On the formation of terrestrial planets in hot-Jupiter systems

  title={On the formation of terrestrial planets in hot-Jupiter systems},
  author={Martyn J. Fogg and R. P. Nelson},
  journal={Astronomy and Astrophysics},
  • 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,
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
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,


Oligarchic and giant impact growth of terrestrial planets in the presence of gas giant planet migration
Giant planets found orbiting close to their central stars, the so-called hot Jupiters, are thought to have originally formed in the cooler outer regions of a protoplanetary disk and then to have
The formation and habitability of terrestrial planets in the presence of close-in giant planets
Orbital Evolution and Migration of Giant Planets: Modeling Extrasolar Planets
Giant planets in circumstellar disks can migrate inward from their initial (formation) positions. Radial migration is caused by inward torques between the planet and the disk, by outward torques
A Reduced Efficiency of Terrestrial Planet Formation following Giant Planet Migration
Substantial orbital migration of massive planets may occur in most extrasolar planetary systems. Since migration is likely to occur after a significant fraction of the dust has been locked up into
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Origin and Ubiquity of Short-Period Earth-like Planets: Evidence for the Sequential Accretion Theory of Planet Formation
The formation of gas giant planets is assumed to be preceded by the emergence of solid cores in the conventional sequential accretion paradigm. This hypothesis implies that the presence of Earth-like
Survival of Terrestrial Planets in the Presence of Giant Planet Migration
The presence of "hot Jupiters," Jovian-mass planets with very short orbital periods orbiting nearby main-sequence stars, has been proposed to be primarily due to the orbital migration of planets
Oligarchic growth of giant planets
Models of giant planet formation with migration and disc evolution
We present a new model of giant planet formation that extends the core-accretion model of Pollack et al. (1996, Icarus, 124, 62) to include migration, disc evolution and gap formation. We show that
Orbital migration of the planetary companion of 51 Pegasi to its present location
THE recent discovery1 and confirmation2 of a possible planetary companion orbiting the solar-type star 51 Pegasi represent a breakthrough in the search for extrasolar planetary systems. Analysis of