Companions to peculiar red giants: HR 363 and HR 1105

Details Companions to peculiar red giants: HR 363 and HR 1105 Companions to peculiar red giants: HR 363 and HR 1105

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988esasp.281a.245a&link_type=abstract

In ESA, A Decade of UV Astronomy with the IUE Satellite, Volume 1 p 245-248 (SEE N89-10682 01-89)

Astronomy and Astrophysics

Astronomy

9

Companion Stars, Iue, Red Giant Stars, Spaceborne Astronomy, Ultraviolet Astronomy, Ultraviolet Spectra, Abundance, Mass Transfer, Stellar Activity, Stellar Composition

Scientific paper

Recent IUE observations of two Tc-deficient S-type peculiar red giants that are also spectroscopic binaries, HR 363 and HR 1105 are reported. A 675 min SWP exposure of HR 363 shows emission lines of O I 1304 and Si II 1812 and a trace of continuum. Compared to the M giants, the far UV flux may be relatively larger, indicating a possible contribution from a white dwarf companion, but no high temperature emission lines are seen to indicate that this is an interacting system where mass-transfer recently occurred. However, HR 1105 appears to have a highly variable UV companion. In 1982, no UV flux was discerned for this system, but by 1986 C IV was strong, increasing by a factor of 3 in 1987 with prominent lines of Si III, C III, O III, Si IV, and N V. Using orbital parameters, these observations are consistent with high activity occuring when the side of the S-star primary illuminated by the companion faces the Earth, but since the IUE data were taken over 3 orbits, a secular change in the UV component cannot be excluded.

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