Direct Measurement of the Size of 2003 UB313 from the<i>Hubble Space Telescope</i>

Brown, Michael E.; Schaller, E. L.; Roe, H. G.; Rabinowitz, D.; Trujillo, C. A.

doi:10.1086/504843

Cited by 58 publications

(47 citation statements)

References 15 publications

(27 reference statements)

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“…3. Direct measurements of a single geometry: Stellar occultations or disk-resolved images can provide an extremely precise measure of the apparent size and shape of a small body (e.g., Brown and Trujillo 2004;Brown et al 2006;Marchis et al 2006bMarchis et al , 2008aDunham et al 2011). When these direct measurements are limited to a single geometry, however, the evaluation of the diameter may be biased.…”

Section: Volume Estimatesmentioning

confidence: 99%

Density of asteroids

Carry

2012

Planetary and Space Science

517

444

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The small bodies of our solar system are the remnants of the early stages of planetary formation. A considerable amount of information regarding the processes that occurred during the accretion of the early planetesimals is still present among this population. A review of our current knowledge of the density of small bodies is presented here. Density is indeed a fundamental property for the understanding of their composition and internal structure. Intrinsic physical properties of small bodies are sought by searching for relationships between the dynamical and taxonomic classes, size, and density. Mass and volume estimates for 287 small bodies (asteroids, comets, and transneptunian objects) are collected from the literature. The accuracy and biases affecting the methods used to estimate these quantities are discussed and best-estimates are strictly selected. Bulk densities are subsequently computed and compared with meteorite density, allowing to estimate the macroporosity (i.e., amount of voids) within these bodies. Dwarf-planets apparently have no macroporosity, while smaller bodies (<400 km) can have large voids. This trend is apparently correlated with size: C and S-complex asteroids tends to have larger density with increasing diameter. The average density of each Bus-DeMeo taxonomic classes is computed (DeMeo et al., 2009, Icarus 202). S-complex asteroids are more dense on average than those in the C-complex that in turn have a larger macroporosity, although both complexes partly overlap. Within the C-complex asteroids, B-types stand out in albedo, reflectance spectra, and density, indicating a unique composition and structure. Asteroids in the Xcomplex span a wide range of densities, suggesting that many compositions are included in the complex. Comets and TNOs have high macroporosity and low density, supporting the current models of internal structures made of icy aggregates. Although the number of density estimates sky-rocketed during last decade from a handful to 287, only a third of the estimates are more precise than 20%. Several lines of investigation to refine this statistic are contemplated, including observations of multiple systems, 3-D shape modeling, and orbital analysis from Gaia astrometry.Keywords: Minor planets, Mass, Volume, Density, Porosity Small bodies as remnants of planetesimalsThe small bodies of our solar System are the left-overs of the building blocks that accreted to form the planets, some 4.6 Gyr ago. They represent the most direct witnesses of the conditions that reigned in the proto-planetary nebula (Bottke et al. 2002a). Indeed, terrestrial planets have thermally evolved and in some cases suffered erosion (e.g., plate tectonic, volcanism) erasing evidence of their primitive composition. For most small bodies, however, their small diameter limited the amount of radiogenic nuclides in their interior, and thus the amount of energy for internal heating. The evolution of small bodies is therefore mainly exogenous, through eons of collisions, external heating, and bombardm...

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Section: Volume Estimatesmentioning

confidence: 99%

Density of asteroids

Carry

2012

Planetary and Space Science

517

444

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“…Both Kuiper belt observations and numerical studies of coagulation favor a largest size of ∼1000 km. The largest object yet found in the Kuiper Belt, (136199) Eris, has a radius of 1200 ± 50 km (Brown et al 2006). In the simulations of Kenyon & Bromley (2004a), coagulation of planetesimals at 30-150 AU produces bodies as large as 1000-3000 km.…”

Section: Initial Size Distribution Of the Planetesimalsmentioning

confidence: 99%

Planetesimals in Debris Disks of Sun-Like Stars

Shannon

2011

ApJ

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Observations of dusty debris disks can be used to test theories of planetesimal coagulation. Planetesimals of sizes up to a couple of thousand kilometers are embedded in these disks and their mutual collisions generate the small dust grains that are observed. The dust luminosities, when combined with information on the dust spatial extent and the system age, can be used to infer initial masses in the planetesimal belts. Carrying out such a procedure for a sample of debris disks around Sun-like stars, we reach the following two conclusions. First, if we assume that colliding planetesimals satisfy a primordial size spectrum of the form dn/ds ∝ s −q , observed disks strongly favor a value of q between 3.5 and 4, while both current theoretical expectations and statistics of Kuiper belt objects favor a somewhat larger value. Second, number densities of planetesimals are two to three orders of magnitude higher in detected disks than in the Kuiper belt, for comparably sized objects. This is a surprise for the coagulation models. It would require a similar increase in the disk surface density over that of the Minimum Mass Solar Nebula, which is unreasonable. Both of our conclusions are driven by the need to explain the presence of bright debris disks at a few gigayears of age.

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“…Measurements from direct imaging are available for only a handful of them (Brown & Trujillo 2004;Brown et al 2006). Most recently, sizes have become available from stellar occultations (Elliot et al 2010;Sicardy et al 2011).…”

Section: Introductionmentioning

confidence: 99%

“TNOs are Cool”: A survey of the trans-Neptunian region

Santos-Sanz

Lellouch

Fornasier

et al. 2012

A&A

145

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Context. Physical characterization of trans-Neptunian objects, a primitive population of the outer solar system, may provide constraints on their formation and evolution. Aims. The goal of this work is to characterize a set of 15 scattered disk (SDOs) and detached objects, in terms of their size, albedo, and thermal properties. Methods. Thermal flux measurements obtained with the Herschel-PACS instrument at 70, 100 and 160 μm, and whenever applicable, with Spitzer-MIPS at 24 and 70 μm, are modeled with radiometric techniques, in order to derive the objects' individual size, albedo and when possible beaming factor. Error bars are obtained from a Monte-Carlo approach. We look for correlations between these and other physical and orbital parameters. Results. Diameters obtained for our sample range from 100 to 2400 km, and the geometric albedos (in V band) vary from 3.8% to 84.5%. The unweighted mean V geometric albedo for the whole sample is 11.2% (excluding Eris); 6.9% for the SDOs, and 17.0% for the detached objects (excluding Eris). We obtain new bulk densities for three binary systems: Ceto/Phorcys, Typhon/Echidna and Eris/Dysnomia. Apart from correlations clearly due to observational bias, we find significant correlations between albedo and diameter (more reflective objects being bigger), and between albedo, diameter and perihelion distance (brighter and bigger objects having larger perihelia). We discuss possible explanations for these correlations.

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Direct Measurement of the Size of 2003 UB313 from theHubble Space Telescope

Cited by 58 publications

References 15 publications

Density of asteroids

Density of asteroids

Planetesimals in Debris Disks of Sun-Like Stars

“TNOs are Cool”: A survey of the trans-Neptunian region

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