Catastrophic Impacts on Gravity Dominated Asteroids

Love, S. G.; Ahrens, Thomas J.

doi:10.1006/icar.1996.0195

Cited by 171 publications

(177 citation statements)

References 8 publications

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“…The fit is a power law of slope −1.1 ± 0.3 and intercept 3.5 ± 0.7. For a 1-m projectile this fit gives Q * D ∼ 10 2.8 -10 4.2 J kg −1 , which is consistent with those found by Love and Ahrens (1996) and Benz and Asphaug (1999), for example, but disagrees with that found by Ryan and Melosh (1998).…”

Section: Critical Dispersal: Resultssupporting

confidence: 65%

“…However, although the projectile size changed by two orders of magnitude, over half of their simulations used a projectile that was <1/100 the mass of the target-small enough that changes in the projectile size may not be important. Benz and Asphaug (1999) found results similar to those of Love and Ahrens (1996) but with a more sophisticated code that included an explicit model of fracture.…”

Section: Critical Dispersal: Discussionsupporting

confidence: 53%

“…In many respects our simulations were conducted in a similar way to those of Love and Ahrens (1996). Using a 3D smoothed particle hydrocode with a Tillotson equation of state for granite without strength or fracturing, they ran several simulations at various target diameters (10-1000 km) and speeds (3, 5, and 7 km s −1 ) to find Q * D as a function of target diameter.…”

Section: Critical Dispersal: Discussionmentioning

confidence: 99%

“…The impact speed was kept constant at 2 km s −1 and the projectile size was varied to find Q * D . However, the mass ratio was consistently much more extreme than that of Love and Ahrens (1996); thus the change in the projectile size may not be as important.…”

Section: Fig 7 Critical Disruption Energy (Q *mentioning

confidence: 92%

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N-Body Simulations of Planetesimal Evolution: Effect of Varying Impactor Mass Ratio

Leinhardt¹,

Richardson

2002

Icarus

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Section: Critical Dispersal: Resultssupporting

confidence: 65%

Section: Critical Dispersal: Discussionsupporting

confidence: 53%

Section: Critical Dispersal: Discussionmentioning

confidence: 99%

Section: Fig 7 Critical Disruption Energy (Q *mentioning

confidence: 92%

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N-Body Simulations of Planetesimal Evolution: Effect of Varying Impactor Mass Ratio

Leinhardt¹,

Richardson

2002

Icarus

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“…A body 10 km across, for example, receives 50× more kinetic energy from projectiles per kg of target each year than Vesta, but its escape velocity is 50× smaller. Second, the maximum impact energy deposited per kg of target during a near-catastrophic collision will be ~100× higher for Vesta than for a 10 km body (Love and Ahrens, 1996). Because of the size distribution of projectiles in the asteroid belt, the large rare events do much more damage to an asteroid than all of the more numerous smaller cratering events.…”

Section: Origin Of Unbrecciated Eucritesmentioning

confidence: 99%

Oxygen isotopic constraints on the origin and parent bodies of eucrites, diogenites, and howardites

Scott

Greenwood

Franchi

et al. 2009

Geochimica et Cosmochimica Acta

149

177

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A few eucrites have anomalous oxygen isotopic compositions. To help understand their origin and identify additional samples, we have analyzed the oxygen isotopic compositions of 18 eucrites and four diogenites. Except for five eucrites, these meteorites have ∆ 17 O values that lie within 2σ of their mean value viz., -0.242±0.016‰, consistent with igneous isotopic homogenization of Vesta. The five exceptional eucrites-NWA 1240, Pasamonte (both clast and matrix samples), PCA 91007, A-881394, and Ibitira-have ∆ 17 O values that lie respectively 4σ, 5σ, 5σ, 15σ, and 21σ away from this mean value. NWA 1240 has a δ 18 O value that is 5σ below the mean eucrite value. Four of the five outliers are unbrecciated and unshocked basaltic eucrites, like NWA 011, the first eucrite found to have an anomalous oxygen isotopic composition. The fifth outlier, Pasamonte, is composed almost entirely of unequilibrated basaltic clasts. Published chemical data for the six eucrites with anomalous oxygen isotopic compositions (including NWA 011) exclude contamination by chondritic projectiles as a source of the oxygen anomalies. Only NWA 011 has an anomalous Fe/Mn ratio, but several anomalous eucrites have exceptional Na, Ti, or Cr concentrations. We infer that the six anomalous eucrites are probably derived from five distinct Vesta-like parent bodies (Pasamonte and PCA 91007 could come from one body). These anomalous eucrites, like many unbrecciated eucrites from Vesta, are probably deficient in brecciation and shock effects because they were sequestered in small asteroids (~10 km diameter) during the Late Heavy Bombardment following ejection from Vesta-like bodies. The preservation of Vesta's crust and the lack of deeply buried samples from the hypothesized Vestalike bodies are consistent with the removal of these bodies from the asteroid belt by gravitational perturbations from planets and protoplanets, rather than by collisonal grinding.

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Geometric characterization of the Arjuna orbital domain

Marcos

2015

Astron Nachr

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Arjuna-type orbits are characterized by being Earth-like, having both low-eccentricity and low-inclination. Objects following these trajectories experience repeated trappings in the 1:1 commensurability with the Earth and can become temporary Trojans, horseshoe librators, quasi-satellites, and even transient natural satellites. Here, we review what we know about this peculiar dynamical group and use a Monte Carlo simulation to characterize geometrically the Arjuna orbital domain, studying its visibility both from the ground and with the European Space Agency Gaia spacecraft. The visibility analysis from the ground together with the discovery circumstances of known objects are used as proxies to estimate the current size of this population. The impact cross-section of the Earth for minor bodies in this resonant group is also investigated. We find that, for ground-based observations, the solar elongation at perigee of nearly half of these objects is less than 90 • . They are best observed by space-borne telescopes, but Gaia is not going to improve significantly the current discovery rate for members of this class. Our results suggest that the size of this population may have been underestimated by current models. On the other hand, their intrinsically low encounter velocities with the Earth induce a 10-1000-fold increase in the impact cross-section with respect to what is typical for objects in the Apollo or Aten asteroid populations. We estimate that their probability of capture as transient natural satellites of our planet is about 8 %.

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Catastrophic Impacts on Gravity Dominated Asteroids

Cited by 171 publications

References 8 publications

N-Body Simulations of Planetesimal Evolution: Effect of Varying Impactor Mass Ratio

N-Body Simulations of Planetesimal Evolution: Effect of Varying Impactor Mass Ratio

Oxygen isotopic constraints on the origin and parent bodies of eucrites, diogenites, and howardites

Geometric characterization of the Arjuna orbital domain

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