Other
Scientific paper
Jul 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984iue..prop.1751a&link_type=abstract
IUE Proposal ID #IBGTA
Other
Scientific paper
In the course of an IUE investigation of chromospheric activity in S stars, we have discovered a hot, interacting companion to the otherwise unremarkable S star HD 35155. Intense emission lines of N V, C IV, Si IV, Si III] and C III] are superimposed on a moderately hot continuum apparently partially obscured by strong absorption features. The emission-line spectrum is of higher excitation than found in the mild Ba star 56 Peg and more closely resembles that of symbiotic stars or the recurrent nova T CrB. The absorptionline spectrum appears to be dominated by Fe II as seen in Zeta-Aur systems and the peculiar binaries SX Cas and HD 207739. The few IUE observations available show UV variations of nearly a factor of 2 in the emission lines and continuum and suggest that the secondary is either highly variable on a time scale of weeks, with an outburst having occurred in late 1982, or that an eclipse occurred early in 1983. The variations of emission lines are found to depend upon excitation level, the highest level lines varying the greatest. The Mg II emission appears to show a strong absorption component obliterating part of the blue profile of the feature. If this is an eclipsing system, we are seeing stratification effects as different parts of the secondary are eclipsed. If the secondary is an accretion disk, the variations can be explained by changes in the physical conditions of the line forming regions at outburst. We propose to make further IUE observations of HD 35155, the first S star known to have an interacting companion, to distinguish between the possible models for the system. Groundbased time is being requested at KPNO to study this system and other potentially interesting S and MS stars, selected by anomalous UBV colors or radial velocity variations, which we have included here as secondary targets.
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