Three short-period binaries seen at high-dispersion UX ARI, IOTA TRI and HA5110

Details Three short-period binaries seen at high-dispersion UX ARI, IOTA TRI and HA5110 Three short-period binaries seen at high-dispersion UX ARI, IOTA TRI and HA5110

Dec 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984nascp2349..404l&link_type=abstract

In NASA. Goddard Space Flight Center Future of Ultraviolet Astronomy Based on Six Years of IUE Res. p 404-407 (SEE N85-20961 1

Astronomy and Astrophysics

Astronomy

Binary Stars, Radial Velocity, Stellar Mass, Stellar Spectra, Variable Stars, G Stars, Stellar Coronas, Stellar Temperature, Ultraviolet Radiation

Scientific paper

The three short-period binary systems UX Ari (P=6.43791 days), iota Tri (P=14.732 days) and RH5110 (P=2.61328 days) represent three different evolutionary stages: (1) an evolved subgiant primary with a secondary still on the main sequence (UX Ari); (2) two evolved G giants that appear to be crossing the Hertzsprung gap for the first time together (iota Tri); and (3) an evolved subgiant that fills its Roche lobe and has lost mass to the secondary to the point where the original secondary is now about 3.5 times as massive as its evolved KOIV companion (HR5110). All three systems show strong UV emission lines indicative of plasmas ranging in temperature from 6000K to 20,000K. X-ray emission was detected from UX Ari and HR5110 indicating hot coronae. The chromospheric, transition region and coronal activity appears to be related primarily to the rotational velocity of the stars (but also to other parameters such as the depth of the convection zone). High-dispersion short-wavelength as well as long-wavelength IUE spectra of all three systems were analyzed.

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