ICME Lists

Interplanetary coronal mass ejections (ICMEs) are defined by the net effects that a CME displays in the interplanetary medium, detected by in situ instrumentation, with specific imprints in the observations. These catalogues provide the compiled list of ICME events with an embedded magnetic obstacle (MO) observed by the spacecrafts. A MO is defined as the interval within an ICME where the magnetic pressure dominates over the plasma pressure concurrent with a rotation in the magnetic field direction.

Helios Catalog

MESSENGER Catalog

Parker Solar Probe Catalog

Solar Orbiter Catalog

STEREO Catalog

Wind Catalog


Single Viewpoint:

The single-viewpoint lists have been catalogued by year with the following ICME in situ parameters:
  • Start ICME time: defined by the IP forward shock or sheath signatures
  • End ICME time: defined by the end of the MO
  • Magnetic obstacle (MO) start/end times
  • MO characteristics:
    • Flux-Rope (F-/Fr/F+): Magnetic field changes monotonically with organized signatures of magnetic structure
      • (F-) Small field rotation
      • (Fr) Magnetic field rotation between 90 and 180 degrees
      • (F+) Large field rotation
    • Ejecta (E): Magnetic field changes monotonically without clear pattern of changes
    • Complex (Cx): Indications of more than one magnetic field rotation
  • In situ data plots
    • Magnetic field (MFI)
    • Plasma parameters (SWE)
  • Heliospheric overview using the current solar, heliospheric, and magnetospheric observatories

**Multi-Viewpoint:

The Solar Orbiter Heliospheric Imager (SoloHI), developed and operated by the U.S. Naval Research Laboratory (NRL), is one of the six remote sensing instruments on board the Solar Orbiter Mission and observes the photospheric visible light scattered by electrons in the solar wind. This catalog is based on the SoloHI observations with a multi-viewpoint perspective.

For each event detected by SoloHI:

  • We present available in-situ data and remote sensing observations detected by other solar missions that help to understand the trajectory and evolution of it
  • When possible, we identify the source of the CME and describe its main characteristics
  • We also track the CME throughout the different coronagraph and heliospheric imagers available
  • Additionally, we present a set of plots when the event is detected in-situ by the different missions
  • Finally, we complement the observations with the event described and modeled by the Space Weather Database Of Notifications, Knowledge, Information (DONKI) developed at the Community Coordinated Modeling Center (CCMC).