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

Halo coronal mass ejections (CMEs) had been rarely reported in coronagraph observations of the Sun before the Solar and Heliospheric Observatory (SOHO) mission. Since mid-1996, however, the SOHO Large Angle Spectrometric Coronagraph (LASCO) instruments have observed many halo or partial-halo CMEs. A halo CME, especially when associated with solar activity near sun center, is important for space weather concerns because it suggests the launch of a potentially geoeffective disturbance toward Earth. During the post-solar minimum period from December 1996 to June 1997, we found that all six halo CMEs that were likely Earthward-directed were associated with shocks, magnetic clouds, and moderate geomagnetic storms at Earth 3–5 days later. The results imply that magnetic cloud-like structures are a general characteristic of CMEs. Most of the storms were driven by strong, sustained southward fields either in the magnetic clouds, in the post-shock region, or both. We discuss the characteristics of the halo events observed during this period, their associated signatures near the solar surface, and their usefulness as predictors of space weather at Earth.

[1]  Gerd W. Prölss,et al.  Classification and mean behavior of magnetic storms , 1997 .

[2]  R. Howard,et al.  The observation of a coronal transient directed at earth , 1982 .

[3]  Robert L. Tokar,et al.  A prolonged He+ enhancement within a coronal mass ejection in the solar wind , 1999 .

[4]  S. Wu,et al.  Disruption of Helmet Streamers by Current Emergence , 1996 .

[5]  Bernard V. Jackson,et al.  The identification and characteristics of solar mass ejections observed in the heliosphere by the Helios 2 photometers , 1990 .

[6]  J. T. Hoeksema,et al.  THE INTERACTION OF NEW AND OLD MAGNETIC FLUXES AT THE BEGINNING OF SOLAR CYCLE 23 , 1999, astro-ph/9903404.

[7]  Douglas G. Torr,et al.  Use of FUV auroral emissions as diagnostic indicators , 1994 .

[8]  J. Bougeret,et al.  On the origin of radio emissions associated with the January 6–11, 1997, CME , 1998 .

[9]  O. S. St. Cyr,et al.  Correction to “The interplanetary events of January–May, 1997 as inferred from energetic particle data, and their relationship with solar events” , 1998 .

[10]  Charles J. Farrugia,et al.  A magnetic cloud containing prominence material: January 1997 , 1998 .

[11]  B. Tsurutani,et al.  Interplanetary origin of geomagnetic activity in the declining phase of the solar cycle , 1995 .

[12]  J. Phillips,et al.  Geomagnetic activity associated with earth passage of interplanetary shock disturbances and coronal mass ejections , 1991 .

[13]  H. Hudson,et al.  X‐ray coronal changes during Halo CMEs , 1998 .

[14]  P. K. Manoharan,et al.  IDENTIFICATION OF THE SOLAR SOURCE FOR THE 18 OCTOBER 1995 MAGNETIC CLOUD , 1997 .

[15]  Edward W. Cliver,et al.  The solar origin of the January 1997 coronal mass ejection, magnetic cloud and geomagnetic storm , 1998 .

[16]  O. White,et al.  What is solar cycle minimum , 1999 .

[17]  I. Richardson,et al.  The interplanetary events of January–May, 1997 as inferred from energetic particle data, and their relationship with solar events , 1998 .

[18]  C. Russell,et al.  Magnetic pulsations at the quasi-parallel shock , 1990 .

[19]  R. Howard,et al.  Associations between coronal mass ejections and soft X-ray events , 1983 .

[20]  C. Russell,et al.  An empirical relationship between interplanetary conditions and Dst , 1975 .

[21]  Clarence M. Korendyke,et al.  Observations of CMEs from SOHO/LASCO , 2013 .

[22]  D. Webb,et al.  Large‐scale structures and multiple neutral lines associated with coronal mass ejections , 1997 .

[23]  B. Jackson.  Helios observations of the earthward-directed mass ejection of 27 November, 1979 , 1985 .

[24]  J. Steinberg,et al.  Evidence for multiple ejecta: April 7–11, 1997, ISTP Sun‐Earth connection event , 1998 .

[25]  S. Kahler.  Solar Flares and Coronal Mass Ejections , 1992 .

[26]  J. Linker,et al.  Disruption of a helmet streamer by photospheric shear , 1995 .

[27]  B. Thompson,et al.  Cradle to grave tracking of the January 6–11,1997 Sun‐Earth connection event , 1998 .

[28]  A. Hundhausen,et al.  Activity associated with the solar origin of coronal mass ejections , 1987 .

[29]  J. Gosling,et al.  Magnetic clouds at sector boundaries , 1998 .

[30]  S. Antiochos,et al.  A Model for Solar Coronal Mass Ejections , 1998, astro-ph/9807220.

[31]  Donald A. Gurnett,et al.  The January 10, 1997 auroral hot spot, horseshoe aurora and first substorm: A CME loop? , 1998 .

[32]  L. Burlaga,et al.  Magnetic field structure of interplanetary magnetic clouds at 1 AU , 1990 .

[33]  H. Hudson,et al.  Yohkoh SXT Observations of X-Ray “Dimming” Associated with a Halo Coronal Mass Ejection , 1997 .

[34]  Jean-Pierre Delaboudiniere,et al.  Geomagnetic storms caused by coronal mass ejections (CMEs): March 1996 through June 1997 , 1998 .

[35]  A. Guglielmi.  Comment on the ponderomotive self‐action of Alfvén waves , 1997 .

[36]  Craig E. Deforest,et al.  The origin and development of the May 1997 magnetic cloud , 2000 .

[37]  D. Webb.  The solar sources of coronal mass ejections , 1992 .

[38]  D. Webb,et al.  Activity associated with coronal mass ejections at solar minimum: SMM observations from 1984–1986 , 1991 .

[39]  E. Cliver,et al.  An estimate of the maximum speed of the solar wind, 1938-1989 , 1990 .

[40]  S. Kahler.  The morphological and statistical properties of solar X-ray events with long decay times , 1977 .

[41]  N. Crooker,et al.  Transients associated with recurrent storms , 1997 .

[42]  Nancy U. Crooker,et al.  Postmodern view of M-regions , 1994 .

[43]  P. Lamy,et al.  The Large Angle Spectroscopic Coronagraph (LASCO) , 1995 .

[44]  Jean-Pierre Delaboudiniere,et al.  SOHO/EIT Observations of the 1997 April 7 Coronal Transient: Possible Evidence of Coronal Moreton Waves , 1999 .

[45]  J. Steinberg,et al.  A two‐stream, four‐sector, recurrence pattern: Implications from WIND for the 22‐year geomagnetic activity cycle , 1996 .

[46]  R. MacQueen,et al.  The association of coronal mass ejection transients with other forms of solar activity , 1979 .

[47]  B. Tsurutani,et al.  Origin of interplanetary southward magnetic fields responsible for major magnetic storms near solar maximum (1978–1979) , 1988 .

[48]  J. Geiss,et al.  Unusual composition of the solar wind in the 2–3 May 1998 CME observed with SWICS on ACE , 1999 .

[49]  J. B. Gurman,et al.  SOHO/EIT observations of an Earth‐directed coronal mass ejection on May 12, 1997 , 1998 .

[50]  P. Lamy,et al.  The Large Angle Spectroscopic Coronagraph (LASCO) , 1995 .