The origin of the Kuiper Belt high-inclination population

By R. Gomes. 2003

225 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/f4e1a327e8b7d6111210d73ea5f1727347db349d

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In Astronomy and Astrophysics

Citations in the corpus

Neptune’s Migration into a Stirred-Up Kuiper Belt: A Detailed Comparison of Simulations to Observations (2005, background): “KBO sizes can also vary with inclination [Levison & Stern (2001), but see also footnote 1 of Gomes (2003)].”
The Size Distribution of Kuiper Belt Objects (2004, background): “…observations improve, the theoretical challenge is to combine collisional (this paper; Goldreich et al. 2004) and dynamical (e.g., Malhotra 1995; Gomes 2003; Hahn 2003; Levison & Morbidelli 2003; Quillen et al. 2004) calculations to derive robust predictions for the formation and evolution of…”
Resonant Trapping of Planetesimals by Planet Migration: Debris Disk Clumps and Vega’s Similarity to the Solar System (2003, background): “…does not completely describe the KBO distribution, it turns out that some of its puzzling features, such as the high inclination population of the classical KBOs (i.e., those not trapped in resonance with Neptune), can now be accounted for with more detailed models of the migration (Gomes 2003).”
Oort Cloud Formation and Dynamics (2004, background): “Harrington R. S. (1985) Implications of the observed distributions”
THE ABSOLUTE MAGNITUDE DISTRIBUTION OF KUIPER BELT OBJECTS (2014, background): “A popular dynamical model of Kuiper Belt formation is one in which most, or all KBOs formed in a region much closer to the Sun, and via a dynamical instability among the gas-giant planets, the primordial KBOs were scattered out to their current locales (Gomes 2003; Levison et al. 2008).”
EVIDENCE FOR SLOW MIGRATION OF NEPTUNE FROM THE INCLINATION DISTRIBUTION OF KUIPER BELT OBJECTS (2015, methodology): “Hahn & Malhotra (2005) were aware of the previous work of Gomes (2003) and correctly pointed out the possibility that a more successful model can be constructed from a massive disk below 30 AU.”
The primordial nucleus of comet 67P/Churyumov-Gerasimenko (2015, background): “These objects may have formed at rh ≈ 25–30 AU and then been scattered outward by Neptune because only distant bodies maintain dynamically cold orbits during the transfer (Gomes 2003).”
The Size Distribution of Trans-Neptunian Bodies (2003, background): “This is crudely consistent with scenarios in which the Excited bodies were formed at smaller heliocentric distances than the CKB (Malhotra 1993, 1995; Gomes 2003).”
Planetary migration in a planetesimal disk: why did Neptune stop at 30 AU? (2004, methodology): “Gomes (2003)showed that the origin o the so called ‘hot classical Kuiper belt’ (a population of no resonant bodies with inclinations larger than 4◦) can also be explained as a result of Neptune’s migration, which lowed a small portion of the scattered disk population be trapped on stable orbits…”
Nomenclature in the Outer Solar System (2008, background): “3 arrived there by (1) eccentricity pumping after trapping in resonances during an outward migration of Neptune (Malhotra, 1993), (2) being trapped into the 2:1 from a scattered orbit (e.g., Duncan and Levison, 1997; Gomes, 2003; Hahn and Malhotra, 2005), or (3) diffusing up to e =”
THE CANADA–FRANCE ECLIPTIC PLANE SURVEY—L3 DATA RELEASE: THE ORBITAL STRUCTURE OF THE KUIPER BELT (2009, background): “Models by Gomes (2003); Hahn & Malhotra (2005);749 Levison et al. (2008) all succeed in creating a hot population that has a similar radial extent to what is cur-750 rently observed, but have varying success in matching the inclination distribution.”
Building the terrestrial planets: Constrained accretion in the inner Solar System (2009, background): “Given that Neptune cannot easily eject these planetesimals (e.g., Duncan et al. 1987), the scattering of these small bodies also causes Uranus and Saturn to migrate outward, and Jupiter, which does eject most of the small bodies, to migrate inward (Fernandez & Ip 1984; Hahn & Malhotra 1999).”
Origin of the structure of the Kuiper belt during a dynamical instability in the orbits of Uranus and Neptune (2007, background): “4 AU), and the 3:8 MMRs (57.9 AU). The 2:5 MMR has the most prominent population. This is consistent with the observed distribution in the belt (Chiang et al., 2003). In a recent paper, Lykawka and Mukai (2007) studied the orbital distribution of objects in these resonances and pointed out that thes”