A survey of interplanetary coronal mass ejections in the near-Earth solar wind during 1996-2002

By I. G. Richardson, H. Cane. 2003

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[1] We summarize the occurrence of interplanetary coronal mass ejections (ICMEs) in the near-Earth solar wind during 1996–2002, corresponding to the increasing and maximum phases of solar cycle 23. In particular, we give a detailed list of such events. This list, based on in situ observations, is not confined to subsets of ICMEs, such as “magnetic clouds” or those preceded by “halo” coronal mass injections (CMEs) observed by the Solar and Heliospheric Observatory/Large Angle and Spectrometric Coronagraph, and provides an overview of 214 ICMEs in the near-Earth solar wind during this period. The ICME rate increases by about an order of magnitude from solar minimum to solar maximum (when the rate is ∼3 ICMEs per solar rotation period). The rate also shows a temporary reduction during 1999 and another brief, deeper reduction in late 2000 to early 2001, which only approximately track variations in the solar 10-cm flux. In addition, there are occasional periods of several rotations duration when the ICME rate is enhanced in association with high solar activity levels. We find an indication of a periodic variation in the ICME rate, with a prominent period of ∼165 days similar to that previously reported in various solar phenomena. It is found that the fraction of ICMEs that are magnetic clouds has a solar cycle variation, the fraction being larger near solar minimum. For the subset of events that we could associate with a CME at the Sun the transit speeds from the Sun to the Earth were highest after solar maximum.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/d7bb123b4b0990ac11a85878a4c727a70223eb13

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In Astronomy and Astrophysics

1. Nat Gopalswamy
2. M. Temmer
3. N. Lugaz
4. R. Schwenn
5. T. Howard
6. D. Webb
7. B. Vršnak
8. A. Vourlidas

Citations in the corpus

• The Heliospheric Magnetic Field (2013, background): “CMEs move out through the corona and into the heliosphere where fast (slow) CMEs are accelerated (decelerated) towards the ambient solar wind speed (e.g., Gopalswamy et al., 2000; Cargill, 2004).”
• Geoeffective Properties of Solar Transients and Stream Interaction Regions (2017, background): “One additional, interesting solar cycle trend related to MCs, is their fraction from all ICMEs; near solar minimum roughly all ICME are MCs, while at solar maximum the fraction of MCs decreases dramatically to about 10–20% (e.g., Cane and Richardson 2003; Huttunen et al. 2005; Jian et al. 2006a).”
• Differences between CME‐driven storms and CIR‐driven storms (2006, background): “Plotted in purple in Figure 1b are times when CMEs are passing the Earth (the Cane and Richardson catalog [Cane and Richardson, 2003]) and plotted in yellow are times when magnetic clouds are passing the Earth (the Lepping online catalog http://lepmfi.gsfc.nasa.gov/mfi/mag_cloud_pub1. html, see…”
• Altered solar wind-magnetosphere interaction at low Mach numbers: Coronal mass ejections (2008, methodology): “…A pr 2 00 9 In section 3.1 we use the hourly-averaged OMNI-2 solar wind dataset [King and Papitashvili, 2005], together with lists of intervals of coronal mass ejections [Cane and Richardson, 2003], magnetic clouds [e.g., Lepping et al., 2006], high-speed streams, and global sawtooth oscillations.”
• Major geomagnetic storms (Dst<=-100~nT) generated by corotating interaction regions in 1996--2004 (2006, methodology): “The Richardson and Cane [2005] Dst–Bs relationship for ICMEs, if applicable to CIRs, suggests that since Bs in CIRs rarely exceeds 20 nT, CIR-generated storms may only be expected to reach Dst 175 nT.”
• CME interactions with coronal holes and their interplanetary consequences (2009, background): “It is well known that coronal mass ejections (CMEs) arriving at Earth generally originate close to the disk center (within the longitude range of ±30o) of the Sun [see, e.g., Bravo and Blanco-Cano, 1998; Gopalswamy et al., 2000a; Cane and Richardson, 2003].”
• A statistical study of the properties of interplanetary coronal mass ejections from 0.3 to 5.4 AU (2005, background): “Fortunately these situations do not occur frequently, as shown by Cane and Richardson (2003).”
• Interplanetary conditions causing intense geomagnetic storms (Dst ≤ −100 nT) during solar cycle 23 (1996–2006) (2008, methodology): “This shock is preceded by a MC ICME and followed by a nonMC ICME, according to the Cane and Richardson [2003] catalogue.”
• Coronal Mass Ejections: Observations (2012, background): “Studies investigating this include those involving post-eruptive arcades (Tripathi et al., 2004), interplanetary transients and shocks (Cane and Richardson, 2003; Howard and Tappin, 2005), and heliospheric imagers (Howard and Simnett, 2008).”
• The Physical Processes of CME/ICME Evolution (2017, background): “Ruffenach et al. (2015) analyzed the magnetic flux content of 50 MCs and found erosion at the front or rear in similar proportions with an average of 40% of the total azimuthal magnetic flux removed by reconnection.”
• How Many CMEs Have Flux Ropes? Deciphering the Signatures of Shocks, Flux Ropes, and Prominences in Coronagraph Observations of CMEs (2012, background): “Cane and Richardson (2003) found that 100% of ICMEs detected during solar minimum were MCs reducing to 20% during solar maximum.”
• Particle acceleration at perpendicular shock waves: Model and observations (2005, background): “( Cane and Richardson [2003] identified a short time interval with solar wind characteristics typical of an ICME from 42/1600 UT to 42/2000 UT (i.e., from 42.666 to 42.8333), but it is difficult to see what influence it may have had on the upstream medium and especially on the possible absence of w”
• Properties and geoeffectiveness of magnetic clouds in the rising, maximum and early declining phases of solar cycle 23 (2005, background): “Cane and Richardson(2003) found that near solar minimum nearly 100% of all observed ICMEs at 1 AU had the MC structure and the fraction decreased to 10–20% when solar maximum was reached.”
• Catalog of large-scale solar wind phenomena during 1976–2000 (2009, background): “It is important to note that, unlike numerous papers where similar boundary approaches were used for selection of only one or two stream types (see, for example, [12, 13 ]), this paper realizes this approach with a single set of criteria to eight large-scale stream types and demonstrates that it ca”
• Near-earth solar wind flows and related geomagnetic activity during more than four solar cycles (1963-2011) (2012, methodology): “The ICME identifications made in our previous studies (e.g., Richardson & Cane 1993; Richardson & Cane 1995; Richardson et al. 1997; Cane & Richardson 2003; Richardson & Cane 2010) have been incorporated into the solar wind classification.”