pub2011.bib

@comment{{This file has been generated by bib2bib 1.96}}

@comment{{Command line: bib2bib -c 'not journal:"Discussions"' -c 'not title:"Correction to"' -c year=2011 -c $type="ARTICLE" -oc pub2011.txt -ob pub2011.bib leconte.link.bib}}

@article{2011OLEB...41..539H,
  author = {{Heller}, R. and {Barnes}, R. and {Leconte}, J.},
  title = {{Habitability of Extrasolar Planets and Tidal Spin Evolution}},
  journal = {Origins of Life and Evolution of the Biosphere},
  archiveprefix = {arXiv},
  eprint = {1108.4347},
  primaryclass = {astro-ph.EP},
  keywords = {Habitability, Orbital dynamics, Tidal processes, Habitable zone, Gl581d},
  year = 2011,
  volume = 41,
  pages = {539-543},
  abstract = {{Stellar radiation has conservatively been used as the key constraint to
planetary habitability. We review here the effects of tides, exerted by
the host star on the planet, on the evolution of the planetary spin.
Tides initially drive the rotation period and the orientation of the
rotation axis into an equilibrium state but do not necessarily lead to
synchronous rotation. As tides also circularize the orbit, eventually
the rotation period does equal the orbital period and one hemisphere
will be permanently irradiated by the star. Furthermore, the rotational
axis will become perpendicular to the orbit, i.e. the planetary surface
will not experience seasonal variations of the insolation. We illustrate
here how tides alter the spins of planets in the traditional habitable
zone. As an example, we show that, neglecting perturbations due to other
companions, the Super-Earth Gl581d performs two rotations per orbit and
that any primordial obliquity has been eroded.
}},
  doi = {10.1007/s11084-011-9252-3},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2011OLEB...41..539H},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011OLEB...41..539H.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011OLEB...41..539H.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011OLEB...41..539H.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011OLEB...41..539H.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011OLEB...41..539H.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011OLEB...41..539H.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011OLEB...41..539H.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011OLEB...41..539H.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2011A&A...536C...1L,
  author = {{Leconte}, J. and {Lai}, D. and {Chabrier}, G.},
  title = {{Distorted, non-spherical transiting planets: impact on the transit depth and on the radius determination (Corrigendum)}},
  journal = {\aap},
  keywords = {planets and satellites: interiors, planets and satellites: fundamental parameters, planets and satellites: general, errata, addenda, equation of state},
  year = 2011,
  volume = 536,
  eid = {C1},
  pages = {C1},
  doi = {10.1051/0004-6361/201015811e},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2011A%26A...536C...1L},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...536C...1L.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...536C...1L.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...536C...1L.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...536C...1L.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...536C...1L.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...536C...1L.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...536C...1L.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...536C...1L.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2011A&A...535A..94B,
  author = {{Bolmont}, E. and {Raymond}, S.~N. and {Leconte}, J.},
  title = {{Tidal evolution of planets around brown dwarfs}},
  journal = {\aap},
  archiveprefix = {arXiv},
  eprint = {1109.2906},
  primaryclass = {astro-ph.EP},
  keywords = {brown dwarfs, stars: rotation, planets and satellites: dynamical evolution and stability, planet-star interactions, astrobiology},
  year = 2011,
  volume = 535,
  eid = {A94},
  pages = {A94},
  abstract = {{Context. The tidal evolution of planets orbiting brown dwarfs (BDs)
presents an interesting case study because BDs' terrestrial planet
forming region is located extremely close-in. In fact, the habitable
zones of BDs range from roughly 0.001 to 0.03 AU and for the lowest-mass
BDs are located interior to the Roche limit. 
 Aims: In contrast
with stars, BDs spin up as they age. Thus, the corotation distance moves
inward. This has important implications for the tidal evolution of
planets around BDs. 
 Methods: We used a standard equilibrium tidal
model to compute the orbital evolution of a large ensemble of planet-BD
systems. We tested the effect of numerous parameters such as the initial
semi-major axis and eccentricity, the rotation period of the BD, the
masses of both the BD and planet, and the tidal dissipation factors. 
 Results: We find that all planets that form at or beyond the
corotation distance and with initial eccentricities smaller than \~{}0.1
are repelled from the BD. Some planets initially interior to corotation
can survive if their inward tidal evolution is slower than the BD's spin
evolution, but most initially close-in planets fall onto the BD. 

