Modeling Iron Density Enhancements In The Corona

Details Modeling Iron Density Enhancements In The Corona Modeling Iron Density Enhancements In The Corona

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21640305s&link_type=abstract

American Astronomical Society, AAS Meeting #216, #403.05; Bulletin of the American Astronomical Society, Vol. 41, p.878

Astronomy and Astrophysics

Astronomy

Scientific paper

The study is motivated by recent observations of localized enhancements in the Fe +10 and Fe +12 density at around 1.5 solar radii, near coronal streamers and streamer legs. Using a self-consistent solar wind model that extends from the chromosphere to 1 AU we study the buildup of iron in the slow solar wind. It has been suggested that iron buildup is a consequence of low heating rates, and occurs when iron decouples from the protons. The degree of coupling to the protons, which for heavy ions such as iron mainly depends on the proton temperature and density, is important for the energy budget of the heavy ions. The location and magnitude of iron buildups will therefore depend on the proton density and temperature, as well as on the rate of energy deposited in the iron gas. In this study we investigate the role of the proton density on the buildup of iron in the corona. Can observations of iron density enhancements tell us something about the proton density?

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