The Fe/O elemental abundance ratio in the solar wind as observed with SOHO CELIAS CTOF

Details The Fe/O elemental abundance ratio in the solar wind as observed with SOHO CELIAS CTOF The Fe/O elemental abundance ratio in the solar wind as observed with SOHO CELIAS CTOF

Nov 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999jgr...10424769a&link_type=abstract

Journal of Geophysical Research, Volume 104, Issue A11, p. 24769-24780

Astronomy and Astrophysics

Astrophysics

13

Interplanetary Physics: Solar Wind Plasma, Interplanetary Physics: Sources Of The Solar Wind, Solar Physics, Astrophysics, And Astronomy: Chromosphere, And Astronomy: Corona

Scientific paper

Using data of the Charge Time-of-Flight (CTOF) mass spectrometer of the Charge, Element, and Isotope Analysis System (CELIAS) on board the Solar and Heliospheric Observatory (SOHO) from ~80 days of observation around solar minimum we derive a value for the Fe/O abundance ratio for the inecliptic solar wind of 0.11+/-0.03. Since Fe has a low first ionization potential (FIP) and O is a high-FIP element, their relative abundance is diagnostic for the FIP fractionation process. The unprecedented time resolution of the CELIAS CTOF sensor allows a fine-scaled study of the Fe/O ratio as a function of the solar wind bulk speed. On average, the Fe/O abundance ratio shows a continuous decrease by a factor of 2 with increasing solar wind speed between 350 and 500 km/s. This corresponds to the well-known FIP effect dependence. Our value at ~500 km/s agrees with the previously observed Fe/O ratio in the fast solar wind emerging from polar coronal holes whereas the value for speeds below 350 km/s is consistent with a remote abundance determination in the leg of a coronal streamer. The variability of the Fe/O abundance ratio is much larger in the slow than in the fast solar wind.

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