Relationship of halo coronal mass ejections, magnetic clouds, and magnetic storms

By D. Webb, E. Cliver, N. Crooker, O. S. Cyr, Barbara J. Thompson. 2000

315 citations recorded by the source corpus.

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In Astronomy and Astrophysics

Citations in the corpus

Determination of geometrical and kinematical properties of halo coronal mass ejections using the cone model (2002, background): “The close relationship of front-side halo CMEs, magnetic clouds, and magnetic storms has been demonstrated recently [Webb et al., 2000; Zhao and Webb, 2000], further suggesting that the central position of halo CMEs is located far away from the solar limb.”
Geoeffectiveness of halo coronal mass ejections (2007, background): “discussed by Webb et al. [2000] who found temporal association between three geomagnetic storms and backside halo CMEs.”
Identification of Solar Sources of Major Geomagnetic Storms between 1996 and 2000 (2003, methodology): “They may be caused by puzzling ‘‘ toroidal ’’ halo CMEs (Brueckner et al. 1998; Webb et al. 2000).”
Coronal prominence structure and dynamics: A magnetic flux rope interpretation (2006, background): “[2] Coronal mass ejections (CMEs) are arguably the most important solar drivers of space weather [Lindsay et al., 1999; Webb et al., 2000].”
Multiple magnetic clouds: Several examples during March-April 2001 (2003, background): “Usually, such geoeffective halo CMEs will affect geomagnetic field within 3–5 days [Webb et al., 2000].”
A survey of interplanetary coronal mass ejections in the near-Earth solar wind during 1996-2002 (2003, background): “Various studies have linked apparently Earthward-directed CMEs with in situ observations of ICMEs at 1 AU, focusing, for example, on their geomagnetic effects or transit times [e.g., Webb et al., 2000; Cane et al., 1998a, 2000; Gopalswamy et al., 2000, 2001; Wang et al., 2002].”
NO TRACE LEFT BEHIND: STEREO OBSERVATION OF A CORONAL MASS EJECTION WITHOUT LOW CORONAL SIGNATURES (2009, background): “These storms were driven by magnetic clouds with flux-rope characteristics, but could not be associated with any frontside (halo) CME (Webb et al. 2000).”
A Global Picture of CMEs in the Inner Heliosphere (2004, background): “Although halo CMEs are known from pre-SOHO observations (Howard et al. 1982), SOHO observations have demonstrated their prevalence (Webb et al., 2000; St. Cyr et al., 2000; Webb, 2002; Gopal- 14 swamy et al., 2003b; Michalek et al. 2003; Yashiro et al., 2004).”
A statistical study on the geoeffectiveness of Earth‐directed coronal mass ejections from March 1997 to December 2000 (2002, background): “…including solar wind speed, interplanetary magnetic field, proton temperature, and density observations from Wind spacecraft [e.g., Cliver et al., 1990; Richardson and Cane, 1995; McAllister and Crooker, 1997; Lindsay et al., 1999; Webb et al., 1998, 2000; Gopalswamy et al., 2000, 2001a, 2001b].”
Coronal mass ejections of solar cycle 23 (2006, background): “Halo CMEs, once thought to be of questionable existence, have proved to be the major players in space weather, thanks to the high sensitivity and large field of view of the SOHO/LASCO coronagraphs (see, e.g., Webb et al., 2000).”
What is the source of the magnetic helicity shed by CMEs? The long-term helicity budget of AR 7978 (2002, background): “It is a strong hypothesis to suppose that each CME detected by LASCO becomes a magnetic cloud but there are increasing evidences that it is so (Webb et al. 2000).”
The Interaction of Successive Coronal Mass Ejections: A Review (2016, background): “CMEs are also the primary drivers of intense geomagnetic storms at Earth (Gonzalez and Tsurutani, 1987; Gosling et al., 1991; Webb et al., 2000; Zhang et al., 2007), and they are also associated with many of the strongest substorms (Kamide et al., 1998; Tsurutani et al., 2015), changes in Earth…”