The spectrum of the B[e] star BAL224

Simple item page
dc.creatorMartayan, Christophe
dc.creatorFloquet, Michele
dc.creatorHubert, Anne-Marie
dc.creatorZorec, Jean
dc.date2005-10-24
dc.date.accessioned2026-07-07T06:44:00Z
dc.date.available2026-07-07T06:44:00Z
dc.descriptionWe 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.
dc.description4 pages
dc.identifierhttps://arxiv.org/abs/astro-ph/0510690
dc.identifierhttp://arxiv.org/abs/astro-ph/0510690
dc.identifierThe B(e) phenomenon, Pays-Bas (2005)
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/102630
dc.subjectAstrophysics
dc.titleThe spectrum of the B[e] star BAL224
dc.typetext

Files

Collections

arXiv