Comparison of the extent and mass of CME events in the interplanetary medium using IPS and SMEI Thomson scattering observations

The Solar-Terrestrial Environment Laboratory (STELab), Japan, interplanetary scintillation (IPS) g-level and velocity measurements can be used to give the extent of CME disturbances in the interplanetary medium arising from the scattering of the radio waves from distant point-like natural sources through the intervening medium. In addition, white-light Thomson-scattering observations from the Solar Mass Ejection Imager (SMEI) have recorded the inner heliospheric response to several hundred CMEs. The work described here compares and details the difference in three-dimensional (3D) reconstructions for these two data sets for the well-observed 28 October 2003 halo CME seen in LASCO; this passed Earth on 29 October in the SMEI data at the same elongations as IPS g-level observations. The SMEI data analysis employs a 3D tomographic reconstruction technique that obtains perspective views from outward-flowing solar wind as observed from Earth, iteratively fitting a kinematic solar wind density model, and when av...

[1]  Z. Houminer,et al.  Corotating Plasma Streams revealed by Interplanetary Scintillation , 1971 .

[2]  Bernard V. Jackson,et al.  Low resolution three dimensional reconstruction of CMEs using solar mass ejection imager (SMEI) data , 2005, SPIE Optics + Photonics.

[3]  Bernard V. Jackson,et al.  Three-Dimensional Tomography of Interplanetary Disturbances , 2004 .

[4]  Bernard V. Jackson,et al.  Preliminary three‐dimensional analysis of the heliospheric response to the 28 October 2003 CME using SMEI white‐light observations , 2006 .

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

[6]  P. Edenhofer,et al.  Remote Sensing Observations of the Solar Corona , 1990 .

[7]  J. Steinberg,et al.  Extremely high speed solar wind: 29–30 October 2003 , 2004 .

[8]  B. Jackson,et al.  Heliospheric tomography using interplanetary scintillation observations. 1. Combined Nagoya and Cambridge data , 1998 .

[9]  Bernard V. Jackson,et al.  The Solar Mass-Ejection Imager (SMEI) Mission , 2003 .

[10]  E. Cliver,et al.  The 1859 Solar–Terrestrial Disturbance And the Current Limits of Extreme Space Weather Activity , 2004 .

[11]  M. Tokumaru,et al.  Toroidal-shaped interplanetary disturbance associated with the halo coronal mass ejection event on 14 July 2000 , 2003 .

[12]  S. Mancuso,et al.  Coronal Faraday Rotation Observations: Measurements and Limits on Plasma Inhomogeneities , 1999 .

[13]  C. Russell,et al.  The Cassini solar Faraday rotation experiment , 2004 .

[14]  Colin J. Lonsdale,et al.  Space weather capabilities of low frequency radio arrays , 2005, SPIE Optics + Photonics.

[15]  S. Mancuso,et al.  Faraday Rotation and Models for the Plasma Structure of the Solar Corona , 2000 .

[16]  N. R. Sheeley,et al.  White-light and radio sounding observations of coronal transients , 1985 .

[17]  A. Hewish,et al.  Interplanetary Scintillation of Small Diameter Radio Sources , 1964, Nature.

[18]  H. Volland,et al.  Coronal Faraday rotation during solar occultation of PSR0525 + 21 , 1980, Nature.

[19]  Bernard V. Jackson,et al.  Comparative Analyses of the CSSS Calculation in the UCSD Tomographic Solar Observations , 2005 .

[20]  T. Ohmi,et al.  Time‐dependent tomography of hemispheric features using interplanetary scintillation (IPS) remote‐sensing observations , 2003 .

[21]  B. Jackson,et al.  The source and propagation of the interplanetary disturbance associated with the full‐halo coronal mass ejection on 28 October 2003 , 2007 .

[22]  Bernard V. Jackson,et al.  Analysis of Solar Wind Events Using Interplanetary Scintillation Remote Sensing 3D Reconstructions and Their Comparison at Mars , 2007 .

[23]  M. Kojima,et al.  Solar cycle evolution of solar wind speed structure between 1973 and 1985 observed with the interplanetary scintillation method , 1987 .