Gravitational Deformation in Shaping Asteroids and Small Satellites

Slyuta, E. N.; Воропаев, С. А.

doi:10.1006/icar.1997.5776

Cited by 15 publications

(5 citation statements)

References 30 publications

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“…The approach here is to look for equilibrium stresses directly, without necessarily introducing elastic displacement considerations. Dobrovolskis (1982) also resorted to numerical methods to solve for the constants for particular application to several satellite bodies, while Slyuta and Voropaev (1997) restricted their analysis to prolate bodies without spin, where the additional symmetry allowed them to obtain closed-form solutions. In fact, the use of a modern symbolic algebra program eliminates those practical considerations.…”

Section: Equilibrium Statesmentioning

confidence: 99%

“…The calculations are somewhat complex but straightforward and can be accomplished entirely in closed algebraic form using the symbolic algebra program MATHE-MATICA. Dobrovolskis (1982) and Slyuta and Voropaev (1997) used a similar approach to determine elastic solutions. However, they began with polynomial expressions for the displacements and then calculated the strains and then the stresses using Hooke's law, which resulted in the stress forms above.…”

Section: Equilibrium Statesmentioning

confidence: 99%

“…The difference should instead be attributed to their assumption of a spherical body, while the fluid solutions exist only for certain significantly nonspherical ellipsoidal bodies. Dobrovolskis (1982) considered the equilibrium of elastic triaxial ellipsoids with gravitational, spin, and tidal forces; Slyuta and Voropaev (1997) considered only prolate spheroids with self-gravitation. Both papers presented complete elastic stress, strain, and displacement fields.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Equilibrium Configurations of Solid Cohesionless Bodies

Holsapple¹

2001

Icarus

138

176

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Section: Equilibrium Statesmentioning

confidence: 99%

Section: Equilibrium Statesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Equilibrium Configurations of Solid Cohesionless Bodies

Holsapple¹

2001

Icarus

138

176

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“…The effect of mechanical stresses on planetesimals has previously been examined by some authors (e.g. Slyuta & Voropaev 1997;Davidsson 1999), with Brown et al (2017) recently considering the disruption of high mechanical-strength planetesimals in the context of white dwarf accretion. They show that for an asteroid with density ρ, size a0, and tensile strength S, a simple relation for the tidal disruption radius R td is given by…”

Section: Fe-rich Objectsmentioning

confidence: 99%

Cool DZ white dwarfs II: compositions and evolution of old remnant planetary systems

Hollands

Gänsicke

Koester

2018

Monthly Notices of the Royal Astronomical Society

165

155

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In a previous study, we analysed the spectra of 230 cool (T eff < 9000 K) white dwarfs exhibiting strong metal contamination, measuring abundances for Ca, Mg, Fe and in some cases Na, Cr, Ti, or Ni. Here we interpret these abundances in terms of the accretion of debris from extrasolar planetesimals, and infer parent body compositions ranging from crust-like (rich in Ca and Ti) to core-like (rich in Fe and Ni). In particular, two white dwarfs, SDSS J0823+0546 and SDSS J0741+3146, which show log[Fe/Ca] > 1.9 dex, and Fe to Ni ratios similar to the bulk Earth, have accreted by far the most core-like exoplanetesimals discovered to date. With cooling ages in the range 1-8 Gyr, these white dwarfs are among the oldest stellar remnants in the Milky Way, making it possible to probe the long-term evolution of their ancient planetary systems. From the decrease in maximum abundances as a function of cooling age, we find evidence that the arrival rate of material on to the white dwarfs decreases by 3 orders of magnitude over a ≃ 6.5 Gyr span in white dwarf cooling ages, indicating that the mass-reservoirs of post-main sequence planetary systems are depleted on a ≃ 1 Gyr e-folding time-scale. Finally, we find that two white dwarfs in our sample are members of wide binaries, and both exhibit atypically high abundances, thus providing strong evidence that distant binary companions can dynamically perturb white dwarf planetary systems.

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“…A problem with Maindl's analysis is that small asteroids of the scale they studied are not expected to be solid bodies. Only the largest asteroids are essentially solid, due to internal deformation under pressure generated by self-gravity (Slyuta and Voropaev, 1997). Eq.…”

Section: Asteroid Compositionmentioning

confidence: 99%

Habitat Bennu: Design Concepts for Spinning Habitats Constructed From Rubble Pile Near-Earth Asteroids

Miklavcic

Siu

Wright

et al. 2022

Front. Astron. Space Sci.

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The authors explore the possibility that near-earth, rubble pile asteroids might be used as habitats for human settlement by increasing their rotation to produce spin gravity. Using previously published scaling by Maindl et al. and studies of asteroid populations, it is shown that there is no class of hollowed body that would survive the spin-up process on its own without additional reinforcement. Large solid-rock asteroids (diameter D > 10 km) would not have the tensile strength to withstand the required rotation rates and would fracture and break apart. Smaller asteroids, being ‘rubble piles’, have little tensile strength and would quickly disperse. The possibility of containing the asteroid mass using higher-strength materials like carbon nanofiber is instead considered. It is found that a moderate tensile strength container can maintain the integrity of a large spinning cylinder composed of dispersed asteroid regolith. The research extends the range of possible asteroid habitat candidates, since it may become feasible to construct habitats from the more numerous smaller bodies, including NEAs (Near Earth Asteroids). The required tensile strength of the container material scales with habitat radius and thickness and is ∼ 200 MPa for a starting asteroid body of radius 300 m that is spun up to provide 0.3 g⊕ while increasing its radius to 3 km and maintaining a rubble and regolith shield thickness of 2 m to protect against cosmic rays. Ambient solar power can be harvested to aid in spin-up and material processing.

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Gravitational Deformation in Shaping Asteroids and Small Satellites

Cited by 15 publications

References 30 publications

Equilibrium Configurations of Solid Cohesionless Bodies

Equilibrium Configurations of Solid Cohesionless Bodies

Cool DZ white dwarfs II: compositions and evolution of old remnant planetary systems

Habitat Bennu: Design Concepts for Spinning Habitats Constructed From Rubble Pile Near-Earth Asteroids

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