In-Situ Solar Wind and Magnetic Field Signatures of Interplanetary Coronal Mass Ejections

By T. Zurbuchen, I. G. Richardson. 2006

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In Astronomy and Astrophysics

Citations in the corpus

Bulk properties of the slow and fast solar wind and interplanetary coronal mass ejections measured by Ulysses: Three polar orbits of observations (2009, methodology): “[15] The identification of ICMEs from in-situ solar wind measurements is not a straightforward process [Gosling, 1996; Zurbuchen and Richardson, 2006].”
Geoeffective Properties of Solar Transients and Stream Interaction Regions (2017, background): “When detected in-situ CMEs are called interplanetary CME (ICMEs) based on a set of characteristic solar wind magnetic field, plasma and compositional signatures, see e.g., Zurbuchen and Richardson (2006) and Wimmer-Schweingruber et al. (2006).”
The Physical Processes of CME/ICME Evolution (2017, methodology): “The charge state composition of MCs shows elevated ionization states, which are suggestive of flare heated material being ejected with the CME (e.g., Neugebauer and Goldstein 1997; Lepri and Zurbuchen 2004; Zurbuchen and Richardson 2006).”
> 25 MeV Proton Events Observed by the High Energy Telescopes on the STEREO A and B Spacecraft and/or at Earth During the First ∼ Seven Years of the STEREO Mission (2014, background): “…decrease on 8 March is associated with passage of the ICME (Leske et al. (2013) reported field-aligned bidirectional ∼ 5 MeV SOLA: multiscsep6_fin.tex; 24 March 2014; 14:42; p. 21 proton flows, characteristic of ICMEs (e.g., Zurbuchen and Richardson (2006) and references therein) in this region).”
The Plasma and Suprathermal Ion Composition (PLASTIC) Investigation on the STEREO Observatories (2008, background): “As described, for example, by Galvin (1997) and more extensively by Zurbuchen and Richardson (2006), there are several in situ signatures used to identify ICMEs in interplanetary space; however, not all signatures are normally seen for a given event, and some signatures are not even unique to ICMEs…”
A summary of WIND magnetic clouds for years 1995-2003: model-fitted parameters, associated errors and classifications (2006, background): “Other reviews on CMEs/ICMEs are by Gosling (1990, 2000), and more recently by Zurbuchen and Richardson (2006).”
Solar wind drivers of geomagnetic storms during more than four solar cycles (2012, background): “These include interplanetary coronal mass ejections (ICMEs), the manifestations in the solar wind of CMEs, and the associated upstream shocks and postshock/sheath regions (e.g., Wimmer-Schweingruber et al. 2006; Zurbuchen & Richardson 2006, and references therein).”
The standard flare model in three dimensions - III. Slip-running reconnection properties (2013, background): “Moreover, including the magnetic could-like ICMEs, evidence of flux ropes in in-situ data accounts for at least two-thirds of observed ICMEs (see Zurbuchen & Richardson 2006 and Riley & Richardson 2012).”
Near-earth solar wind flows and related geomagnetic activity during more than four solar cycles (1963-2011) (2012, background): “…(CMEs) at the Sun, including interplanetary coronal mass ejections (ICMEs), the manifestations in the solar wind of CMEs, and the associated upstream shocks and postshock/sheath regions (see Zurbuchen & Richardson 2006 and references therein for discussion of the in-situ signatures of ICMEs).”