SPECTRAL AND PHOTOMETRIC DIAGNOSTICS OF GIANT PLANET FORMATION SCENARIOS

@article{Spiegel2012SPECTRALAP,
  title={SPECTRAL AND PHOTOMETRIC DIAGNOSTICS OF GIANT PLANET FORMATION SCENARIOS},
  author={David S. Spiegel and Adam S. Burrows},
  journal={The Astrophysical Journal},
  year={2012},
  volume={745}
}
Gas-giant planets that form via core accretion might have very different characteristics from those that form via disk instability. Disk-instability objects are typically thought to have higher entropies, larger radii, and (generally) higher effective temperatures than core-accretion objects. In this paper, we provide a large set of models exploring the observational consequences of high-entropy (hot) and low-entropy (cold) initial conditions, in the hope that this will ultimately help to… 

The Planetary Luminosity Problem: “Missing Planets” and the Observational Consequences of Episodic Accretion

The high occurrence rates of spiral arms and large central clearings in protoplanetary disks, if interpreted as signposts of giant planets, indicate that gas giants commonly form as companions to

The formation of giant planets in wide orbits by photoevaporation-synchronized migration

The discovery of giant planets in wide orbits represents a major challenge for planet formation theory. In the standard core accretion paradigm planets are expected to form at radial distances

Luminosity of young Jupiters revisited Massive cores make hot planets

Context. The intrinsic luminosity of young Jupiters is of high interest for planet formation theory. It is an observable quantity that is determined by important physical mechanisms during formation,

DISK-FED GIANT PLANET FORMATION

Massive giant planets, such as the ones being discovered by direct imaging surveys, likely experience the majority of their growth through a circumplanetary disk. We argue that the entropy of

Constraints on planets in nearby young moving groups detectable by high-contrast imaging and Gaia astrometry

The formation of giant planets can be studied through direct imaging by observing planets both during and after formation. Giant planets are expected to form either by core accretion, which is

Observability of planet–disc interactions in CO kinematics

Empirical evidence of planets in gas-rich circumstellar discs is required to constrain giant planet formation theories. Here we study the kinematic patterns which arise from planet-disc interactions

Synthetic evolution tracks of giant planets

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 this

The likelihood of detecting young giant planets with high-contrast imaging and interferometry

Giant planets are expected to form at orbital radii that are relatively large compared to transit and radial velocity detections (>1 au). As a result, giant planet formation is best observed

Detectability of embedded protoplanets from hydrodynamical simulations

We predict magnitudes for young planets embedded in transition discs, still affected by extinction due to material in the disc. We focus on Jupiter-sized planets at a late stage of their formation,

THE EVOLUTION OF CIRCUMPLANETARY DISKS AROUND PLANETS IN WIDE ORBITS: IMPLICATIONS FOR FORMATION THEORY, OBSERVATIONS, AND MOON SYSTEMS

Using radiation hydrodynamics simulations, we explore the evolution of circumplanetary disks around wide-orbit proto-gas giants. At large distances from the star (∼100 AU), gravitational instability
...

References

SHOWING 1-10 OF 69 REFERENCES

THE FORMATION MECHANISM OF GAS GIANTS ON WIDE ORBITS

The recent discoveries of massive planets on ultra-wide orbits of HR 8799 and Fomalhaut present a new challenge for planet formation theorists. Our goal is to figure out which of three giant planet

HIGH-CONTRAST IMAGING SEARCH FOR PLANETS AND BROWN DWARFS AROUND THE MOST MASSIVE STARS IN THE SOLAR NEIGHBORHOOD

There has been a long-standing discussion in the literature as to whether core accretion or disk instability is the dominant mode of planet formation. Over the last decade, several lines of evidence

THE RUNTS OF THE LITTER: WHY PLANETS FORMED THROUGH GRAVITATIONAL INSTABILITY CAN ONLY BE FAILED BINARY STARS

Recent direct imaging discoveries suggest a new class of massive, distant planets around A stars. These widely separated giants have been interpreted as signs of planet formation driven by

Possible Rapid Gas Giant Planet Formation in the Solar Nebula and Other Protoplanetary Disks

  • A. Boss
  • Physics, Geology
    The Astrophysical journal
  • 2000
New three-dimensional, "locally isothermal," hydrodynamical models without velocity damping show that a disk instability can form Jupiter-mass clumps, implying that disk instability could obviate the core accretion mechanism in the solar nebula and elsewhere.

Young Jupiters are Faint : New Models of the Early Evolution of Giant Planets

Here we show preliminary calculations of the cooling and con traction of a 2MJ planet. These calculations, which are being extended to 1–10 MJ, differ from other published “cooling tracks” in that

Can Giant Planets Form by Direct Gravitational Instability?

Gravitational instability has been invoked as a possible mechanism of the giant planet production in protoplanetary disks. Here we critically revise its viability by noting that to form planets

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 updated

The Evolution of Gravitationally Unstable Protoplanetary Disks: Fragmentation and Possible Giant Planet Formation

We carry out a large set of very high resolution, three-dimensional, smoothed particle hydrodynamics simulations describing the evolution of gravitationally unstable gaseous protoplanetary disks. We

Giant Planet Occurrence in the Stellar Mass-Metallicity Plane

Correlations between stellar properties and the occurrence rate of exoplanets can be used to inform the target selection of future planet-search efforts and provide valuable clues about the

On the Luminosity of Young Jupiters

Traditional thermal evolution models of giant planets employ arbitrary initial conditions selected more for computational expediency than physical accuracy. Since the initial conditions are
...