EDP Sciences
Free Access
Volume 408, Number 1, September II 2003
Page(s) 205 - 229
Section Formation, structure and evolution of stars
DOI https://doi.org/10.1051/0004-6361:20030921
Published online 17 November 2003

A&A 408, 205-229 (2003)
DOI: 10.1051/0004-6361:20030921

On the structure and kinematics of nebulae around LBVs and LBV candidates in the LMC

K. Weis

Institut für Theoretische Astrophysik, Universität Heidelberg, Tiergartenstr. 15, 69121 Heidelberg, Germany University of Minnesota, Astronomy Department, 116 Church Street SE, Minneapolis, MN 55455, USA

Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
(Received 23 December 2002 / Accepted 10 June 2003)

We present a detailed analysis of the morphology and kinematics of nebulae around LBVs and LBV candidates in the Large Magellanic Cloud. HST images and high-resolution Echelle Spectra were used to determine the size, shape, brightness, and expansion velocities of the LBV nebulae around R 127, R 143, and S 61. For S Dor, R 71, R 99, and R 84 we discuss the possible presence of nebular emission, and derive upper limits for the size and lower limits on the expansion velocities of possible nebulae. Including earlier results for the LBV candidates S 119 and Sk $-69^\circ279$ we find that in general the nebulae around LBVs in the LMC are comparable in size to those found in the Milky Way. The expansion velocities of the LMC nebulae, however, are significantly lower - by about a factor of 3 to 4 - than those of galactic nebulae of comparable size. Galactic and LMC nebulae show about the same diversity of morphologies, but only in the LMC do we find nebulae with outflow. Bipolarity - at least to some degree - is found in nebulae in the LMC as well as in the Milky Way, and manifests a much more general feature among LBV nebulae than previously known.

Key words: stars: evolution -- stars: mass-loss -- ISM: bubbles -- ISM: jets and outflows

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© ESO 2003

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