Ejecta formation and crater development of the Mjølnir impact

Шувалов, В. В.; Dypvik, Henning

doi:10.1111/j.1945-5100.2004.tb00105.x

Cited by 53 publications

(34 citation statements)

References 22 publications

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“…SOVA is a two-step Eulerian code that can model multidimensional, multimaterial, large deformation, strong shock wave physics. It includes a general treatment of viscosity for modeling viscous flow with Newtonian or Bingham rheology, while the implementation of the Rigid-Plastic Model (RPM; Dienes and Walsh 1970;Shuvalov and Dypvik 2004) allows us to mimic plastic behavior of the projectile. In addition, SOVA can describe the motion of solid/melt particles in an evolving ejecta-gas-vapor plume and their momentum-energy exchange using two-phase hydrodynamics, which takes into account both individual particle characteristics (mass, density, shape) and their collective behavior (momentum and energy exchange with surrounding gas).…”

Section: Full-scale Hydrodynamic Model (Sova)mentioning

confidence: 99%

The Canyon Diablo impact event: Projectile motion through the atmosphere

Artemieva

Pierazzo

2009

Meteorit & Planetary Scien

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Abstract-Meteor Crater is one of the first impact structures systematically studied on Earth. Its location in arid northern Arizona has been ideal for the preservation of the structure and the surviving meteoric material. The recovery of a large amount of meteoritic material in and around the crater has allowed a rough reconstruction of the impact event: an iron object 50 m in diameter impacted the Earth's surface after breaking up in the atmosphere. The details of the disruption, however, are still debated. The final crater morphology (deep, bowl-shaped crater) rules out the formation of the crater by an open or dispersed swarm of fragments, in which the ratio of swarm radius to initial projectile radius C d is larger than 3 (the final crater results from the sum of the craters formed by individual fragments). On the other hand, the lack of significant impact melt in the crater has been used to suggest that the impactor was slowed down to 12 km/s by the atmosphere, implying significant fragmentation and fragments' separation up to 4 initial radii. This paper focuses on the problem of entry and motion through the atmosphere for a possible Canyon Diablo impactor as a first but necessary step for constraining the initial conditions of the impact event which created Meteor Crater.After evaluating typical models used to investigate meteoroid disruption, such as the pancake and separated fragment models, we have carried out a series of hydrodynamic simulations using the 3D code SOVA to model the impactor flight through the atmosphere, both as a continuum object and a disrupted swarm.Our results indicate that the most probable pre-atmospheric mass of the Meteor Crater projectile was in the range of 4⋅10 8 to 1.2⋅10 9 kg (equivalent to a sphere 46-66 m in diameter). During the entry process the projectile lost probably 30% to 70% of its mass, mainly because of mechanical ablation and gross fragmentation. Even in the case of a tight swarm of particles (C d <3), small fragments can separate from the crater-forming swarm and land on the plains (tens of km away from the crater) as individual meteorites. Starting from an impactor pre-atmospheric velocity of ~18 km/s, which represents an average value for Earth-crossing asteroids, we find that after disruption, the most probable impact velocity at the Earth's surface for a tight swarm is around 15 km/s or higher. A highly dispersed swarm would result in a much stronger deceleration of the fragments but would produce a final crater much shallower than observed at Meteor Crater.

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Section: Full-scale Hydrodynamic Model (Sova)mentioning

confidence: 99%

The Canyon Diablo impact event: Projectile motion through the atmosphere

Artemieva

Pierazzo

2009

Meteorit & Planetary Scien

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“…Whether this asymmetric collapse was a 276 consequence of oblique impact, lateral asymmetry in crustal strength, or random instabilities 277 during crater modification remains an open question. Numerical models of oblique impact 278 suggest that central uplifts do rise with a downrange velocity component (e.g., Ivanov and 279 Artemieva, 2002;Shuvalov and Dypvik, 2004) as suggested by Schultz and d'Hondt (1996). 280 This is supported by geological field evidence for preferred transport direction in central uplifts 281 at eroded terrestrial craters (Scherler et al, 2006;Kenkmann and Poelchau, 2009).…”

Section: Introduction 26mentioning

confidence: 96%

Mantle deformation beneath the Chicxulub impact crater

Christeson

Collins

Morgan

et al. 2009

Earth and Planetary Science Letters

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9 The surface expression of impact craters is well-known from visual images of the Moon, 10Venus, and other planets and planetary bodies, but constraints on deep structure of these 11 craters is largely limited to interpretations of gravity data. Although the gravity models are 12 non-unique, they do suggest that large impact craters are associated with structure at the 13 base of the crust. We use seismic data to map Moho (crust-mantle interface) topography 14 beneath the Chicxulub crater, the youngest and best preserved of the three largest known 15

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“…Systematic high-resolution modelling of oblique impacts was first described in Melosh (1999, 2000a,b). Since that work, advances in computer hardware have allowed more widespread simulation of oblique impacts Shuvalov et al, 2002;Artemieva and Ivanov, 2004;Gisler et al, 2004;Shuvalov and Dypvik, 2004;Elbeshausen et al, 2009).…”

Section: Introductionmentioning

confidence: 99%

Numerical Modelling of Impact Processes

Collins¹,

Wünnemann²,

Artemieva³

et al. 2012

Impact Cratering

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Numerical modelling is now a well-established and important component of impact research. When used to complement small-scale impact experiments, it provides a powerful tool for exposing the physical processes in a cratering event and for investigating the effect of individual physical parameters that are not otherwise under the experimenter's control. Moreover, once adequately validated against small-scale laboratory experiments, numerical models allow us to simulate impacts much larger and more energetic than those that can be studied experimentally.The first numerical impact simulation was published in 1961 by R.L. Bjork (Fig. 17.1). That calculation of the Meteor Crater impact simulated only the first 60 ms of the collision and did not account for gravity or the strength of the target rocks (Bjork, 1961). Nevertheless, that simulation, and those that followed in the next decades, provided great insight into the physics of hypervelocity impact, including the formation and attenuation of the detached shock wave, the fate of the impactor, and the scaling of crater dimensions (e.g. Ahrens and O'Keefe, 1977;Orphal, 1977;O'Keefe and Ahrens, 1993).Nearly half a century on, and thanks to advances in numerical impact models and much improved computational resources, numerical models that include gravity and complex material models are used routinely to simulate large terrestrial impacts, aiding interpretation of geological and geophysical observations and quantifying the energy of the impact and impact-related consequences. For example, several numerical impact models of the Chicxulub impact have been performed and compared with observational data to constrain the impact energy, the fate of the projectile, the volume of climate forcing gases released into the atmosphere, the transport and re-entry of ejected material and the regional seismicity (e.g.

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Ejecta formation and crater development of the Mjølnir impact

Cited by 53 publications

References 22 publications

The Canyon Diablo impact event: Projectile motion through the atmosphere

The Canyon Diablo impact event: Projectile motion through the atmosphere

Mantle deformation beneath the Chicxulub impact crater

Numerical Modelling of Impact Processes

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