A statistical study of the properties of interplanetary coronal mass ejections from 0.3 to 5.4 AU

By Ying Liu, J. Richardson, John Winston Belcher. 2005

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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, background): “Several other studies have examined the radial evolution in the properties of the solar wind [Gazis and Lazarus, 1982; Richardson et al., 1995], ICMEs [ Liu et al., 2005 ] or both [Wang and Richardson, 2004; Liu et al., 2006].”
GEOMETRIC TRIANGULATION OF IMAGING OBSERVATIONS TO TRACK CORONAL MASS EJECTIONS CONTINUOUSLY OUT TO 1 AU (2010, background): “The MC radial width (average speed times the duration) is about 0.1 AU, relatively small compared with the average level 0.2 - 0.3 AU at 1 AU (e.g., Liu et al. 2005, 2006b).”
Properties of Interplanetary Coronal Mass Ejections at One AU During 1995 – 2004 (2006, background): “…lists of ICMEs, which are somewhat different from each other, e.g., Larson (http://sprg.ssl.berkeley.edu/∼davin/clouds/cloud list.html); Lepping (http://lepmfi.gsfc.nasa.gov/mfi/mag cloud pub1.html); Cane and Richardson (2003); Liu, Richardson, and Belcher (2005); Russell and Shinde (2005).”
Constraints on the global structure of magnetic clouds: Transverse size and curvature (2006, background): “D R A F T March 19, 2018, 6:52pm D R A F T”
The Physical Processes of CME/ICME Evolution (2017, methodology): “2007; Richardson and Cane 2010a; Liu et al. 2012, 2014c; Lugaz et al. 2015, 2016). Vandas et al. (1997) noted that a shock propagates faster inside a magnetic cloud due to the enhanced fast magnetosonic speed inside, which may result in shock-shock merging close to the nose of the magnetic cloud but”
CONNECTING SPEEDS, DIRECTIONS AND ARRIVAL TIMES OF 22 CORONAL MASS EJECTIONS FROM THE SUN TO 1 AU (2014, background): “…a CME has already expanded into an enormous structure, covering up to around 100◦ in heliocentric longitude and several tenths of an AU along the radial direction to the Sun (Burlaga et al. 1981; Bothmer & Schwenn 1998; Liu et al. 2005; Richardson & Cane 2010; Wood et al. 2010; Möstl et al. 2012).”
THE DEFLECTION OF THE TWO INTERACTING CORONAL MASS EJECTIONS OF 2010 MAY 23–24 AS REVEALED BY COMBINED IN SITU MEASUREMENTS AND HELIOSPHERIC IMAGING (2012, background): “…ejecta and the ICME are very close to the relation of Bothmer & Schwenn (1994), who found a power law of 0.78 based on in situ measurements at 1 AU for magnetic clouds, and relatively close to the power-law values of 0.92 and 0.91 found by Liu et al. (2005) and Gulisano et al. (2010), respectively.”