On the Radii of Extrasolar Giant Planets

  title={On the Radii of Extrasolar Giant Planets},
  author={Peter H. Bodenheimer and Gregory Laughlin and Douglas N. C. Lin},
  journal={The Astrophysical Journal},
We have computed evolutionary models for extrasolar planets that range in mass from 0.1MJ to 3.0MJ and that range in equilibrium temperature from 113 to 2000 K. We present four sequences of models, designed to show the structural effects of a solid (20 M⊕) core and of internal heating due to the conversion of kinetic to thermal energy at pressures of tens of bars. The model radii at ages of 4-5 Gyr are intended for future comparisons with radii derived from observations of transiting extrasolar… Expand

Tables from this paper

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
We present a systematic evaluation of the agreement between the observed radii of 90 well-characterized transiting extrasolar giant planets and their corresponding model radii. Our model radii areExpand
Shrinking binary and planetary orbits by Kozai cycles with tidal friction
At least two arguments suggest that the orbits of a large fraction of binary stars and extrasolar planets shrank by 1-2 orders of magnitude after formation: (1) the physical radius of a star shrinksExpand
Rapid heating of the atmosphere of an extrasolar planet
8-μm photometric observations of the planet HD 80606b during a 30-hour interval bracketing the periastron passage of its extremely eccentric 111.4-day orbit indicate the global heating rate is ∼4.5 h, in comparison with 3–5 days in Earth’s stratosphere, and a secondary eclipse for the planet is detected. Expand
The Evolution of Irradiated Planets: Application to Transits
Extending the theory that we derived recently for HD 209458b to different cases of strongly irradiated gaseous exoplanets, we have calculated the consistent evolution of a new transiting planet,Expand
Two extrasolar planets, HD 209458b and TrES-1, are currently known to transit bright parent stars for which physical properties can be accurately determined. The two transiting planets have veryExpand
Possible Solutions to the Radius Anomalies of Transiting Giant Planets
We calculate the theoretical evolution of the radii of all 14 of the known transiting extrasolar giant planets (EGPs) for a variety of assumptions concerning atmospheric opacity, dense inner coreExpand
Tidal evolution of close-in extra-solar planets
Abstract The distribution of eccentricities e of extra-solar planets with semi-major axes a > 0.2 AU is very uniform, and values for e are generally large. For a < 0.2 AU, eccentricities are muchExpand
On the Size Distribution of Close-In Extrasolar Giant Planets
The precisions of extrasolar planet radius measurements are reaching the point at which meaningful and discriminatory comparisons with theoretical predictions are can be made. However, care must beExpand
On the Period Distribution of Close-in Extrasolar Giant Planets
Transit (TR) surveys for extrasolar planets have recently uncovered a population of "very hot Jupiters," planets with orbital periods of P ≤ 3 days. At first sight this may seem surprising, givenExpand


Stability of Satellites around Close-in Extrasolar Giant Planets
We investigate the long-term dynamical stability of hypothetical moons orbiting extrasolar giant planets. Stellar tides brake a planet's rotation and, together with tidal migration, act to removeExpand
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
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
Models of the in Situ Formation of Detected Extrasolar Giant Planets
Abstract We present numerical simulations of the formation of the planetary companions to 47 UMa, ρ CrB, and 51 Peg. They are assumed to have formed in situ according to the basic model that a coreExpand
On the Radii of Close-in Giant Planets.
It is found that HD 209458b must be a hydrogen-rich gas giant and the large radius of a close-in gas giant is not due to the thermal expansion of its atmosphere but to the high residual entropy that remains throughout its bulk by dint of its early proximity to a luminous primary. Expand
Detection of Planetary Transits Across a Sun-like Star.
High-precision, high-cadence photometric measurements of the star HD 209458 are reported, which is known from radial velocity measurements to have a planetary-mass companion in a close orbit and the detailed shape of the transit curve due to both the limb darkening of thestar and the finite size of the planet is clearly evident. Expand
Q in the solar system
Abstract Secular changes brought about by tidal friction in the solar system are reviewed. The presence or absence of specific changes is used to bound the values of Q (the specific dissipationExpand
An extrasolar planet that transits the disk of its parent star
Planets orbiting other stars could in principle be found through the periodic dimming of starlight as a planet moves across—or ‘transits’—the line of sight between the observer and the star.Expand
A Transiting "51 Peg-like" Planet.
Doppler measurements from Keck exhibit a sinusoidal periodicity in the velocities of the G0 dwarf HD 209458, having a semiamplitude of 81 m s-1 and a period of 3.5239 days, which is indicative of aExpand
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