Data Access
The ICMEs are identified based by inspection of a combination of signatures: a stronger than ambient magnetic field, relatively quiet and smooth magnetic field rotations, a low proton temperature, a higher density ratio of alpha particles to protons, an enhancement of total perpendicular pressure (Pt), a declining solar wind speed, etc. At least three of the above features are required to identify an ICME, with careful consideration of ambient solar wind. The boundaries of ICMEs are identified from a consensus of available features, usually delimited by sharp changes in plasma and magnetic field properties. For ambiguous events, we have checked the SOHO LASCO CME catalog and STEREO SECCHI observations. When there is a clear magnetic
obstacle (flux rope) in an ICME, we give the start time of the magnetic obstacle as well.
In order to survey the ICMEs as completely as possible, the ACE data has been used when the Wind data were unavailable or noisy and when Wind was near or within the magnetosphere.
Version:2.7.0
The ICMEs are identified based by inspection of a combination of signatures: a stronger than ambient magnetic field, relatively quiet and smooth magnetic field rotations, a low proton temperature, a higher density ratio of alpha particles to protons, an enhancement of total perpendicular pressure (Pt), a declining solar wind speed, etc. At least three of the above features are required to identify an ICME, with careful consideration of ambient solar wind. The boundaries of ICMEs are identified from a consensus of available features, usually delimited by sharp changes in plasma and magnetic field properties. For ambiguous events, we have checked the SOHO LASCO CME catalog and STEREO SECCHI observations. When there is a clear magnetic
obstacle (flux rope) in an ICME, we give the start time of the magnetic obstacle as well.
In order to survey the ICMEs as completely as possible, the ACE data has been used when the Wind data were unavailable or noisy and when Wind was near or within the magnetosphere.
| Role | Person | StartDate | StopDate | Note | |
|---|---|---|---|---|---|
| 1. | Author GeneralContact | spase://SMWG/Person/Lan.Jian | |||
| 2. | MetadataContact | spase://SMWG/Person/Olga.Y.Uritskaya |
For most Group 3 ICMEs, the spacecraft do not traverse some part of magnetic obstacle, so that the start time of obstacle is not given for such events.
The stop time of the magnetic obstacle, not given in the survey, is the same as the end time of the ICME event.
ΔV: change in solar wind velocity during one event; negative value indicates that the solar wind velocity declines through the event
Group: classification of ICME into three groups depending on the time variation of Pt.
Group 1: central maximum of Pt;
Group 2: plateau-like profile of Pt;
Group 3: gradual decrease after sharp increase at the leading edge.
From Group 1 to Group 3, the relative impact distance between spacecraft and central flux rope approximately increases.