Large-scale structure of the solar wind from interplanetary scintillation measurements during the rising phase of cycle 23

2002 ◽  
Vol 29 (3) ◽  
pp. 379-388 ◽  
Author(s):  
A.R. Breen ◽  
A. Canals ◽  
R.A. Fallows ◽  
P.J. Moran ◽  
M. Kojima
Keyword(s):  
Solar Wind ◽  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Interplanetary Scintillation

Interplanetary Scintillation and Flare — Produced Disturbances

1975 ◽  
Vol 2 (6) ◽  
pp. 378-379 ◽  
Author(s):  
B.D. Ward
Keyword(s):  
Numerical Simulations ◽  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Interplanetary Scintillation ◽  
Ensemble Averaging ◽  
Multiple Spacecraft ◽  
Spacecraft Data

Determination of the large-scale structure of flare-produced disturbances requires either multiple spacecraft observations or an ensemble averaging of single spacecraft observations of a number of events. There is currently some confusion in the results of studies of shock normals derived from spacecraft data. Chao and Lepping (1974) suggest that the average shock shape near 1 AU is essentially spherical while Bavassano et al. (1973) suggest that the disturbance corresponds closely to the shapes predicted in the numerical simulations of de Young and Hundhausen (1971).

scholarly journals Non-radial solar wind flows induced by the motion of interplanetary coronal mass ejections

2004 ◽  
Vol 22 (12) ◽  
pp. 4397-4406 ◽  
Author(s):  
M. Owens ◽  
P. Cargill
Keyword(s):  
Solar Wind ◽  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Variance Analysis ◽  
Axis Orientation ◽  
Interplanetary Magnetic Fields ◽  
Interplanetary Physics ◽  
Wind Flows ◽  
Upstream Flow

Abstract. A survey of the non-radial flows (NRFs) during nearly five years of interplanetary observations revealed the average non-radial speed of the solar wind flows to be ~30km/s, with approximately one-half of the large (>100km/s) NRFs associated with ICMEs. Conversely, the average non-radial flow speed upstream of all ICMEs is ~100km/s, with just over one-third preceded by large NRFs. These upstream flow deflections are analysed in the context of the large-scale structure of the driving ICME. We chose 5 magnetic clouds with relatively uncomplicated upstream flow deflections. Using variance analysis it was possible to infer the local axis orientation, and to qualitatively estimate the point of interception of the spacecraft with the ICME. For all 5 events the observed upstream flows were in agreement with the point of interception predicted by variance analysis. Thus we conclude that the upstream flow deflections in these events are in accord with the current concept of the large-scale structure of an ICME: a curved axial loop connected to the Sun, bounded by a curved (though not necessarily circular) cross section. Key words. Interplanetary physics (flare and stream dynamics; interplanetary magnetic fields; interplanetary shocks)

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