pub2009.bib

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@comment{{Command line: bib2bib -c 'not journal:"Discussions"' -c 'not title:"Correction to"' -c year=2009 -c $type="ARTICLE" -oc pub2009.txt -ob pub2009.bib leconte.link.bib}}

@article{2009A&A...506..385L,
  author = {{Leconte}, J. and {Baraffe}, I. and {Chabrier}, G. and {Barman}, T. and 
	{Levrard}, B.},
  title = {{Structure and evolution of the first CoRoT exoplanets: probing the brown dwarf/planet overlapping mass regime}},
  journal = {\aap},
  archiveprefix = {arXiv},
  eprint = {0907.2669},
  primaryclass = {astro-ph.EP},
  keywords = {stars: low-mass, brown dwarfs, stars: planetary systems},
  year = 2009,
  volume = 506,
  pages = {385-389},
  abstract = {{We present detailed structure and evolution calculations for the first
transiting extrasolar planets discovered by the space-based CoRoT
mission. Comparisons between theoretical and observed radii provide
information on the internal composition of the CoRoT objects. We
distinguish three different categories of planets emerging from these
discoveries and from previous ground-based surveys: (i) planets
explained by standard planetary models including irradiation; (ii)
abnormally bloated planets; and (iii) massive objects belonging to the
overlapping mass regime between planets and brown dwarfs. For the second
category, we show that tidal heating can explain the relevant CoRoT
objects, providing non-zero eccentricities. We stress that the usual
assumption of a quick circularization of the orbit by tides, as usually
done in transit light curve analysis, is not justified a priori, as
suggested recently by Levrard et al. (2009), and that eccentricity
analysis should be carefully redone for some observations. Finally,
special attention is devoted to CoRoT-3b and to the identification of
its very nature: giant planet or brown dwarf? The radius determination
of this object confirms the theoretical mass-radius predictions for
gaseous bodies in the substellar regime but, given the present
observational uncertainties, does not allow an unambiguous
identification of its very nature. This opens the avenue, however, to an
observational identification of these two distinct astrophysical
populations, brown dwarfs and giant planets, in their overlapping mass
range, as done for the case of the 8 Jupiter-mass object Hat-P-2b.
According to the presently published error bars for the radius
determination and to our present theoretical description of planet
structure and evolution, the high mean density of this object requires a
substantial metal enrichment of the interior and is inconsistent at
about the 2-sigma limit with the expected radius of a solar-metallicity
brown dwarf. Within the aforementioned observational and theoretical
determinations, this allows a clear identification of its planetary
nature, suggesting that planets may form up to at least 8 Jupiter
masses.
}},
  doi = {10.1051/0004-6361/200911896},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2009A%26A...506..385L},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2009A_26A...506..385L.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2009A_26A...506..385L.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2009A_26A...506..385L.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2009A_26A...506..385L.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2009A_26A...506..385L.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2009A_26A...506..385L.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2009A_26A...506..385L.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2009A_26A...506..385L.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2009A_26A...506..385L.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2009A_26A...506..385L.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}