Planet formation and migration

By J. Papaloizou, C. Terquem. 2005

163 citations recorded by the source corpus.

We review the observations of extrasolar planets, ongoing developments in theories of planet formation, orbital migration and the evolution of multiplanet systems.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/798f0238791bdd79d5a0ca763b8a8888fa4ab696

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In Astronomy and Astrophysics

1. D. Lin
2. Shigeru Ida
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4. Gordon I. Ogilvie
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Citations in the corpus

• The faint young Sun problem (2012, background): “Using the presentday solar constant S0 ≃ 1361 W m −2 [Kopp and Lean, 2011] and Earth’s current albedo A ≃ 0.3 yields values of ∆F ≈ 60 W m−2 and ∆F ≈ 40 W m−2 at times 3.8 Ga and 2.5 Ga, respectively.”
• Concentrating small particles in protoplanetary disks through the streaming instability (2016, background): “The course of planet formation is usually divided into different stages according to the size of the solids or planetary objects involved, and each stage has its own major difficulties (e.g., Papaloizou & Terquem 2006; Baruteau et al. 2014; Testi et al. 2014).”
• Toward a Deterministic Model of Planetary Formation. IV. Effects of Type I Migration (2008, methodology): “Many simulations have been carried out (see, e.g., Papaloizou & Terquem 2006) with different numerical methods and resolutions, protoplanetary potentials and orbits, and disk structures.”
• Migration and the Formation of Systems of Hot Super-Earths and Neptunes (2006, background): “…of close orbiting giant planets, the so–called ’hot Jupiters’ and ’hot Neptunes’, has been taken as an indication of the operation of large scale migration induced by the interaction of recently formed protoplanets with protoplanetary disks (e.g., Papaloizou & Terquem 2006 and references therein).”
• The coronal X-ray - age relation and its implications for the evaporation of exoplanets (2011, background): “This has provoked much work to investigate where and how these hot Jupiters form and how tey might migrate to their current positions (see Papaloizou & Terquem 2006 for a review).”
• On the tidal evolution of Hot Jupiters on inclined orbits (2009, background): “In both of the giant planet formation scenarios (see Papaloizou & Terquem 2006 for a comprehensive review), core accretion and gravitational instability, it is difficult to produce HJs in situ.”
• Prospects for the Characterization and Confirmation of Transiting Exoplanets via the Rossiter-McLaughlin Effect (2006, background): “There is a large literature on this subject (as reviewed by Papaloizou & Terquem 2006), but broadly speaking, there is no apparent reason why these mechanisms would perturb spin-orbit alignment; in fact, they may even drive the system toward closer alignment.”