Volume 411, Number 2, November IV 2003
|Page(s)||193 - 196|
|Section||Stellar structure and evolution|
|Published online||17 November 2003|
The LBV nature of Romano's star (GR 290) in M 33 *
Istituto di Astrofisica Spaziale e Fisica Cosmica, CNR, via Fosso del Cavaliere 100, 00133, Roma, Italy
2 Bologna Astronomical Observatory, INAF, Loiano Observing Station, Loiano, Italy
3 Dunsink Observatory, Castleknock, Dublin 15, Ireland
4 Dipartimento di Fisica, Università di Roma La Sapienza, Pz.le Aldo Moro 3, 00185 Roma, Italy
Corresponding author: V. F. Polcaro, email@example.com
Accepted: 23 July 2003
We report the first spectroscopic study of the LBV candidate GR 290 in M 33 (“Romano's star”) taken in February 2003, showing, besides prominent hydrogen and He i emission lines, the 4630–60 Å blend and weak He ii 4686 Å emission typical of Of stars. Our broad–band photometry shows that the star was observed during a phase of minimum optical luminosity, with , and a slightly positive colour index, which we tentatively attribute to an anomalous continuum energy distribution. We argue that GR 290 is indeed an LBV star presently in a high temperature phase, that should be followed – also in a short time – by ample spectroscopic and associated photometric variations.
Key words: stars: evolution / stars: emission-lines, Be / stars: individual: GR 290 / stars: mass-loss / galaxies: individual: M 33
© ESO, 2003
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