Near-Earth Interplanetary Coronal Mass Ejections During Solar Cycle 23 (1996 – 2009): Catalog and Summary of Properties

Abstract

In a previous study (Cane and Richardson, J. Geophys. Res. 108(A4), SSH6-1, 2003), we investigated the occurrence of interplanetary coronal mass ejections in the nearEarth solar wind during 1996 -2002, corresponding to the increasing and maximum phases of solar cycle 23, and provided a "comprehensive" catalog of these events. In this paper, we present a revised and updated catalog of the ≈300 near-Earth ICMEs in 1996 -2009, encompassing the complete cycle 23, and summarize their basic properties and geomagnetic effects. In particular, solar wind composition and charge state observations are now considered when identifying the ICMEs. In general, these additional data confirm the earlier identifications based predominantly on other solar wind plasma and magnetic field parameters. However, the boundaries of ICME-like plasma based on charge state/composition data may deviate significantly from those based on conventional plasma/magnetic field parameters. Furthermore, the much studied "magnetic clouds", with flux-rope-like magnetic field configurations, may form just a substructure of the total ICME interval.

Relativistic electron response to the combined magnetospheric impact of a coronal mass ejection overlapping with a high‐speed stream: Van Allen Probes observations

“…Figure 3g). The proton number density and the total pressure increase early on 11 November as seen in Figures 3d and Figure 3f, showing the expected increase ahead of a CME, i.e., the so-called "sheath" region [e.g., Richardson and Cane, 2010], and the ICME itself seen as a drop in proton temperature (Figure 3e) when the proton number density and dynamic pressure have decreased (Figures 3d and 3f ). Ahead of the sheath, the transitions in B (Figure 3a), number density, and dynamic pressure, are quite distinct, suggesting a weak or steeping fast forward shock, since the transitions are somewhat less abrupt than as would be expected for a "clear" shock.…”

Solar Energetic Particles and Associated EIT Disturbances in Solar Cycle 23

“…In order to characterize the conditions in the IP medium, we used the Richardson and Cane (2010) catalog of global magnetic disturbances, i.e. ICMEs.…”

Magnetic Field Configuration Models and Reconstruction Methods for Interplanetary Coronal Mass Ejections

“…However, there is no single characteristic that is consistently observed. Lists of ICMEs measured by ACE and STEREO are maintained by Jian et al (2006), Lepping et al (2006), Richardson and Cane (2010) and Gopalswamy et al (2008), among others. ICMEs have been classified into three different classes based on their magnetic field and plasma properties (Zurbuchen and Richardson, 2006): 1.…”

“…This became the most widely-used model to describe the magnetic field structure of MCs. MCs are believed to represent about one third of the total number of ICMEs (Gosling, 1990;Richardson and Cane, 2010). However, a number of other studies proposed that a larger fraction of ICMEs are MCs; for example, the study by Li et al (2011) andMarubashi (2000) estimated the proportion of MCs to be 50% and 80%, respectively.…”

“…However, a number of other studies proposed that a larger fraction of ICMEs are MCs; for example, the study by Li et al (2011) andMarubashi (2000) estimated the proportion of MCs to be 50% and 80%, respectively. Other authors have studied the variation of the proportion of MCs among ICMEs during the solar cycle Richardson and Cane, 2010) and found that it varies from close to 100% near solar minimum to about 20-25% near solar maximum.…”