On the formation of terrestrial planets in hot-Jupiter systems

@article{Fogg2007OnTF,
  title={On the formation of terrestrial planets in hot-Jupiter systems},
  author={Martyn J. Fogg and R. P. Nelson},
  journal={Astronomy and Astrophysics},
  year={2007},
  volume={461},
  pages={1195-1208}
}
  • M. Fogg, R. Nelson
  • Published 11 October 2006
  • Geology, Physics
  • Astronomy and Astrophysics
Context. There are numerous extrasolar giant planets which orbit close to their central stars. These “hot-Jupiters” probably formed in the outer, cooler regions of their protoplanetary disks, and migrated inward to ∼ 0.1 AU. Since these giant planets must have migrated through their inner systems at an early time, it is uncertain whether they could have formed or retained terrestrial planets. Aims. We present a series of calculations aimed at examining how an inner system of planetesimals… 
Terrestrial planet formation in low-eccentricity warm-Jupiter systems
Context. Extrasolar giant planets are found to orbit their host stars with a broad range of semi-major axes 0.02 ≤ a ≤ 6 AU. Current theories suggest that giant planets orbiting at distances between
On the possibility of terrestrial planet formation in hot-Jupiter systems
About a fifth of the exoplanetary systems that have been discovered contain a so-called hot-Jupiter – a giant planet orbiting within 0.1 AU of the central star. Since these stars are typically of the
The effect of type I migration on the formation of terrestrial planets in hot-Jupiter systems
Context. Our previous models of a giant planet migrating through an inner protoplanet/planetesimal disk find that the giant shepherds a portion of the material it encounters into interior orbits,
THE DESTRUCTION OF INNER PLANETARY SYSTEMS DURING HIGH-ECCENTRICITY MIGRATION OF GAS GIANTS
Hot Jupiters are giant planets on orbits of a few hundredths of an AU. They do not share their system with low-mass close-in planets, despite the latter being exceedingly common. Two migration
Debris disks as signposts of terrestrial planet formation
There exists strong circumstantial evidence from their eccentric orbits that most of the known extra-solar planetary systems are the survivors of violent dynamical instabilities. Here we explore the
TOWARD CHEMICAL CONSTRAINTS ON HOT JUPITER MIGRATION
The origin of hot Jupiters—gas giant exoplanets orbiting very close to their host stars—is a long-standing puzzle. Planet formation theories suggest that such planets are unlikely to have formed in
Formation of Earth-like Planets During and After Giant Planet Migration
Close-in giant planets are thought to have formed in the cold outer regions of planetary systems and migrated inward, passing through the orbital parameter space occupied by the terrestrial planets
In situ formation of hot Jupiters with companion super-Earths
Observations have confirmed the existence of multiple-planet systems containing a hot Jupiter and smaller planetary companions. Examples include WASP-47, Kepler-730, and TOI-1130. We examine the
Planet formation in radiatively inefficient protoplanetary discs
I examine the effects on planetary system formation of radiatively inefficient disc models where positive corotation torques may counter the rapid inward migration of low-mass planets driven by
Terrestrial planet formation in extra-solar planetary systems
  • S. Raymond
  • Physics, Geology
    Proceedings of the International Astronomical Union
  • 2007
Abstract Terrestrial planets form in a series of dynamical steps from the solid component of circumstellar disks. First, km-sized planetesimals form likely via a combination of sticky collisions,
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