Spectral lines from source regions of the solar wind: the O VI resonance doublet

Details Spectral lines from source regions of the solar wind: the O VI resonance doublet Spectral lines from source regions of the solar wind: the O VI resonance doublet

Sep 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...276..571s&link_type=abstract

Astronomy and Astrophysics, Vol. 276, p. 571 (1993)

Astronomy and Astrophysics

Astrophysics

9

Sun: Corona - Sun: Solar Wind - Sun: Uv Radiation

Scientific paper

We present numerical simulations of intensities and profiles of the O VI λ1O32 and λ1O38 lines expected from an equatorial and polar coronal hole at solar minimum, when observed on the plane of the sky in the 1.2 Rsun-8 Rsun range of heliocentric distance. The radial variations of coronal temperatures, densities and outflow speeds inside these structures are those n}} Withbroe (1988) through a one-fluid steady-state energy balance model. We discuss how the spectral features depend on the physical parameters of the examined structures, in order to evaluate to which extent they can put constraints on empirical models of the extended solar corona. These results may contribute to prepare and interpret SPARTAN and UVCS/SOHO future observations.

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