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CME/ICME list by Cho et al., 2003

ResourceID
spase://NASA/Catalog/CME-ICME_Cho2003

Description

CME/ICME list created by Cho et al., 2003. 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)."

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ResourceID
spase://NASA/Catalog/CME-ICME_Cho2003
ResourceHeader
ResourceName
CME/ICME list by Cho et al., 2003
AlternateName
Cho2003
ReleaseDate
2020-07-07 19:17:05Z
Description

CME/ICME list created by Cho et al., 2003. 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)."

Acknowledgement
Cho, K.-S.; Moon, Y.-J.; Dryer, M.; Fry, C. D.; Park, Y.-D.; Kim, K.-S., A statistical comparison of interplanetary shock and CME propagation models, Journal of Geophysical Research, Volume 108, Issue A12, pp. SSH 8-1, CiteID 1445, DOI 10.1029/2003JA010029
Contacts
RolePerson
1.Scientistspase://SMWG/Person/Kyung-Seok.Cho
InformationURL
Name
Cho et al. (2003): A statistical comparison of interplanetary shock and CME propagation models
URL
https://agupubs.onlinelibrary.wiley.com/doi/abs/10.1029/2003JA010029
Description

Paper published in Journal of Geophysical Research describing the method of CME/ICME selection

PriorIDs
spase://VHO/Catalog/CME-ICME_Cho2003
spase://VSPO/Catalog/CME-ICME_Cho2003
AccessInformation
RepositoryID
spase://SMWG/Repository/NASA/GSFC/CDAW
Availability
Online
AccessRights
Open
AccessURL
Name
SOHO LASCO CME CATALOG
URL
https://cdaw.gsfc.nasa.gov/CME_list/
Description

SOHO LASCO CME CATALOG

Format
Text
Encoding
ASCII
InstrumentIDs
spase://SMWG/Instrument/ACE/MAG
spase://SMWG/Instrument/ACE/SWEPAM
spase://SMWG/Instrument/Wind/3DP
spase://SMWG/Instrument/Wind/MFI
spase://SMWG/Instrument/SOHO/LASCO
PhenomenonType
CoronalMassEjection
PhenomenonType
InterplanetaryShock
PhenomenonType
MagneticCloud
TimeSpan
StartDate
1997-02-01 00:00:00Z
StopDate
2000-10-09 23:50:00Z
Caveats
Restrictions: The goal of Cho et al. [2003] article is to compare CME propagation models. so the selected CMEs are such as to have temporal and spatial proximity to the type II events in Table 1 of Fry et al (2003).
Parameter #1
Name
Event number
ParameterKey
Column 1
Description

Event number is taken from the metric type II/flare events of Fry et al. 2003

Support
SupportQuantity
Other
Parameter #2
Name
CME time
ParameterKey
Column 2
Description

UT time of first CME appearance in the LASCO C2 image (yymmdd/hhmm)

Support
SupportQuantity
Temporal
Parameter #3
Name
PA
ParameterKey
Column 3
Description

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

Units
deg
FillValue
Halo
Support
SupportQuantity
Positional
Parameter #4
Name
VCME
ParameterKey
Column 4
Description

CME velocity as determined by a linear fit from the LASCO C2 and C3 images

Units
km/s
UnitsConversion
1e3>m/s
Support
SupportQuantity
Other
Parameter #5
Name
VtypeII
ParameterKey
Column 5
Description

Mean speed of the type II radio burst

Units
km/s
UnitsConversion
1e3>m/s
Support
SupportQuantity
Other
Parameter #6
Name
DT
ParameterKey
Column 6
Description

Difference in time between the first C2 appearance of the CME and the starting time of the Type II radio burst, respectively.

Units
min
UnitsConversion
60>s
Support
SupportQuantity
Temporal
Parameter #7
Name
Shock arrival time
ParameterKey
Column 7
Description

Arrival time of shock at L1 (mmdd/hhmm)

Support
SupportQuantity
Temporal
Parameter #8
Name
ICME arrival time
ParameterKey
Column 8
Description

Observed ICME arrival date and time at L1. (mmdd/hhmm)

FillValue
-999
Support
SupportQuantity
Temporal
Parameter #9
Name
MC/Ejecta
ParameterKey
Column 9
Description

Type of ICME. M denotes magnetic cloud and E denotes ejecta.

Support
SupportQuantity
Other