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- W2153760237 abstract "We present new high-resolution coronographic imaging and medium-resolution spectroscopy of the circum- stellar region around S 61 and BE 381, two Ofpe/WN9 stars in the Large Magellanic Cloud. The observations were carried out at the ESO/NTT (La Silla) in January 1996 and July 1998. The excellent seeing conditions allowed the circumstellar nebulae associated with both S 61 and BE 381 to be spatially resolved for the first time. The nebula surrounding S 61 has the appear- ance of a shell with a mild central axisymmetry. The surface brightness is not uniform, and the northern region of the nebula is the brightest. The nebula exhibits a bipolar structure with an overall morphology very similar to nebulae around other LBVs or Opfe/WN9 stars, especially S119. The diameter of the shell is 7.3 00 , corresponding to a linear size of 1.8 pc. From the profile of nebular emission lines we clearly detect an expansion mo- tion with a velocity of 28 km s 1 , which indicates a dynamical age of 30000 yrs. We find an electron density of 400 cm 3 and an electron temperature of 6120 K. The nebula is similar to other LBV nebulae in that it is nitrogen enriched. The observed chemical and dynamical properties confirm that the nebula is as- sociated with the central star and is of stellar origin. This result implies that S 61 is likely to have undergone a LBV-type ouburst and, therefore, strenghtens the suggestion that Ofpe/WN9 stars are quiescent LBVs. The situation is different for BE 381. The H images of BE 381 also reveal the presence of a faint neb- ulosity around the star; most of the nebular flux appears to be emitted by an arc of gas located to the east of BE 381, while a much dimmer arc is detectable on the western side. The arcs delineate a shell of 13 00 in diameter, corresponding to a linear size of 3.2 pc, which appears to be expanding with a velocity of 14 km s 1 . From the nebular emission lines we derive an elec- tron density ranging between 30 cm 3 and 120 cm 3 (assuming Te = 10000 K), and a N + /S + ratio between 1.5 and 2.3, which are typical of HII regions. We therefore conclude that the shell detected around BE 381 is not of stellar origin and probably represents the relic of the interstellar bubble blown by BE 381 during its O main-sequence phase." @default.
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- W2153760237 date "1999-03-01" @default.
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- W2153760237 title "SPATIALLY RESOLVED NEBULAE AROUND THE OFPE/WN9 STARS S 61 AND BE 381" @default.
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