Elemental Fractionation in the Solar Wind: SOHO Observations and Modelling

Details Elemental Fractionation in the Solar Wind: SOHO Observations and Modelling Elemental Fractionation in the Solar Wind: SOHO Observations and Modelling

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja....13362w&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #13362

Computer Science

Scientific paper

We report on the abundace of heav yions in the solar wind for selected tiime periods of about one day duration of slow (VSW < 400 km/s) and fast VSW > 500 km/s solar wind. These time periods were selected to study elemental fractionation as a function of the first ionization potential (FIP). Data were recorded with the MTOF sensor of the CELIAS instrument on SOHO. Slow and fast solar wind flows typically attributed to soolar wind originating from the streamer belt or from coronal holes, respectively. However, we find that such a simple assignement is not always possible and compositional information is needed to decide on the type of solar wind.

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