Radial Expansion of Coronal Mass Ejections at 1 AU

Details Radial Expansion of Coronal Mass Ejections at 1 AU Radial Expansion of Coronal Mass Ejections at 1 AU

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh61a10m&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SH61A-10

Physics

2111 Ejecta, Driver Gases, And Magnetic Clouds, 2134 Interplanetary Magnetic Fields, 2164 Solar Wind Plasma

Scientific paper

We study the the radial dependence of the interplanetary magnetic field (IMF) intensity inside coronal mass ejections (CME) around 1 AU. We selected the CME times from the OMNI database (1965-2000) using the low-temperature criterion T/Texp<0.5, where T is the observed plasma temperature and Texp is the temperature expected from the measured solar wind speed. We find a significant difference in the IMF intensity at perihelion and apohelion for low-temperature events (i.e., CMEs). Moreover, this difference is twice as much as that obtained for the non-low-temperature times, i.e. in the ambient solar wind. During low-temperature times, the radial dependence is found to be similar for the total, tangential and radial IMF magnitudes, deviating strongly from the Parker prediction. Our observations verify that the radial expansion of CMEs is still going on at 1 AU and that the the average expansion rate is close to R-3, where R stands for the radial distance from the Sun.

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