Impact Simulations with Fracture. I. Method and Tests

Benz, W.; Asphaug, Erik

doi:10.1006/icar.1994.1009

Cited by 281 publications

(292 citation statements)

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“…First-order consistency is achieved by a tensorial correction as discussed in Schäfer et al (2007). It includes self-gravity and models material strength using the full elastoplastic continuum mechanics and the Grady-Kipp fragmentation model for fracture and brittle failure (Grady & Kipp 1980;Benz & Asphaug 1994). The scenarios involve collisions of rocky basaltic objects with one lunar mass at different encounter velocities and angles α.…”

Section: Initial Conditions and Dynamical Modelmentioning

confidence: 99%

Asteroid flux towards circumprimary habitable zones in binary star systems

Bancelin

Pilat-Lohinger

Eggl

et al. 2015

A&A

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Context. So far, more than 130 extrasolar planets have been found in multiple stellar systems. Dynamical simulations show that the outcome of the planetary formation process can lead to different planetary architecture (i.e. location, size, mass, and water content) when the star system is single or double. Aims. In the late phase of planetary formation, when embryo-sized objects dominate the inner region of the system, asteroids are also present and can provide additional material for objects inside the habitable zone (HZ). In this study, we make a comparison of several binary star systems and how efficient they are at moving icy asteroids from beyond the snow line into orbits crossing the HZ. Methods. We modelled a belt of 10 000 asteroids (remnants from the late phase of the planetary formation process) beyond the snow line. The planetesimals are placed randomly around the primary star and move under the gravitational influence of the two stars and a gas giant. As the planetesimals do not interact with each other, we divided the belt into 100 subrings which were integrated separately. In this statistical study, several double star configurations with a G-type star as primary are investigated. Results. Our results show that small bodies also participate in bearing a non-negligible amount of water to the HZ. The proximity of a companion moving on an eccentric orbit increases the flux of asteroids to the HZ, which could result in a more efficient water transport on a short timescale, causing a heavy bombardment. In contrast to asteroids moving under the gravitational perturbations of one G-type star and a gas giant, we show that the presence of a companion star not only favours a faster depletion of our disk of planetesimals, but can also bring 4-5 times more water into the whole HZ.

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Section: Initial Conditions and Dynamical Modelmentioning

confidence: 99%

Asteroid flux towards circumprimary habitable zones in binary star systems

Bancelin

Pilat-Lohinger

Eggl

et al. 2015

A&A

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“…We included a model of fragmentation of porous materials (Jutzi et al 2008) in our 3D numerical hydrodynamical code based on the Smooth Particle Hydrodynamics (SPH) technique (Benz 1990;Monaghan 1992), which already contained a model of fragmentation of non-porous materials (Benz & Asphaug 1994). This new model was then tested in the laboratory by comparing with impact experiments on pumice targets (Jutzi et al 2009).…”

Section: Introductionmentioning

confidence: 99%

A large crater as a probe of the internal structure of the E-type asteroid Steins

Jutzi

Michel²,

Benz

2010

A&A

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Context. The detection of a large crater (2 km in diameter) on Steins, a diamond-shape asteroid with a diameter of only about 4.6 km, was a large surprise given the size of the asteroid itself. Steins belongs to the rare class of E-type asteroids, which had not been observed by any spacecraft before the Rosetta mission of the European Space Agency (ESA) in 2008. Aims. We demonstrate that this large crater places constraints on both the internal structure of Steins and its age based on crater counting. Methods. Numerical simulations of impacts were performed to reproduce the large crater, assuming four different initial internal structures of the asteroid: monolithic with or without microporosity, and rubble pile with or without microporosity. Results. To reproduce this crater, Steins must be either a rubble pile, which also contains microporosity, or a monolithic body with or without microporosity. The lack of porosity in meteorite analogues favors a structure without microporosity, which, according to our results, must have been monolothic. Moreover, the asteroid would be transformed into a rubble pile structure as a result of the crater formation, allowing it to be reshaped in its current shape by the YORP spin-up thermal effect. Conclusions. A combination of modeling and observations of surface features can thus serve as a probe of the internal structure of a small body and constrains its age estimate. Since the surface was totally refreshed when the large crater was formed, crater counting on Steins indicates the time that has passed since this impact event occurred.

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“…The standard gas dynamics SPH approach was extended (see for example Libersky and Petschek, 1991) to include an elastic-perfectly plastic material description and a fracture model based on the one of Grady and Kipp (1980) in order to model the behavior of brittle solids (Benz and Asphaug, 1994). As our porosity model interfaces with this material description, we begin with a short review of this previous approach.…”

Section: Model Equations and Implementationmentioning

confidence: 99%

“…resolved) level. Numerical codes, called hydrocodes (see, e.g., Benz and Asphaug, 1994) have been developed to compute the impact induced fragmentation of such solid bodies by solving the elastic-plastic conservation equations associated with a model of brittle failure to account for the fracture of the solid material. This already allowed to improve our understanding of the impact response of small bodies such as basalt-like material and asteroids belonging to the taxonomic class S, supposed to be composed of material with negligible porosity.…”

Section: Introductionmentioning

confidence: 99%

“…2.2). Our 3D Smooth Particle Hydrodynamics (SPH) code, originally developed by Benz and Asphaug (1994), includes a model of brittle failure of non-porous material and successfully reproduced impact experiments on non-porous basalt targets. Moreover, associated to the N-body code pkdgrav to account for the effect of gravity (see e.g., Richardson et al, 2000), it reproduced successfully for the first time the formation of S-type asteroid families resulting from the catastrophic disruption of non-porous parent bodies (see, e.g., Michel et al, 2001;Michel et al 2003).…”

Section: Introductionmentioning

confidence: 99%

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Numerical simulations of impacts involving porous bodies

Jutzi

Benz

Michel

2008

Icarus

130

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In this paper, we extend our Smooth Particle Hydrodynamics (SPH) impact code to include the effect of porosity at a sub-resolution scale by adapting the so-called P − alpha model. Many small bodies in the different populations of asteroids and comets are believed to contain a high degree of porosity and the determination of both their collisional evolution and the outcome of their disruption requires that the effect of porosity is taken into account in the computation of those processes. Here, we present our model and show how porosity interfaces with the elastic-perfectly plastic material description and the brittle fracture model generally used to simulate the fragmentation of non-porous rocky bodies. We investigate various compaction models and discuss their suitability to simulate the compaction of (highly) porous material. Then, we perform simple test cases where we compare results of the simulations to the theoretical solutions. We also present a Deep Impact-like simulation to show the effect of porosity on the outcome of an impact. Detailed validation tests will be presented in a next paper by comparison with high-velocity laboratory experiments on porous materials (Jutzi et al., in preparation). Once validated at small scales, our new impact code can then be used at larger scales to study impacts and collisions involving brittle solids including porosity, such as the parent bodies of C-type asteroid families or cometary materials, both in the strength-and in the gravity-dominated regime.

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Impact Simulations with Fracture. I. Method and Tests

Cited by 281 publications

References 0 publications

Asteroid flux towards circumprimary habitable zones in binary star systems

Asteroid flux towards circumprimary habitable zones in binary star systems

A large crater as a probe of the internal structure of the E-type asteroid Steins

Numerical simulations of impacts involving porous bodies

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