Relation between Shock and CME Velocities During the Rise to Solar Maximum in the Intermediate Corona

Details Relation between Shock and CME Velocities During the Rise to Solar Maximum in the Intermediate Corona Relation between Shock and CME Velocities During the Rise to Solar Maximum in the Intermediate Corona

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh21b..04z&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SH21B-04

Physics

7509 Corona, 7513 Coronal Mass Ejections, 7534 Radio Emissions, 7549 Ultraviolet Emissions, 7851 Shock Waves

Scientific paper

We considered type II radio bursts observations in conjunction with the SOHO-UVCS synoptic program of monitoring of the extended solar corona. We selected events observed during the period 1999-2000, in order to have a good continuity in the synoptic observations and frequency of radio bursts. Our main purpose is to obtain information about the velocity of the shock, and compare it with the observed CME speed to determine if the shock is piston-driven or blast-wave driven. A major improvement with respect to previous analogous studies, is that we do not use electron density models taken from literature, but we estimate the densities soon before and after the passage of the shock from UVCS observations of the O VI doublet line intensities. The background outflow speed of the coronal plasma is calculated with the Doppler dimming technique applied to the O VI doublet. The above density determinations allow us to constrain the magnetic field intensity above the active regions corresponding to CME's and radio bursts with proper assumptions about the magnetic field geometry and the propagation direction of the shock.

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