Asteroid Density, Porosity, and Structure

By D. Britt, D. Yeomans, K. Housen, G. Consolmagno. 2002

427 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/0a2baae5e0f7d86099cf7e3cda776e4feb8ec48a

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

Citations in the corpus

Meteoritic parent bodies: Their number and identification (2002, background): “They are divided into two groups (EH and EL) and exhibit a range of metamorphic types (3–6). These meteorites have no distinctive absorption features from 0.3 to 2.5 μm because of the absence of Fe2+ in their silicates. M asteroids have moderate visual albedos (~0.10 to ~0.30), relatively featureles”
The global effects of impact-induced seismic activity on fractured asteroid surface morphology (2005, background): “Arnold is given credit for first suggesting that the downslope movement of regolith could be an important surface process on asteroids, despite the tiny surface gravitational fields on these small bodies (Chapman, 1978). In the same year, Cintala et al. (1978) published two of the primary reasons wh”
THE IMPORTANCE OF SECONDARY CRATERING TO AGE CONSTRAINTS ON PLANETARY SURFACES (2006, background): “There may not be a standard penetration depth for a given-sized primary projectile, as there appears to be a range of densities for different asteroid types (e.g., Britt et al. 2002), and although thought to be low (less than 1 g cm−3), comet densities are not well known.”
Bias-corrected population, size distribution, and impact hazard for the near-Earth objects (2004, methodology): “However, for C-type and S-type teroids, there does appear to be a fairly consistent t (Britt et al., 2002).”
Density of asteroids (2012, background): “As already discussed else-where, however, when a reliable mass estimate is available ( i.e. , usually from the presence of a satellite), the precision on the volume generally limits the accuracy on the density (Merline et al., 2002; Britt et al., 2002; Consolmagno et al., 2008).”
The fossilized size distribution of the main asteroid belt (2003, background): “8 g cm−3 for ordinary chondrites) (Britt et al., 2002).”
Asteroid Catalog Using AKARI: AKARI/IRC Mid-Infrared Asteroid Survey (2011, methodology): “In some cases, by combining the size and the mass, which are precisely measured using modern techniques (Hilton 2002), the bulk density of the asteroid can be estimated (Britt et al. 2002).”
Scaling forces to asteroid surfaces: The role of cohesion (2010, background): “Porosity values have been correlated with asteroid spectral type (Britt et al., 2002), with typical porosities ranging from 30% for S-type asteroids up to 50% and higher for C-type asteroids.”
Hydrated Minerals on Asteroids: The Astronomical Record (2003, background): “This topic is covered in more detail in Britt et al. (2002).”
The taxonomic distribution of asteroids from multi-filter all-sky photometric surveys (2013, methodology): “The density is the least wellconstrained value used in this work because these measurements are extremely difficult to obtain (see discussion in Britt et al. 2002, 2006, Carry 2012).”
Asteroids Were Born Big (2009, methodology): “obtained from the above SFD, where the largest asteroids have known masses (Britt et al., 2002), and from an analysis of the mo-”
In search of the source of asteroid (101955) Bennu: Applications of the stochastic YORP model (2015, background): “The biggest factor, however, is the bulk density used in Vokrouhlický et al. (2006a) was 2.5 g cm 3, a high value for a C-type asteroid (i.e., Mathilde and Bennu have bulk densities of 1.3 g cm 3, respectively; Britt et al., 2002; Chesley et al., 2014).”
Linking the collisional history of the main asteroid belt to its dynamical excitation and depletion (2005, background): “…above, different population sizes, with many large families located in the outer main belt, and/or different asteroidal physical properties, with the inner main belt dominated by S-type asteroids and the outer main belt by primitive C/D-type bodies (Gradie and Tedesco, 1982; Britt et al., 2002).”
A strain-based porosity model for use in hydrocode simulations of impacts and implications for transient crater growth in porous targets (2006, background): “, 1977; Watson, 1978), and recent measurements of their bulk density have revealed that the porosity might be in some cases as high as 75–80% (Britt et al., 2002; Sirono and Greenberg, 2000).”