively.
Arrival time of shock at L1 (mmdd/hhmm)
Observed ICME arrival date and time at L1. (mmdd/hhmm)
Type of ICME. M denotes magnetic cloud and E denotes ejecta.