Physics
Scientific paper
May 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsh53a..09x&link_type=abstract
American Geophysical Union, Spring Meeting 2005, abstract #SH53A-09
Physics
2111 Ejecta, Driver Gases, And Magnetic Clouds, 2139 Interplanetary Shocks, 7513 Coronal Mass Ejections, 7519 Flares
Scientific paper
In this study, we compare the results obtained from two cone models and carry out the statistical study of the distribution of the actual size and space speed of Coronal Mass Ejections (CMEs). We improved the existing empirical CME arrival (ECA) model, based on previously developed empirical models and provided the prediction of CME transit time from the Sun to the Earth. The previous ECA model was in good agreement with the observations for high-speed CMEs. However, the agreement was not as good for low-speed events. One of possible reasons may be due to errors caused by the significant scatter of CME projection speeds in low projected-speed events. Using the cone models we reduced the errors and improved the accuracy of the ECA model by applying the cone models to halo CMEs erupted from near disk center of the Sun (within < 30 deg.) to determine the actual speed. We found that both cone models provide similar improved accuracy for the arrival time.
Gopalswamy Nat
Lara Alejandro
Michalek Gregory
Ofman Leon
Xie Hehu
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