pub2010.bib
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@comment{{Command line: bib2bib -c 'not journal:"Discussions"' -c 'not title:"Correction to"' -c year=2010 -c $type="ARTICLE" -oc pub2010.txt -ob pub2010.bib leconte.link.bib}}
@article{2010ApJ...716.1551L,
author = {{Leconte}, J. and {Soummer}, R. and {Hinkley}, S. and {Oppenheimer}, B.~R. and
{Sivaramakrishnan}, A. and {Brenner}, D. and {Kuhn}, J. and
{Lloyd}, J.~P. and {Perrin}, M.~D. and {Makidon}, R. and {Roberts}, Jr., L.~C. and
{Graham}, J.~R. and {Simon}, M. and {Brown}, R.~A. and {Zimmerman}, N. and
{Chabrier}, G. and {Baraffe}, I.},
title = {{The Lyot Project Direct Imaging Survey of Substellar Companions: Statistical Analysis and Information from Nondetections}},
journal = {\apj},
archiveprefix = {arXiv},
eprint = {1006.3409},
primaryclass = {astro-ph.EP},
keywords = {instrumentation: adaptive optics, methods: data analysis, techniques: image processing},
year = 2010,
volume = 716,
pages = {1551-1565},
abstract = {{The Lyot project used an optimized Lyot coronagraph with extreme
adaptive optics at the 3.63 m Advanced Electro-Optical System telescope
to observe 86 stars from 2004 to 2007. In this paper, we give an
overview of the survey results and a statistical analysis of the
observed nondetections around 58 of our targets to place constraints on
the population of substellar companions to nearby stars. The
observations did not detect any companion in the substellar regime.
Since null results can be as important as detections, we analyzed each
observation to determine the characteristics of the companions that can
be ruled out. For this purpose, we use a Monte Carlo approach to produce
artificial companions and determine their detectability by comparison
with the sensitivity curve for each star. All the non-detection results
are combined using a Bayesian approach and we provide upper limits on
the population of giant exoplanets and brown dwarfs for this sample of
stars. Our nondetections confirm the rarity of brown dwarfs around
solar-like stars and we constrain the frequency of massive substellar
companions (M$\gt$40 M $_{J}$) at orbital separation between and 10
and 50 AU to be lsim20\%.
}},
doi = {10.1088/0004-637X/716/2/1551},
adsurl = {https://ui.adsabs.harvard.edu/abs/2010ApJ...716.1551L},
localpdf = {https://ui.adsabs.harvard.edu/abs/2010ApJ...716.1551L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2010ApJ...716.1551L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2010ApJ...716.1551L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2010ApJ...716.1551L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2010ApJ...716.1551L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2010ApJ...716.1551L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2010ApJ...716.1551L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2010ApJ...716.1551L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2010ApJ...716.1551L.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2010A&A...516A..64L,
author = {{Leconte}, J. and {Chabrier}, G. and {Baraffe}, I. and {Levrard}, B.
},
title = {{Is tidal heating sufficient to explain bloated exoplanets? Consistent calculations accounting for finite initial eccentricity}},
journal = {\aap},
archiveprefix = {arXiv},
eprint = {1004.0463},
primaryclass = {astro-ph.EP},
keywords = {brown dwarfs, planet-star interactions, planets and satellites: dynamical evolution and stability, planets and satellites: general},
year = 2010,
volume = 516,
eid = {A64},
pages = {A64},
abstract = {{We present the consistent evolution of short-period exoplanets coupling
the tidal and gravothermal evolution of the planet. Contrarily to
previous similar studies, our calculations are based on the complete
tidal evolution equations of the Hut (1981) model, valid at any order in
eccentricity, obliquity and spin. We demonstrate both analytically and
numerically that except if the system was formed with a nearly circular
orbit (e {\lap} 0.2), consistently solving the complete tidal equations
is mandatory to derive correct tidal evolution histories. We show that
calculations based on tidal models truncated at 2nd order in
eccentricity, as done in all previous studies, lead to quantitatively
and sometimes even qualitatively erroneous tidal evolutions. As a
consequence, tidal energy dissipation rates are severely underestimated
in all these calculations and the characteristic timescales for the
various orbital parameters evolutions can be wrong by up to three orders
of magnitude. These discrepancies can by no means be justified by
invoking the uncertainty in the tidal quality factors. Based on these
complete, consistent calculations, we revisit the viability of the tidal
heating hypothesis to explain the anomalously large radius of transiting
giant planets. We show that even though tidal dissipation does provide a
substantial contribution to the planet's heat budget and can explain
some of the moderately bloated hot-Jupiters, this mechanism can not
explain alone the properties of the most inflated objects, including HD
209 458 b. Indeed, solving the complete tidal equations shows that
enhanced tidal dissipation and thus orbit circularization occur too
early during the planet's evolution to provide enough extra energy at
the present epoch. In that case either a third, so far undetected,
low-mass companion must be present to keep exciting the eccentricity of
the giant planet, or other mechanisms - stellar irradiation induced
surface winds dissipating in the planet's tidal bulges and thus reaching
the convective layers, inefficient flux transport by convection in the
planet's interior - must be invoked, together with tidal dissipation, to
provide all the pieces of the abnormally large exoplanet puzzle.
}},
doi = {10.1051/0004-6361/201014337},
adsurl = {https://ui.adsabs.harvard.edu/abs/2010A%26A...516A..64L},
localpdf = {https://ui.adsabs.harvard.edu/abs/2010A_26A...516A..64L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2010A_26A...516A..64L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2010A_26A...516A..64L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2010A_26A...516A..64L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2010A_26A...516A..64L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2010A_26A...516A..64L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2010A_26A...516A..64L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2010A_26A...516A..64L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2010A_26A...516A..64L.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}