http://arxiv.org/abs/1601.00218
Aims. Various studies indicate that interacting binary stars of Algol type evolve non-conservatively. However, direct detection of systemic mass loss in Algols has been scarce so far. We aim at studying the systemic mass loss in Algols by looking for the presence of infrared excesses originating from the thermal emission of dust grains, which is linked to the presence of a stellar wind.
Methods. In contrast to previous studies, we make use of the fact that stellar and interstellar material is piled up at the edge of the asterosphere where the stellar wind interacts with the interstellar medium. We analyse WISE W3 $12\,\mu$m and WISE W4 $22\,\mu$m data of Algol-type binary Be and B[e] stars and the properties of their bow shocks. From the stand-off distance of the bow shock we are able to determine the mass loss rate of the binary system.
Results. Although the velocities of the stars with respect to the interstellar medium are quite low, we find bow shocks to be present in two systems, namely $\pi$ Aqr, and $\varphi$ Per, with a third system (CX Dra) showing a more irregular circumstellar environment morphology which might somehow be related to systemic mass-loss. The properties of the two bow shocks point to mass loss rates and wind velocities typical for (single) B stars, which do not support an enhanced systemic mass loss.
A. Mayer, R. Deschamps and A. Jorissen
Tue, 5 Jan 16
80/104
Comments: accepted for publication in A&A, 8 pages, 9 figures
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