High temperature structure in cool binary stars

Details High temperature structure in cool binary stars High temperature structure in cool binary stars

Aug 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995sao..reptr....d&link_type=abstract

In Smithsonian Astrophysical Observatory 5 p (SEE N96-14306 03-90)

Astronomy and Astrophysics

Astronomy

Abundance, Binary Stars, Cool Stars, Emission Spectra, Extreme Ultraviolet Radiation, High Temperature Plasmas, Plasma Radiation, Spaceborne Astronomy, Stellar Atmospheres, Stellar Spectra, Ultraviolet Astronomy, Atmospheric Temperature, Extreme Ultraviolet Explorer Satellite, Helium, Hydrogen, Polar Regions, Stellar Coronas, Stellar Rotation

Scientific paper

Strong high temperature emission lines in the EUVE spectra of binary stars containing cool components (Alpha Aur (Capella), 44 iota Boo, Lambda And, and VY Ari) provide the basis to define reliably the differential emission measure of hot plasma. The emission measure distributions for the short-period (P less than or equal to 13 d) binary systems show a high temperature enhancement over a relatively narrow temperature region similar to that originally found in Capella (Dupree et al. 1993). The emission measure distributions of rapidly rotating single stars 31 Com and AB Dor also contain a local enhancement of the emission measure although at different temperatures and width from Capella, suggesting that the enhancement in these objects may be characteristic of rapid rotation of a stellar corona. This feature might be identified with a (polar) active region, although its density and absolute size are unknown; in the binaries Capella and VY Ari, the feature is narrow and it may arise from an interaction region between the components.

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