Outer atmospheres of cool stars. VI - Models for Epsilon Eridani based on IUE spectra of C II, MG II, SI II, and SI III

Details Outer atmospheres of cool stars. VI - Models for Epsilon Eridani based on IUE spectra of C II, MG II, SI II, and SI III Outer atmospheres of cool stars. VI - Models for Epsilon Eridani based on IUE spectra of C II, MG II, SI II, and SI III

Apr 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...237...72s&link_type=abstract

Astrophysical Journal, Part 1, vol. 237, Apr. 1, 1980, p. 72-81.

Astronomy and Astrophysics

Astrophysics

41

Cool Stars, Iue, Metallic Stars, Stellar Atmospheres, Stellar Models, Stellar Temperature, Ultraviolet Spectra, Calcium, Chromosphere, Electron Density (Concentration), Emission Spectra, Late Stars, Line Spectra, Magnesium, Pressure, Radiative Transfer, Silicon, Stellar Spectrophotometry

Scientific paper

Observations of the ultraviolet line spectrum of the active chromosphere star, Epsilon Eridani, obtained with the IUE satellite have been analyzed. The coupled statistical equilibrium and radiative transfer equations for the prominent transitions of C II, Mg II, Si II, and Si III. A satisfactory fit to all of the line strengths can be achieved with a model similar to that recently proposed to explain bright points on the quiet sun. A surface pressure at the base of the transition region of 0.5 dynes/sq cm is derived, which is a factor of 3 higher than the quiet sun value, but a factor of 3 smaller than predicted by scaling laws, assuming a conductively heated stellar transition region. It is found that the surface fluxes of the C II 1334, 1335 and Si III 1892 emission lines are good diagnostics of pressure at the base of the transition region, but line ratio techniques using the 1892 line for estimating electron densities may be valid.

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