The Inclination Distribution of the Kuiper Belt

By M. Brown. 2001

280 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/0e30cfae1626932a2801d1dfa5413967282d35a6

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Citations in the corpus

Scenarios for the Origin of the Orbits of the Trans-Neptunian Objects 2000 CR105 and 2003 VB12 (Sedna) (2004, background): “More recently, Brunini&Melita (2002) proposed that a planet on a moderate-eccentricity orbit with a 60 AU could explain the putative edge of the Kuiper belt at 50 AU (Allen et al. 2002; Trujillo & Brown 2001).”
THE ABSOLUTE MAGNITUDE DISTRIBUTION OF KUIPER BELT OBJECTS (2014, methodology): “We adopt the hot population inclination distribution discussed above and determine the latitude distribution with the same technique as Brown (2001).”
The origin of the Kuiper Belt high-inclination population (2003, methodology): “2 randomly chosen subsets of the final complete sets from the cold population in order to match the results for the proportion of objects in each population estimated by Brown (2001).”
EXOPLANETARY SPIN–ORBIT ALIGNMENT: RESULTS FROM THE ENSEMBLE OF ROSSITER–MCLAUGHLIN OBSERVATIONS (2009, background): “Brown (2001) has found that a sum of two Fisher-like distributions is needed to fit the inclination distribution of Kuiper belt objects, and this multi-component model has been a very useful constraint on dynamical theories.”
EVIDENCE FOR SLOW MIGRATION OF NEPTUNE FROM THE INCLINATION DISTRIBUTION OF KUIPER BELT OBJECTS (2015, background): “The inclination distribution of various populations in the Kuiper Belt can be represented by =N i di( ) s-i i disin exp( 2 )i2 2 , where si is a parameter (Brown 2001).”
THE CANADA–FRANCE ECLIPTIC PLANE SURVEY—L3 DATA RELEASE: THE ORBITAL STRUCTURE OF THE KUIPER BELT (2009, methodology): “We did not347 test this functional form as this introduces an extra parameter, which is not demanded by the current sample.348 The Brown (2001) functional form may not be an exact representation of every sub-component’s inclination349 distributions; we can, however, obtain an acceptable match to…”
The Deep Ecliptic Survey: A Search for Kuiper Belt Objects and Centaurs. II. Dynamical Classification, the Kuiper Belt Plane, and the Core Population (2005, background): “First, Brown (2001) did not remove those KBOs observed only over a few days interval, which can have large inclination errors (see Table 3) and potentially bias the results by contaminating the sample with too many high-inclination objects.”
Kuiper Belt Objects: Relics from the Accretion Disk of the Sun (2002, background): “Trujillo & Brown (2001) narrowed the location of the edge to 47 ± 1 AU, assuming a differential size distribution with power law index q = 4 and geometric albedo 0.04.”
Properties of the Trans-Neptunian Belt: Statistics from the Canada-France-Hawaii Telescope Survey (2001, methodology): “We also tested the best-fit model presented by Brown (2001), consisting of two Gaussians multiplied by sin(i), [a exp( −i2 2σ21 ) + (1− a) exp(−i 2 2σ22 )] sin i, (7) where a = 0.93, σ1 = 2.2 ◦, and σ2 = 18 ◦, and found it equally compatible with our single Gaussian model (Equation 6).”
Origin of the structure of the Kuiper belt during a dynamical instability in the orbits of Uranus and Neptune (2007, methodology): “In order to perform a quantitative comparison between the model and the observed eccentricity distributions in the classical belt, we have implemented a bias calculator algorithm inspired by the work of Trujillo & Brown (2001). This method takes as input: 1) orbital element distribution from a model”
A Correlation between Inclination and Color in the Classical Kuiper Belt (2002, result): “Such a model is compatible with two recently reported dynamical groupings: (1) the Levison and Stern (2001) large and small size components of the Classical KBOs and (2) the Brown (2001) high-i and low-i components of the Classical KBOs.”
The Scattered Disk as the Source of the Jupiter Family Comets (2008, methodology): “This procedure is not ideal because it only uses a subset of the observed population (28 of 80 objects, in this case) to determine the distribution, and has unquantified biases for objects with large eccentricities as noted by Brown (2001).”
Neptune’s Migration into a Stirred-Up Kuiper Belt: A Detailed Comparison of Simulations to Observations (2005, background): “Since the Kuiper Belt subtends a total solid angle of ∆Ωtotal ≃ 8100 deg2 (Brown 2001), the total number of KBOs larger than R50 is N50 = Σ(R > R50)∆Ωtotal ≃ 1.1× 105 having a total mass of Mtotal ≃ 0.05 M⊕.”
The planet nine hypothesis (2019, background): “The broader class of classical KBOs is often divided into dynamically ‘cold’ and ‘hot’ sub-populations, where the distinction is based on their orbital inclinations, which show a bimodal distribution (Brown, 2001).”
Planetary migration in a planetesimal disk: why did Neptune stop at 30 AU? (2004, background): “, 1996; Chiang and Brown, 199 Trujillo et al., 2001; Gladman et al., 2001) , is now less than 0.1M⊕. Could the Kuiper belt loose most of its mass witho substantially modifying Neptune’s final location? Two general mechanisms have been proposed for mass depletion of the Kuiper belt: (1) the dynamical”
Nomenclature in the Outer Solar System (2008, background): “, 2001; Brown, 2001), an additional “cold” population does seem to be required, but strangely only in the a = 42–45AU region (see chapter by Kavelaars et al.); this cold component does not seem to be present in the inner or outer classical belt, or any of the resonant populations. Elliot et al. (200”
The Dynamics of Known Centaurs (2002, methodology): “A future detailed analysis of observational biases could test how the time-weighted distribution compares with models of inclination- 8 dependent detection bias, such as one proposed by Brown (2001).”