Coronal Outflow Velocities in a 3D Coronal Model Determined from UVCS Doppler Dimming Observations

Details Coronal Outflow Velocities in a 3D Coronal Model Determined from UVCS Doppler Dimming Observations Coronal Outflow Velocities in a 3D Coronal Model Determined from UVCS Doppler Dimming Observations

Apr 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998eostr..79..278s&link_type=abstract

Eos Trans. AGU, 79(17), Spring Mtg. Suppl., S278,

Astronomy and Astrophysics

Astrophysics

1

Solar Corona, Solar Wind

Scientific paper

We constrain coronal outflow velocity solutions, resolved along the line-of-sight, by using Doppler dimming models of H I Lyman alpha and O VI 1032/1037 Angstrom emissivities obtained with data from the Ultraviolet Coronagraph Spectrometer (UVCS) on SOHO. The local emissivities, from heliocentric heights of 1.5 to 3.0 radii, were determined from 3-D reconstructions of line-of-sight intensities obtained during the Whole Sun Month Campaign (10 Aug. -- 8 Sep. 1996). The models use electron densities derived from polarized brightness measurements made with the visible light coronagraphs on UVCS and LASCO, supplemented with data from Mark III at NCAR/MLSO. Electron temperature profiles are derived from `freezing-in' temperatures obtained from an analysis of charge state data from SWICS/Ulysses. The work concentrates on O5+ outflow velocities which are determined from an analysis of the the O VI line ratios. This analysis is less sensitive to the uncertainties in the electron density and independent of the ionization balance and elemental abundance than the analyses which use individual spectral lines. This work is supported in part by NASA under grant NAG-3192 to the Smithsonian Astrophysical Observatory, by the Italian Space Agency and by Swiss funding agencies.

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