A CORAVEL radial-velocity monitoring of S stars: symbiotic activity vs. orbital separation

Details A CORAVEL radial-velocity monitoring of S stars: symbiotic activity vs. orbital separation A CORAVEL radial-velocity monitoring of S stars: symbiotic activity vs. orbital separation

1998-01-28

arxiv.org/abs/astro-ph/9801274v1

Astronomy and Astrophysics

Astrophysics

Astronomy & Astrophysics Supplements, 6 pages, 2 figures, 4 tables (LaTeX A&A). Also available at: http://obswww.unige.ch/~u

Scientific paper

10.1051/aas:1998251

Orbital elements are presented for the Tc-poor S stars HR 363 (= HD 7351) and HD 191226. With an orbital period of 4592 d (=12.6 y), HR 363 has the longest period known among S stars, and yet it is a strong X-ray source. Its X-ray flux is similar to that of HD 35155, an S star with one of the shortest orbital periods (640 d). This surprising result is put in perspective with other diagnostics of binary interaction observed in binary S stars. They reveal that there is no correlation between the level of binary interaction and the orbital period. This situation may be accounted for if the wind mass-loss rate from the giant is the principal factor controlling the activity level in these (detached) systems, via a stream of matter funneled through the inner Lagragian point.

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