Planetary migration in a planetesimal disk: why did Neptune stop at 30 AU?

By R. Gomes, A. Morbidelli, Harold Levison. 2004

194 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/b36ef79e2c0dbc3b41b51132b98ea5851b6a2a59

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In Astronomy and Astrophysics

Citations in the corpus

EVIDENCE FOR SLOW MIGRATION OF NEPTUNE FROM THE INCLINATION DISTRIBUTION OF KUIPER BELT OBJECTS (2015, background): “The outer edge of the massive disk is constrained to 30 AU by Neptune’s present orbit (Gomes et al. 2004).”
Building Terrestrial Planets (2012, background): “e range of radial migration that the giant planets should have suffered after the disappearance of the disk of gas, due to their interaction with planetesimals (Malhotra 1995; Hahn and Malhotra 1999; Gomes et al. 2004, 2005), it is expected that the total mass of the cometary disk was 35-50 Earth ma”
Neptune’s Migration into a Stirred-Up Kuiper Belt: A Detailed Comparison of Simulations to Observations (2005, methodology): “This has been recognized in previous studies (Malhotra 1995; Gomes 1997), but has not been quantified.”
Building the terrestrial planets: Constrained accretion in the inner Solar System (2009, background): “planetesimal disk or closer proximity between Neptune and the disk’s inner edge (Gomes et al., 2004; Gomes et al., 2005).”
Constructing the secular architecture of the solar system II: The terrestrial planets (2009, unknown): “A similar result can be found in Gomes et al. (2004).”
The primordial excitation and clearing of the asteroid belt—Revisited (2006, methodology): “This scenario has been subsequently explored in more detail by a number of researchers, aided in a large part by vast increases in computer speed (e.g., Hahn and Malhotra, 1999; Gomes et al., 2004).”
THE CANADA–FRANCE ECLIPTIC PLANE SURVEY—L3 DATA RELEASE: THE ORBITAL STRUCTURE OF THE KUIPER BELT (2009, background): “…population728 around 45 AU may be explained by the global evolution of solid matter in turbulent protoplanetary disks729 (Stepinski & Valageas 1996, 1997), although an even-more extreme density contrast may be needed at730 ∼30 AU to prevent Neptune’s continued migration outward (Gomes et al. 2004).”
Dynamics of the Giant Planets of the Solar System in the Gaseous Protoplanetary Disk and Their Relationship to the Current Orbital Architecture (2007, background): “More work is needed in order to quantify the statistical outcome of the chaotic evolution of the planets and, particularly, to prove that the onset of the planetary instability can occur late, as in Gomes et al. (2005). This will be the object of a forthcoming paper.”
Origin and Evolution of Short-period Comets (2017, methodology): “We did not account for the disk above 30 au, because constraints from Neptune migration (Gomes et al. 2004) and the population of CCs show that the extension of the planetesimal disk above 30 au was not very massive (relative to the disk below 30 au).”
The primordial nucleus of comet 67P/Churyumov-Gerasimenko (2015, background): “An exterior primordial disk stretched from ∼15 AU to ∼30 AU (Gomes et al. 2004), possibly with a much thinner part reaching to ∼45 AU (Parker & Kavelaars 2010; Parker et al. 2011).”
Origin of the structure of the Kuiper belt during a dynamical instability in the orbits of Uranus and Neptune (2007, background): “This idea also has the advantage of explaining why Neptune stopped migrating at 30 AU — it hit the edge of the disk (Gomes et al. 2004).”
THE FORMATION MECHANISM OF GAS GIANTS ON WIDE ORBITS (2009, unknown): “Hahn & Malhotra (1999), followed by Gomes et al. (2004) and Tsiganis et al. (2005), found that a 30−50M⊕ planetesimal disk could expand Neptune’s orbit from 23 AU to 30 AU.”