| Issue |
EAS Publications Series
Volume 71-72, 2015
The Physics of Evolved Stars: A Conference Dedicated to the Memory of Olivier Chesneau
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|---|---|---|
| Page(s) | 53 - 56 | |
| Section | Winds, Mass Loss, Jets | |
| DOI | https://doi.org/10.1051/eas/1571010 | |
| Published online | 01 December 2015 | |
E. Lagadec, F. Millour and T. Lanz (eds)
EAS Publications Series, 71–72 (2015) 53-56
Detection of Rotational CO Emission From the Red-supergiants in the Large Magellanic Cloud
1 School of Physics and Astronomy, Cardiff University, Cardiff CF24 3AA, UK
2 University College London, London WC1E 6BT, UK
3 Center for Imaging Science and Laboratory for Multiwavelength Astrophysics, Rochester Institute of Technology, 54 Lomb Memorial Drive, Rochester, NY 14623, USA
4 Rutherford Appleton Laboratory, Chilton, Didcot, Oxfordshire OX11 0QX, UK
5 Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D 2401, 3001 Leuven, Belgium
6 Observational Cosmology Lab., Code 665, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
7 Astronomical Institute Anton Pannekoek, University of Amsterdam, PO Box 94249, 1090 GE Amsterdam, The Netherlands
8 Onsala Space Observatory, Dept. of Radio and Space Science, Chalmers University of Technology, 43992 Onsala, Sweden
9 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
10 The Johns Hopkins University, Department of Physics and Astronomy, 366 Bloomberg Center, 3400 N. Charles Street, Baltimore, MD 21218, USA
11 School of Physical & Geographical Sciences, Lennard-Jones Laboratories, Keele University, Staffordshire ST5 5BG, UK
12 Astrophysics Research Centre, School of Mathematics & Physics, Queen's University, University Road, Belfast BT7 1NN, UK
It is yet well understood how mass-loss rates from evolved stars depend on metallicities. With a half of the solar metallicity and the distance of only 50 kpc, the evolved stars of the Large Magellanic Cloud (LMC) are an ideal target for studying mass loss at low metallicity. We have obtained spectra of red-supergiants in the LMC, using the Hershel Space Observatory, detecting CO thermal lines fro J=6–5 up to 15–14 lines. Modelling CO lines with non-LTE Radiative transfer code suggests that CO lines intensities can be well explained with high gas-to-dust ratio, with no obvious reduction in mass-loss rate at the LMC. We conclude that the luminosities of the stars are dominant factors on mass-loss rates, rather than the metallicity.
© EAS, EDP Sciences, 2015