Investigating Coronal Origin of the Solar Wind, a Joint SOHO/UVCS and ACE/SWICS Analysis

Details Investigating Coronal Origin of the Solar Wind, a Joint SOHO/UVCS and ACE/SWICS Analysis Investigating Coronal Origin of the Solar Wind, a Joint SOHO/UVCS and ACE/SWICS Analysis

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsh53a..12k&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SH53A-12

Astronomy and Astrophysics

Astrophysics

2164 Solar Wind Plasma, 2169 Sources Of The Solar Wind, 7500 Solar Physics, Astrophysics, And Astronomy, 7509 Corona

Scientific paper

The solar wind ion composition is generally 'frozen-in' within 5 solar radii of the Sun. Many characteristics in the elemental abundances measured in the solar wind are believed to be set in the chromospheric and low coronal levels. Therefore solar wind ion and elemental composition data combined with spectroscopic observations of the inner corona such as those from SOHO/UVCS, are ideal for investigating the coronal origin of the solar wind. We present such joint analysis using SOHO/UVCS and ACE/SWICS data along with a 3-D MHD traceback model. In October 1999, UVCS observed the west limb for 7 consecutive days with the passing of an equatorial coronal hole followed by an active region. This corresponds to a rarefaction transition from fast to slow wind seen by ACE. We present a correlation study of the electron temperature and elemental abundances between the corona and the solar wind from these two datasets. The solar wind ion and elemental composition measured by PLASTIC onboard STEREO would be valuable in conducting such analysis for investigating the formation of the solar wind.

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