Sun-Earth Propagation Time of the October - November 2003 Shocks

Details Sun-Earth Propagation Time of the October - November 2003 Shocks Sun-Earth Propagation Time of the October - November 2003 Shocks

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agusmsh51a..06l&link_type=abstract

American Geophysical Union, Spring Meeting 2004, abstract #SH51A-06

Astronomy and Astrophysics

Astrophysics

7500 Solar Physics, Astrophysics, And Astronomy, 7513 Coronal Mass Ejections

Scientific paper

We computed the radial and expansion speed profiles of the CMEs that resulted in shocks detected at 1 AU, in order to evaluate the empirical shock arrival (ESA) model. The CMEs were observed by the Large Angle and Spectrometric Coronagraph (LASCO) on board SOHO during October - November 2003 period. The shocks were detected by CELIAS/MTOF Proton Monitor on board SOHO and ACE spacecraft. The basic input to the ESA model is the CME speed. For limb events, we assume axial symmetry in order to obtain the most probable CME speed in the Sun-Earth direction. We apply the ESA model to obtain the travel times of shocks driven by Earth-directed and limb CMEs which had in situ observations at 1AU. For most cases the difference between the predicted and observed shock arrival times is negligible. We discuss these differences and their possible causes. Work supported by NASA/LWS and NSF/SHINE programs

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