Study of variation of propagation velocity of solar wind disturbance

Details Study of variation of propagation velocity of solar wind disturbance Study of variation of propagation velocity of solar wind disturbance

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh12a0738y&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SH12A-0738

Physics

2139 Interplanetary Shocks, 3337 Numerical Modeling And Data Assimilation, 3360 Remote Sensing, 7513 Coronal Mass Ejections

Scientific paper

Interplanetary scintillation (IPS) measurements are an effective method to study the physical properties of solar wind disturbances in the inner heliosphere. In particular, all-sky map of solar wind density disturbance factor, so-called "g-value", which is derived from IPS measurements are useful to clarify the three-dimensional structure and propagation of the coronal mass ejection (CME) in the interplanetary space. All-sky maps of g-value have been obtained regularly from IPS measurements at 327 MHz with the IPS system of the Solar-Terrestrial Environment Lab., Nagoya Univ. However, observed g-value data are biased by the line-of-sight (los) integration, and it is difficult to analyze the property of interplanetary CME from observed g-value data directly. To remove the los integration effect, we made here the calculation of los integration of the g-value by assuming the shell-shape CME model which is determined by six parameters (i.e. distance from the sun, longitude and latitude of the central position, the radial thickness, the half cone angle, the local enhancement factor). We determined the most suitable set of those parameters by matching g-values obtained from the model calculations to those from IPS observations. Then, we determined the propagation speed by comparing coronagraph data, radio observations, and in situ data. In this time, we analyzed five event observed during 1997 to 2000.As result, the propagation speed of interplanetary CME is found to decelerate as radial distance increase. We consider that this deceleration of the propagation speed may depend on the condition of ambient solar wind.

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