Detection of Rotational Co Emission from the Red-Supergiants in the Large Magellanic Cloud
Paper i proceeding, 2015
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.
Författare
M. Matsuura
University College London (UCL)
Cardiff University
B. Sargent
Rochester Institute of Technology
B. Swinyard
Rutherford Appleton Laboratory
University College London (UCL)
J. A. Yates
University College London (UCL)
P. Royer
KU Leuven
M. J. Barlow
University College London (UCL)
M. Boyer
NASA Goddard Space Flight Center
L. Decin
KU Leuven
Anton Pannekoek Institute for Astronomy
Theo Khouri
Chalmers, Rymd- och geovetenskap, Onsala rymdobservatorium
M. Meixner
Johns Hopkins University
Space Telescope Science Institute (STScI)
J. T. van Loon
Keele University
P. M. Woods
Queen's University Belfast
EAS Publications Series
1633-4760 (ISSN) 1638-1963 (eISSN)
Vol. 71-72 53-56Ämneskategorier
Astronomi, astrofysik och kosmologi
Fundament
Grundläggande vetenskaper
DOI
10.1051/eas/1571010
ISBN
978-2-7598-1907-2