Testing Coronal and Solar Wind MHD Models with UV Spectroscopic and Visible Light Coronagraph Data

Details Testing Coronal and Solar Wind MHD Models with UV Spectroscopic and Visible Light Coronagraph Data Testing Coronal and Solar Wind MHD Models with UV Spectroscopic and Visible Light Coronagraph Data

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh42a..08s&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH42A-08

Astronomy and Astrophysics

Astrophysics

[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7549] Solar Physics, Astrophysics, And Astronomy / Ultraviolet Emissions, [7594] Solar Physics, Astrophysics, And Astronomy / Instruments And Techniques

Scientific paper

We present synoptic maps of coronal outflow velocities obtained at 2.3 Rs in the solar wind acceleration region of the corona during Solar Cycle 23. The outflow velocities are obtained by using data from the SOHO coronagraphs: H I Lyman alpha and O VI line profiles (from UVCS) and white light polarized brightness data (from LASCO). The information contained in the maps provide constraints on the electron densities, bulk outflow speeds, and anisotropic kinetic temperatures (velocity distributions for protons and minor ions. We show some examples of how these data can be used to test MHD models of the solar corona and solar wind. The data set can be used to compare empirically derived plasma parameters directly with the MHD model parameters or alternatively it can be used to compare the observed profiles with synthetic profiles obtained by forward modeling of the MHD data.

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