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The spectrum of the B[e] star BAL224

Christophe Martayan·Michele Floquet·Anne-Marie Hubert·Jean Zorec
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Abstract

We present optical spectroscopy of the emission line star BAL 224 (V=17.3, B-V=0.46). This star also named KWBBE 485, [MA93]906 is located at the periphery of the young SMC cluster NGC 330; it is known as a photometric variable with a possible period around 1 day (Balona 1992). Furthermore it was reported as the optical counterpart of the prominent mid-infrared source (MIR1) by Kucinskas et al. (2000), indicating the presence of a dust shell. The star was included in a sample of B-type stars observed using the ESO VLT-FLAMES facilities. The presence of emission lines such as Fe II,[Fe II], [S II] make this object like a B[e] star. The H$ alpha$, H$ gamma$ and H$ delta$ lines show an asymmetrical double-peaked emission profile suggesting the presence of an accretion disk. Moreover the MACHO and OGLE light curves were analyzed; in addition to a long-term variability ($ simeq$ 2300d), a short period very close to 1 day has been detected using different methods, confirming the variability previously reported by Balona (1992). Finally the nature of this object is reconsidered.

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Christophe Martayan, Michele Floquet, Anne-Marie Hubert, Jean Zorec. 2005-10-24. The spectrum of the B[e] star BAL224. https://arxiv.org/abs/astro-ph/0510690

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