pub2012.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=2012 -c $type="ARTICLE" -oc pub2012.txt -ob pub2012.bib leconte.link.bib}}
@article{2012A&A...544A.124B,
author = {{Bolmont}, E. and {Raymond}, S.~N. and {Leconte}, J. and {Matt}, S.~P.
},
title = {{Effect of the stellar spin history on the tidal evolution of close-in planets}},
journal = {\aap},
archiveprefix = {arXiv},
eprint = {1207.2127},
primaryclass = {astro-ph.EP},
keywords = {stars: rotation, planets and satellites: dynamical evolution and stability, planet-star interactions},
year = 2012,
volume = 544,
eid = {A124},
pages = {A124},
abstract = {{Context. The spin rate of stars evolves substantially during their
lifetime, owing to the evolution of their internal structure and to
external torques arising from the interaction of stars with their
environments and stellar winds.
Aims: We investigate how the
evolution of the stellar spin rate affects, and is affected by, planets
in close orbits via star-planet tidal interactions.
Methods: We
used a standard equilibrium tidal model to compute the orbital evolution
of single planets orbiting both Sun-like stars and very low-mass stars
(0.1 M$_{&sun;}$). We tested two stellar spin evolution profiles,
one with fast initial rotation (1.2 day rotation period) and one with
slow initial rotation (8 day period). We tested the effect of varying
the stellar and planetary dissipations, and the planet's mass and
initial orbital radius.
Results: For Sun-like stars, the
different tidal evolution between initially rapidly and slowly rotating
stars is only evident for extremely close-in gas giants orbiting highly
dissipative stars. However, for very low-mass stars the effect of the
initial rotation of the star on the planet's evolution is apparent for
less massive (1 M$_{⊕}$) planets and typical dissipation
values. We also find that planetary evolution can have significant
effects on the stellar spin history. In particular, when a planet falls
onto the star, it can cause the star to spin up.
Conclusions:
Tidal evolution allows us to differentiate between the early behaviors
of extremely close-in planets orbiting either a rapidly rotating star or
a slowly rotating star. The early spin-up of the star allows the
close-in planets around fast rotators to survive the early evolution.
For planets around M-dwarfs, surviving the early evolution means
surviving on Gyr timescales, whereas for Sun-like stars the spin-down
brings about late mergers of Jupiter planets. In the light of this
study, we can say that differentiating one type of spin evolution from
another given the present position of planets can be very tricky. Unless
we can observe some markers of former evolution, it is nearly impossible
to distinguish the two very different spin profiles, let alone
intermediate spin-profiles. Nevertheless, some conclusions can still be
drawn about statistical distributions of planets around fully convective
M-dwarfs. If tidal evolution brings about a merger late in the stellar
history, it can also entail a noticeable acceleration of the star at
late ages, so that it is possible to have old stars that spin rapidly.
This raises the question of how the age of stars can be more tightly
constrained.
}},
doi = {10.1051/0004-6361/201219645},
adsurl = {https://ui.adsabs.harvard.edu/abs/2012A%26A...544A.124B},
localpdf = {https://ui.adsabs.harvard.edu/abs/2012A_26A...544A.124B.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2012A_26A...544A.124B.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2012A_26A...544A.124B.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2012A_26A...544A.124B.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2012A_26A...544A.124B.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2012A_26A...544A.124B.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2012A_26A...544A.124B.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2012A&A...540A..20L,
author = {{Leconte}, J. and {Chabrier}, G.},
title = {{A new vision of giant planet interiors: Impact of double diffusive convection}},
journal = {\aap},
archiveprefix = {arXiv},
eprint = {1201.4483},
primaryclass = {astro-ph.EP},
keywords = {Planets and satellites: general, Planets and satellites: composition, Planets and satellites: interiors, Planets and satellites: individual: Jupiter, Planets and satellites: individual: Saturn},
year = 2012,
volume = 540,
eid = {A20},
pages = {A20},
abstract = {{While conventional interior models for Jupiter and Saturn are based on
the simplistic assumption of a solid core surrounded by a homogeneous
gaseous envelope, we have derived new models with an inhomogeneous
distribution of heavy elements within these planets. Such a
compositional gradient hampers large-scale convection that turns into
double-diffusive convection, yielding an inner thermal profile that
departs from the traditionally assumed adiabatic interior and affecting
these planets heat content and cooling history. To address this problem,
we have developed an analytical approach to describe layered
double-diffusive convection and apply this formalism to solar system
gaseous giant planet interiors. These models satisfy all observational
constraints and yield values for the metal enrichment of our gaseous
giants that are up to 30\% to 60\% higher than previously thought. The
models also constrain the size of the convective layers within the
planets. Because the heavy elements tend to be redistributed within the
gaseous envelope, the models predict smaller than usual central cores
inside Saturn and Jupiter, with possibly no core for the latter. These
models open a new window and raise new challenges to our understanding
of the internal structure of giant (solar and extrasolar) planets, in
particular on how to determine their heavy material content, a key
diagnostic for planet formation theories.
}},
doi = {10.1051/0004-6361/201117595},
adsurl = {https://ui.adsabs.harvard.edu/abs/2012A%26A...540A..20L},
localpdf = {https://ui.adsabs.harvard.edu/abs/2012A_26A...540A..20L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2012A_26A...540A..20L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2012A_26A...540A..20L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2012A_26A...540A..20L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2012A_26A...540A..20L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2012A_26A...540A..20L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2012A_26A...540A..20L.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}