Volume 408, Number 1, September II 2003
|Page(s)||205 - 229|
|Section||Interstellar and circumstellar matter|
|Published online||17 November 2003|
On the structure and kinematics of nebulae around LBVs and LBV candidates in the LMC
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
Corresponding author: email@example.com
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 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
© ESO, 2003
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