Observatoire de Paris http://www.obspm.fr/r127-and-its-massive-star-cluster.html

R127 and its massive star cluster

1er février 2003

R127, one of the most spectacular variable massive stars in the Large Magellanic Cloud, has barely been studied from the viewpoint of its association with a massive star cluster. However such a study reveals new hints about the processes leading to the formation of an extraordinary Luminous Blue Variable (LBV) like R127. A team of astronomers from Paris Observatory and the Space Telescope Science Institute (Baltimore) has performed the most detailed study of the stellar environment of R127. Using the European Southern Observatory’s NTT telescope and a powerful image restoration algorithm, they achieve an angular resolution of 0".26, which enables them to resolve R127 into at least 14 components. The spectral classification as well as the photometry allows studying the history of star formation in this interesting region of our neighbour galaxy.

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The Large Magellanic Cloud massive star clusters R127 (at the center) and R128 (to the left). This "true-colour" picture results from the combination of three individual images obtained in October 2002 with SUSI2 at ESO NTT, through filters H-alpha (red), [O III] (green) and H-beta (blue). The nebula around R127 is particularly prominent. North is up and east to the left. The field size is about 95" x 72", corresponding to 24 x 18 pc. Click on the picture for higher resolution.

The most luminous object of the R127 cluster belongs to the very rare class of LBVs, which has only a dozen confirmed members in the Large Magellanic Cloud. These most luminous stars are characterized by irregular photometric and spectral variations over decades and transform from a hot (OB type) visual minimum phase to a cooler (A) type at visual maximum. In the H-R diagram they are located very close to the observed upper luminosity boundary for very massive stars, the Humphrey-Davidson limit. They are characterized by extreme instability, dramatic outbursts and high mass loss. LBVs are believed to be the precursors of Wolf-Rayet stars ; however their precise evolutionary state is still poorly understood. It is therefore necessary to study every aspect of these rare stars in order to constrain theoretical models. R127 is an odd object even among this extraordinary family of stars : it is the most luminous LBV in the Large Magellanic Cloud (bolometric magnitude of -10.5), and has shown the most intense light variations (about 2.5 mag in the V band). Shortly before its recorded maximum in 1986, R127 was the brightest object of the Large Magellanic Cloud, until the supernova event in 1987. From 1989 until 2000 its brightness decreased, and it has been increasing since. Spectroscopy was obtained for 19 stars associated with the R127/R128 clusters, using the ESO NTT telescope equipped with EMMI. It turns out that the most luminous stars of these clusters are giants or supergiants of spectral type O and, for a smaller number, B. The study of the H-R diagram, involving comparison with models of stellar evolution, yields information about the present and past characteristics of the stars. The team of astronomers arrives at the conclusion that the LBV object was born about 3 million years ago as the most massive star of the R127/R128 clusters, with a mass of about 85 solar masses. Comparison with its present mass indicates that the LBV has lost about 45% of its original mass, with a mean mass loss rate of around 10-5 solar masses per year. The next brightest and hottest stars of the group are two supergiants with initial masses of about 80 solar masses, formed about 3 million years ago. Less massive stars have ages of 3 to 5 million years. It seems therefore that the most massive stars have formed after the formation of less massive stars.

Reference : M. Heydari-Malayeri, F. Meynadier and Nolan R. Walborn, Tight LMC massive star clusters R127 and R128 (A&A : accepted 07/01/2003) Prepublication : astro-ph/0301298 Contact

Frédéric Meynadier (Observatoire de Paris, LERMA)

Dernière modification le 4 mars 2013