Conclusions: We find that the most important parameter for the tidal
evolution is the initial orbital distance with respect to the corotation
distance. Some planets can survive in the habitable zone for Gyr
timescales, although in many cases the habitable zone moves inward past
the planet's orbit in just tens to hundreds of Myr. Surviving planets
can have orbital periods of less than 10 days (as small as 10 h), so
they could be observable by transit.
}},
  doi = {10.1051/0004-6361/201117734},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2011A%26A...535A..94B},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...535A..94B.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...535A..94B.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...535A..94B.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...535A..94B.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...535A..94B.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...535A..94B.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...535A..94B.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...535A..94B.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2011A&A...528A..41L,
  author = {{Leconte}, J. and {Lai}, D. and {Chabrier}, G.},
  title = {{Distorted, nonspherical transiting planets: impact on the transit depth and on the radius determination}},
  journal = {\aap},
  archiveprefix = {arXiv},
  eprint = {1101.2813},
  primaryclass = {astro-ph.EP},
  keywords = {planets and satellites: general, planets and satellites: interiors, planets and satellites: fundamental parameters, equation of state},
  year = 2011,
  volume = 528,
  eid = {A41},
  pages = {A41},
  abstract = {{In this paper, we quantify the systematic impact of the nonspherical
shape of transiting planets caused by tidal forces and rotation on the
observed transit depth. Such a departure from sphericity leads to a bias
in the derivation of the transit radius from the light curve and affects
the comparison with planet structure and evolution models, which assume
spherical symmetry. As the tidally deformed planet projects its smallest
cross section area during the transit, the measured effective radius is
smaller than the one of the unperturbed spherical planet (which is the
radius predicted by 1D evolution models). This effect can be corrected
by calculating the theoretical shape of the observed planet. Using a
variational method and a simple polytropic assumption for the gaseous
planet structure, we derived simple analytical expressions for the
ellipsoidal shape of a fluid object (star or planet) accounting for both
tidal and rotational deformations. We determined the characteristic
polytropic indexes that describe the structures of irradiated close-in
planets within the mass range 0.3 M$_{J}$ $\lt$ M$_{p}$ $\lt$
75 M$_{J}$, at different ages, by comparing polytropic models with
the inner density profiles calculated with the full evolution code. Our
calculations yield a 20\% effect on the transit depth, i.e. a 10\%
decrease in the measured radius, for the extreme case of a 1
M$_{J}$ planet orbiting a Sun-like star at 0.01 AU, and the effect
can be greater for lower mass objects. For the closest planets detected
so far ( {\lsim} 0.05 AU), the effect on the radius is of the order of 1
to 10\%, by no means a negligible effect, enhancing the puzzling problem
of the anomalously large bloated planets. These corrections must thus be
taken into account for correctly determining the radius from the transit
light curve and when comparing theoretical models with observations. Our
analytical expressions can be easily used to calculate these
corrections, caused by the nonspherical shape of the planet, on the
observed transit depth and thus to derive the planet's real equilibrium
radius, the one to be used when comparing models with observations. They
can also be used to model ellipsoidal variations in the stellar flux now
detected in the CoRoT and Kepler light curves. We also derive directly
usable analytical expressions for the moment of inertia and the Love
number (k$_{2}$) of a fluid planet as a function of its mass and,
in the case of significant rotation, for its oblateness.

