Evolutionary models for cool brown dwarfs and extrasolar giant planets. The case of HD 209458

@article{Baraffe2003EvolutionaryMF,
  title={Evolutionary models for cool brown dwarfs and extrasolar giant planets. The case of HD 209458},
  author={Isabelle Baraffe and Gilles Chabrier and T. Barman F. Allard and Peter Hauschildt},
  journal={Astronomy and Astrophysics},
  year={2003},
  volume={402},
  pages={701-712}
}
We present evolutionary models for cool brown dwarfs and extra-solar giant planets. The models re- produce the main trends of observed methane dwarfs in near-IR color-magnitude diagrams. We also present evolutionary models for irradiated planets, coupling for the first time irradiated atmosphere profiles and inner structures. We focus on HD 209458-like systems and show that irradiation effects can substantially affect the ra- dius of sub-jovian mass giant planets. Irradiation effects, however… Expand
Young jupiters are faint: new models of the early evolution of giant planets
Here we show preliminary calculations of the cooling and contraction of a 2 MJ planet. These calculations, which are being extended to 1–10 MJ, differ from other published “cooling tracks” in thatExpand
Effects of helium phase separation on the evolution of extrasolar giant planets
We build on recent new evolutionary models of Jupiter and Saturn and here extend our calculations to investigate the evolution of extrasolar giant planets of mass 0.15MJ-3.0MJ. Our inhomogeneousExpand
CALIBRATION OF EQUILIBRIUM TIDE THEORY FOR EXTRASOLAR PLANET SYSTEMS. II
We present a new empirical calibration of equilibrium tidal theory for extrasolar planet systems, extending a prior study by incorporating detailed physical models for the internal structure ofExpand
Analytical model for the evolution of giant extrasolar planets
Abstract For extrasolar planets with well determined radii and in thermal equilibrium, the planetary luminosity can be determined. A plot of the log of the luminosity against the log of the effectiveExpand
Structure and Evolution of Giant Planets
The understanding of the structure and evolution of our solar system giant planets has significantly advanced within the past years. Important progress is due not only to direct observations and inExpand
Synthetic Spectra and Colors of Young Giant Planet Atmospheres: Effects of Initial Conditions and Atmospheric Metallicity
We examine the spectra and infrared colors of the cool, methane-dominated atmospheres at Teff ≤ 1400 K expected for young gas giant planets. We couple these spectral calculations to an updatedExpand
The physical properties of extra-solar planets
Tremendous progress in the science of extrasolar planets has been achieved since the discovery of a Jupiter orbiting the nearby Sun-like star 51 Pegasi in 1995. Theoretical models have now reachedExpand
Synthetic evolution tracks of giant planets
  • Simon Müller, R. Helled
  • Physics
  • Monthly Notices of the Royal Astronomical Society
  • 2021
Giant planet evolution models play a crucial role in interpreting observations and constraining formation pathways. However, the simulations can be slow or prohibitively difficult. To address thisExpand
Structure and evolution of the first CoRoT exoplanets: probing the brown dwarf/planet overlapping mass regime
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 radiiExpand
The Evolution of L and T Dwarfs in Color-Magnitude Diagrams
We present new evolution sequences for very low mass stars, brown dwarfs, and giant planets and use them to explore a variety of influences on the evolution of these objects. While the predictedExpand
...
1
2
3
4
5
...

References

SHOWING 1-10 OF 42 REFERENCES
Theory of Extrasolar Giant Planet Transits
We present a synthesis of physical effects influencing the observed light curve of an extrasolar giant planet (EGP) transiting its host star. The synthesis includes a treatment of RayleighExpand
Extrasolar Giant Planets under Strong Stellar Irradiation
We investigate irradiation of extrasolar giant planets (EGPs) by treating the radiative transfer in detail, so that the flux from the parent star interacts with all relevant depths of the planetaryExpand
Theoretical Transmission Spectra during Extrasolar Giant Planet Transits
The recent transit observation of HD 209458 ban extrasolar planet orbiting a Sun-like star¨ con—rmed that it is a gas giant and determined that its orbital inclination is 85i. This inclination makesExpand
A Nongray Theory of Extrasolar Giant Planets and Brown Dwarfs
We present the results of a new series of nongray calculations of the atmospheres, spectra, colors, and evolution of extrasolar giant planets (EGPs) and brown dwarfs for effective temperatures belowExpand
Evolutionary Models for Very Low-Mass Stars and Brown Dwarfs with Dusty Atmospheres
We present evolutionary calculations for very low-mass stars and brown dwarfs based on synthetic spectra and nongray atmosphere models which include dust formation and opacity, i.e., objects withExpand
Evolution of "51 Pegasus b-like" planets
About one-quarter of the extrasolar giant planets discovered so far have orbital distances smaller than 0.1 AU. These “51 Peg b-like” planets can now be directly characterized, as shown by the planetExpand
A Theory of Extrasolar Giant Planets
We present a broad suite of models of extrasolar giant planets (EGP's), ranging in mass from 0.3 to 15 Jupiter masses. The models predict luminosity (both reflected and emitted) as a function of age,Expand
Hd 209458: physical parameters of the parent star and the transiting planet
The Sun-like star HD 209458 harbors a close-in giant planet that transits across the star's disk, and thus allows an unprecedented access to the basic parameters of the planet, given a certainExpand
Giant planets at small orbital distances
Using Doppler spectroscopy to detect the reflex motion of the nearby star, 51 Pegasi, Mayor & Queloz (1995) claim to have discovered a giant planet in a 0.05 AU, 4.23 day orbit. They estimate itsExpand
Irradiated Planets
We have modeled irradiated planets located near a dM5 and a G2 primary star. The impinging radiation field was explicitly included in the solution of the radiative transfer equation and in theExpand
...
1
2
3
4
5
...