Radio Signatures of Coronal Mass Ejection Interaction: Coronal Mass Ejection Cannibalism?

By Nat Gopalswamy, S. Yashiro, M. Kaiser, R. Howard, J. Bougeret. 2001

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In Astronomy and Astrophysics

Citations in the corpus

S/WAVES: The Radio and Plasma Wave Investigation on the STEREO Mission (2008, unknown): “(3) The relationship of burst “hotspots” to CMEs, shocks, interactions between several CMEs and solar wind structures (cf. Reiner et al. 1998a; Gopalswamy et al. 2001a; Knock and Cairns 2005) will be firmly established and quantified using S/WAVES direction-finding capabilities and data-driven…”
History and development of coronal mass ejections as a key player in solar terrestrial relationship (2016, methodology): “In fact the deflection could be in any direction, depending on the relative position of the coronal hole and the eruption region (Cremades et al. 2006; Gopalswamy et al. 2001).”
Properties and geoeffectiveness of magnetic clouds in the rising, maximum and early declining phases of solar cycle 23 (2005, background): “Near solar maximum the mutual interaction between CMEs and the ambient solar wind can lead to com- plex structures at 1 AU where the individual characteristics of CME(s) are no longer visible,Gopalswamy et al.(2001); Burlaga et al.(2001); Wang et al.(2003b).”
Interacting Coronal Mass Ejections and Solar Energetic Particles (2002, background): “From the radio emission characteristics of interacting CMEs, Gopalswamy et al. (2001c) found that the interaction starts∼1 hr before the intersection of trajectories.”
Intensity variation of large solar energetic particle events associated with coronal mass ejections (2004, methodology): “This is consistent with the observed DH radio emission enhancement for a duration corresponding to the transit time of the primary shock through the density enhancement of a preceding CME observed by LASCO [ Gopalswamy et al., 2001b, 2002b ].”
Magnetic Topology of Impulsive and Gradual Solar Energetic Particle Events (2002, background): “In addition, fast CMEs often overtake slower ones (Gopalswamy et al. 2001), a process that undoubtedly affects the injection, acceleration, and transport of the particles.”
The association of coronal mass ejections with their effects near the Earth (2005, methodology): “Further studies (e.g. Webb et al., 2000; Cane et al., 2000; Gopalswamy et al., 2001c; Vršnak and Gopalswamy, 2002; Michalek et al., 2002; González- Esparza et al., 2003a,b; Yurchyshyn et al., 2003) tried to improve the prediction accuracy, but they all keep suffering from the problem of deducing…”
A Global Picture of CMEs in the Inner Heliosphere (2004, background): “Some CMEs have voids with no prominence in them (Gopalswamy et al. 2001d).”
Solar Orbiter (2012, background): “Depending on the Alfvén speed in the former, the interaction may result in the strengthening or weakening of an existing shock driven by the overtaking CME or, if there is no existing shock, the formation of one (Gopalswamy et al., 2001; Gopalswamy et al., 2002).”
CME interactions with coronal holes and their interplanetary consequences (2009, background): “…observations of CMEs and their IP counterparts over the past decade have revealed that these shocks are also CME driven but the driver does not arrive at the observer because of the observer’s location with respect to the nose of the CME [see, e.g. Gopalswamy et al., 2001a; Gopalswamy, 2006a].”
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): “With the improvement of coronagraphic observations, it was confirmed in the 1990s that successive ICMEs can merge, as well as interact with solar wind streams to form a compound stream or complex ejecta (Gopalswamy et al. 2001; Burlaga et al. 2002, 2003; Wang et al. 2002).”
The Interaction of Successive Coronal Mass Ejections: A Review (2016, background): “Such complex streams may be caused by a number of factors, including 1) interaction close to the Sun, resulting in quasi-cannibalism (Gopalswamy et al., 2001), 2) the relative orientation of the successive ejecta favorable for reconnection (Lugaz et al., 2013), or 3) interaction between more than…”
The Physical Processes of CME/ICME Evolution (2017, methodology): “The cessation distance of ICME rapid deceleration (about 50 and 85 R for the 7 March 2012 and 12 December 2008 CMEs, respectively) is much shorter than the average cessation distance of 0.76 AU (163 R ) inferred indirectly by Gopalswamy et al. (2001b).”
Coronal mass ejections and other extreme characteristics of the 2003 October–November solar eruptions (2005, background): “One was a backside event and the other was a CME interaction signature [ Gopalswamy et al., 2001d ] related to the 4 November 2003 CME.”
ON SUN-TO-EARTH PROPAGATION OF CORONAL MASS EJECTIONS (2013, background): “Note that neither Gopalswamy et al. (2001) nor Winslow et al. (2015) have or examine wide-angle heliospheric imaging observations, so they cannot follow a CME continuously in the Sun–Earth space and thus cannot determine the deceleration cessation distance precisely.”