IUE Observations of HDE 332077

Details IUE Observations of HDE 332077 IUE Observations of HDE 332077

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...18110013a&link_type=abstract

American Astronomical Society, 181st AAS Meeting, #100.13; Bulletin of the American Astronomical Society, Vol. 24, p.1280

Astronomy and Astrophysics

Astronomy

4

Scientific paper

The Tc-poor S star HDE 332077 has been found by Jorissen and Mayor (A&A, 260, 115, 1992) to be a spectroscopic binary with an unusually high mass function. According to our current understanding of the Tc-deficient S stars, the abundance peculiarities of the primary should have been the result of mass-transfer from the secondary star when it was on the asymptotic giant branch at an earlier time. The secondary should now be a white dwarf (Johnson, Ake, and Ameen, ApJ, 402, in press). For HDE 332077, Jorissen and Mayor argue instead that the mass function, B-V color, and UV upper flux limits constrain the secondary to be an A-type main sequence companion and the primary to be more luminous than typical S stars. The system is still considered to be a post-mass transfer binary since the mass ratio is reversed for any set of reasonable masses. We have obtained IUE low dispersion spectra of this system. The LWP region is quite unusual. The spectral slope is steep and the absorption line spectrum is washed out, while Mg II 2800 Angstroms is strongly in emission. A trace of spectrum appears on a 20 hour exposure with the SWP, with a mean flux level of 6 x 10(-16) erg cm(-2) s(-1) Angstroms(-1) in the 1730 - 1980 Angstroms region. The spectral slope in the SWP is indeed that of an A-type star, but it is difficult to match the LWP and SWP fluxes simultaneously with a simple addition of a red giant and early main sequence star.

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