Modeling Iron Abundance Enhancements in the Slow Solar Wind

Details Modeling Iron Abundance Enhancements in the Slow Solar Wind Modeling Iron Abundance Enhancements in the Slow Solar Wind

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011apj...732..119b&link_type=abstract

The Astrophysical Journal, Volume 732, Issue 2, article id. 119 (2011).

Astronomy and Astrophysics

Astronomy

2

Sun: Abundances, Sun: Corona

Scientific paper

We have studied the behavior of Fe ions in the slow solar wind, using a fluid model extending from the chromosphere to 1 AU. Emphasis is on elemental "pileup" in the corona, i.e., a region where the Fe density increases and has a local maximum. We study the behavior of individual Fe ions relative to each other in the pileup region, where Fe+10 and Fe+12 have been used as examples. We find that elemental pileups can occur for a variety of densities and temperatures in the corona. We also calculate the ion fractions and obtain estimates for the freezing-in distance of Fe in the slow solar wind. We find that the freezing-in distance for iron is high, between 3 and 11 R sun, and that a high outflow velocity, of order 50-100 km s-1, in the region above the temperature maximum is needed to obtain ion fractions for Fe+10 and Fe+12 that are consistent with observations.

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