LiHe spectra from brown dwarfs to helium clusters |
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| Authors: | NF Allard A Nakayama F Stienkemeier JF Kielkopf G Guillon A Viel |
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| Institution: | 1. Observatoire de Paris, GEPI, UMR 8111, CNRS, Université Denis Diderot, 61, Avenue de l’Observatoire, F-75014 Paris, France;2. Division of Chemistry, Graduate School of Science, Hokkaido University, Sapporo 060-0810, Japan;3. Physikalisches Institut, Universität Freiburg, Hermann-Herder-Str. 3, D-76104 Freiburg, Germany;4. Department of Physics and Astronomy, University of Louisville, Louisville, KY 40292, USA;5. Institut de Physique de Rennes, UMR 6251, CNRS et Université de Rennes 1, F-35042 Rennes, France |
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| Abstract: | The detection of Li I lines is the most decisive spectral indicator of substellarity for young brown dwarfs with masses below about 0.06 solar mass. Due to the weakness of the Li resonance lines, it is important to be able to model precisely both their core widths and their wing profiles. This allows an adequate prediction of the mass at which Li lines reappear in the spectra of brown dwarfs for a given age, or reversely an accurate determination of the age of a cluster. We report improved line profiles and the dependence of line width on temperature suitable for modeling substellar atmospheres that were determined from new LiHe molecular potential energies. Over a limited range of density and temperature, comparison with laboratory measurements was used to validate the potential energies which support the spectral line profile theory. |
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| Keywords: | Line: profiles Stars: atmospheres&ndash brown dwarfs Atomic and molecular clusters |
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