LiHe spectra from brown dwarfs to helium clusters

Autor: Grégoire Guillon, John F. Kielkopf, Frank Stienkemeier, Nicole F. Allard, Akira Nakayama, Alexandra Viel
Přispěvatelé: Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Division of Chemistry, Graduate School of Science, Hokkaido University [Sapporo, Japan], Physikalisches Institut [Freiburg], Albert-Ludwigs-Universität Freiburg, Department of Physics and Astronomy [Louisville], University of Louisville, Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS)
Rok vydání: 2014
Předmět:
Atmospheric Science
Line: profiles
Brown dwarf
Aerospace Engineering
chemistry.chemical_element
Astrophysics
Stellar classification
Resonance (particle physics)
Spectral line
Stars: atmospheres-brown dwarfs
chemistry.chemical_compound
Astrophysics::Solar and Stellar Astrophysics
LiHe
Spectroscopy
Astrophysics::Galaxy Astrophysics
Helium
Line (formation)
Physics
Solar mass
Astronomy and Astrophysics
[PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph]
[CHIM.THEO]Chemical Sciences/Theoretical and/or physical chemistry
Geophysics
chemistry
Helium clusters
Space and Planetary Science
General Earth and Planetary Sciences
Astrophysics::Earth and Planetary Astrophysics
Atomic physics
Atomic and molecular clusters
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Zdroj: Advances in Space Research
Advances in Space Research, Elsevier, 2014, 54, pp.1290-1296. ⟨10.1016/j.asr.2013.08.032⟩
Advances in Space Research, 2014, 54, pp.1290-1296. ⟨10.1016/j.asr.2013.08.032⟩
ISSN: 0273-1177
Popis: International audience; 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.
Databáze: OpenAIRE
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