Tables B.2 and B.3 are only available in electronic form at http://www.aanda.org
}},
  doi = {10.1051/0004-6361/201015811},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2011A%26A...528A..41L},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...528A..41L.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...528A..41L.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...528A..41L.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...528A..41L.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...528A..41L.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...528A..41L.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...528A..41L.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...528A..41L.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2011A&A...528A..27H,
  author = {{Heller}, R. and {Leconte}, J. and {Barnes}, R.},
  title = {{Tidal obliquity evolution of potentially habitable planets}},
  journal = {\aap},
  archiveprefix = {arXiv},
  eprint = {1101.2156},
  primaryclass = {astro-ph.EP},
  keywords = {planets and satellites: dynamical evolution and stability, celestial mechanics, planet-star interactions, astrobiology, stars: low-mass, planets and satellites: tectonics},
  year = 2011,
  volume = 528,
  eid = {A27},
  pages = {A27},
  abstract = {{Context. Stellar insolation has been used as the main constraint on a
planet's potential habitability. However, as more Earth-like planets are
discovered around low-mass stars (LMSs), a re-examination of the role of
tides on the habitability of exoplanets has begun. Those studies have
yet to consider the misalignment between a planet's rotational axis and
the orbital plane normal, i.e. the planetary obliquity. 
 Aims:
This paper considers the constraints on habitability arising from tidal
processes due to the planet's spin orientation and rate. Since tidal
processes are far from being understood we seek to understand
differences between commonly used tidal models. 
 Methods: We apply
two equilibrium tide theories - a constant-phase-lag model and a
constant-time-lag model - to compute the obliquity evolution of
terrestrial planets orbiting in the habitable zones around LMSs. The
time for the obliquity to decrease from an Earth-like obliquity of
23.5{\deg} to 5{\deg}, the ``tilt erosion time'', is compared to the
traditional insolation habitable zone (IHZ) in the parameter space
spanned by the semi-major axis a, the eccentricity e, and the stellar
mass M$_{s}$. We also compute tidal heating and equilibrium
rotation caused by obliquity tides as further constraints on
habitability. The Super-Earth Gl581 d and the planet candidate Gl581 g
are studied as examples for these tidal processes. 
 Results:
Earth-like obliquities of terrestrial planets in the IHZ around stars
with masses {\lsim} 0.25 M$_{&sun;}$ are eroded in less than 0.1
Gyr. Only terrestrial planets orbiting stars with masses {\gsim} 0.9
M$_{&sun;}$ experience tilt erosion times larger than 1 Gyr
throughout the IHZ. Tilt erosion times for terrestrial planets in highly
eccentric orbits inside the IHZ of solar-like stars can be {\lsim} 10
Gyr. Terrestrial planets in the IHZ of stars with masses {\lsim} 0.25
M$_{&sun;}$ undergo significant tidal heating due to obliquity
tides, whereas in the IHZ of stars with masses {\gsim} 0.5
M$_{&sun;}$ they require additional sources of heat to drive
tectonic activity. The predictions of the two tidal models diverge
significantly for e {\gsim} 0.3. In our two-body simulations, Gl581 d's
obliquity is eroded to 0{\deg} and its rotation period reached its
equilibrium state of half its orbital period in $\lt$ 0.1 Gyr. Tidal
surface heating on the putative Gl581 g is {\lsim} 150 mW/m$^{2}$
as long as its eccentricity is smaller than 0.3. 
 Conclusions:
Obliquity tides modify the concept of the habitable zone. Tilt erosion
of terrestrial planets orbiting LMSs should be included by atmospheric
modelers. Tidal heating needs to be considered by geologists.
}},
  doi = {10.1051/0004-6361/201015809},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2011A%26A...528A..27H},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...528A..27H.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...528A..27H.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...528A..27H.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...528A..27H.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...528A..27H.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...528A..27H.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...528A..27H.pdf},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...528A..27H.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}