Calcium Emission in Interacting Binary Be Stars

Pavel Koubsk\'y , Lenka Kotkov\'a , Viktor Votruba , Mirek \v{S}lechta , Petr \v{S}koda , Petr Harmanec , Jana Nemravov\'a , Kl\'ara \v{S}ejnov\'a

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\v{S}\'arka Dvo\v{r}\'akov\'a Daniela Kor\v{c}\'akov\'a

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classification 🌌 astro-ph.SR

keywords emissioninteractingstarsbinarybinarieslinespaschenpeculiar

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Polidan (1976) suggested that Be stars showing the CaII IR triplet in emission are interacting binaries. With the advent of the Gaia satellite, which will host a spectrometer to observe stars in the range 8470--8750 \AA, we carried out a spectroscopic survey of 150 Be stars, including Be binaries. We show that the Ca II triplet in emission, often connected with emission in Paschen lines, is an indicator of a peculiar environment in a Be star disc rather than a signature of an interacting binary Be star. However, Ca II emission without visible emission in Paschen lines is observed in interacting binary stars, as well as in peculiar objects. During the survey, a new interacting Be binary - HD 81357 - was discovered.

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Calcium Emission in Interacting Binary Be Stars

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