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It is well know that the coronagraphic observations of halo CMEs are subjectto projection effects. Viewing in the plane of the sky does not allow us todetermine the crucial parameters defining geoeffectivness of CMEs, such as thevelocity, width or source location. We assume that halo CMEs at the beginningphase of propagation have constant velocities, are symmetric and propagate withconstant angular widths. Using these approximations and determining projectedvelocities and difference between times when CME appears on the opposite sidesof the occulting disk we are able to get the necessary parameters. We presentconsideration for the whole halo CMEs from SOHO/LASCO catalog until the end of2000. We show that the halo CMEs are in average much more faster and wider thanthe all CMEs from the SOHO/LASCO catalog.

A new possibility to estimate the width, source location and velocity of halo CMEs