HR: 1330h
AN: SH53A-10    [Abstracts]
TI: Sun-Earth Propagation Time of CMEs Originated at different Helio Longitudes
AU: * Lara, A
EM: alara@geofisica.unam.mx
AF: Insituto de Geofisica, UNAM, C.U., Mexico D. F, 04510 Mexico
AU: Gopalswamy, N
EM: gopals@fugee.gsfc.nasa.gov
AF: NASA Goddard Space Flight Center, Code 695.0, Greenbelt, MD 20771 United States
AU: Xie, H
EM: hong@lepvax.gsfc.nasa.gov
AF: Catholic University of America, 620 Michigan Ave., NE, Washington, DC, DC 20064 United States
AU: Gonzalez-Esparza, A
EM: americo@geofisica.unam.mx
AF: Insituto de Geofisica, UNAM, C.U., Mexico D. F, 04510 Mexico
AB: We present a study of the transport of coronal mass ejections (CMEs) in the interplanetary medium and the probability that they, or the associated shocks, reach the Earth surroundings when they are ejected in different Helio-longitudes. To reach this goal we choose the CME events associated with the active region 0486 which crosses the solar disk during October - November 2003 and produced several CMEs during its crossing from East to West limb. We measured and analyzed the speed profile of each event, we found that the speed profile of halos and partial-halo CMEs are very symmetric and an elliptical model seems to fit the profiles very well. Using a cone model we determine the space direction of CMEs and then, the most probable speed in the Sun-Earth direction. Using these speeds, we applied the CME travel time empirical model to determine the near Earth arrival times of both interplanetary CME and related shock. We found that the difference between the predicted and observed arrival times increase with the Helio-longitude of the CME. To help in the identification of CME - 1 AU shocks and to validate the empirical model, we use 2D numerical simulations of the events.
DE: 7509 Corona
DE: 7513 Coronal mass ejections
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2005 Joint Assembly