Comparison of CME masses and kinetic energies near the sun and in the inner heliosphere

Details Comparison of CME masses and kinetic energies near the sun and in the inner heliosphere Comparison of CME masses and kinetic energies near the sun and in the inner heliosphere

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aipc..382..540w&link_type=abstract

Proceedings of the eigth international solar wind conference: Solar wind eight. AIP Conference Proceedings, Volume 382, pp. 540

Computer Science

5

Particle Emission, Solar Wind, Solar Instruments

Scientific paper

Masses have now been determined for many CMEs observed in the inner heliosphere by the Helios 1 and 2 zodiacal light photometers. The speed of the brightest material of each CME has also been measured so that, for events having both mass and speed determinations, their kinetic energies can be estimated. We compare the excess masses and kinetic energies of individual CMEs estimated in the inner heliosphere by Helios and near the Sun from observations by the Solwind (1979-1980) and SMM coronagraphs (1980). We also compare the speeds of the same CMEs. We find that the Helios mass and energy estimates are larger by factors of ~3 and 3-8, respectively, than those derived from the coronagraph data. Possible causes for the mass difference include the extended flow of CME mass through the corona that is not well measured by coronagraphs, and an increase of CME mass with height due to compression of ambient solar wind material. These results provide an important baseline for observations of CMEs from coronagraphs, from the WIND and Ulysses spacecraft and in the near future from SOHO.

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