Rock fluidization during peak-ring formation of large impact structures

  title={Rock fluidization during peak-ring formation of large impact structures},
  author={Ulrich Riller and Michael H. Poelchau and Auriol S. P. Rae and Felix M. Schulte and Gareth S. Collins and H. Jay Melosh and Richard A. F. Grieve and Joanna V. Morgan and Sean P. S. Gulick and Johanna Lofi and Abdou Karim Diagne Diaw and Naoma McCall and David A. Kring and IODP–IC DP Expedition 364 Science Party},
Large meteorite impact structures on the terrestrial bodies of the Solar System contain pronounced topographic rings, which emerged from uplifted target (crustal) rocks within minutes of impact. To flow rapidly over large distances, these target rocks must have weakened drastically, but they subsequently regained sufficient strength to build and sustain topographic rings. The mechanisms of rock deformation that accomplish such extreme change in mechanical behaviour during cratering are largely… 

Ocean resurge-induced impact melt dynamics on the peak-ring of the Chicxulub impact structure, Mexico

Core from Hole M0077 from IODP/ICDP Expedition 364 provides unprecedented evidence for the physical processes in effect during the interaction of impact melt with rock-debris-laden seawater,

Stress‐Strain Evolution During Peak‐Ring Formation: A Case Study of the Chicxulub Impact Structure

Deformation is a ubiquitous process that occurs to rocks during impact cratering; thus, quantifying the deformation of those rocks can provide first‐order constraints on the process of impact

Explosive interaction of impact melt and seawater following the Chicxulub impact event

The impact of asteroids and comets with planetary surfaces is one of the most catastrophic, yet ubiquitous, geological processes in the solar system. The Chicxulub impact event, which has been

Seismic attribute analysis of Chicxulub impact crater

Chicxulub crater formed ~ 66 Ma ago by an asteroid impact on the Yucatan platform in the southern Gulf of Mexico. The crater has a ~ 200 km rim diameter and has been covered by carbonate sediments up

The first day of the Cenozoic

High-resolution section from the Chicxulub peak ring provides insight into the impact environmental effects, including charcoal as evidence for impact-induced wildfires and a paucity of sulfur-rich evaporites from the target supporting rapid global cooling and darkness as extinction mechanisms.

Central uplift collapse in acoustically fluidized granular targets: Insights from analog modeling

Depending on their sizes, impact craters have either simple or complex geometries. Peak‐ring craters such as the Chicxulub impact structure possess a single interior ring of peaks and hills and a

Petrophysics of Chicxulub Impact Crater's Peak Ring

A new set of physical property measurements was undertaken on 29 peak‐ring samples from the IODP‐ICDP Expedition 364. Among the studied lithologies, the dominant one recovered in the peak ring

Impact‐Induced Porosity and Microfracturing at the Chicxulub Impact Structure

Porosity and its distribution in impact craters has an important effect on the petrophysical properties of impactites: seismic wave speeds and reflectivity, rock permeability, strength, and density.

Tracing shock-wave propagation in the Chicxulub crater: Implications for the formation of peak rings

The Chicxulub crater (Yucatán Peninsula, Mexico) is considered exceptional in many scientific aspects; morphologically it is the only known impact structure on Earth with a well-preserved peak



The formation of peak rings in large impact craters

Rock samples from IODP/ICDP Expedition 364 support the dynamic collapse model for the formation of the Chicxulub crater and have implications for far-ranging subjects, from how giant impacts alter the climate on Earth to the morphology of crater-dominated planetary surfaces.

Folding within seconds

Hypervelocity impacts of cosmic projectiles larger than ∼200 m diameter are capable of forming complex craters on Earth. At these craters, shock loading, shock damage, and excavation flow are

Full waveform tomographic images of the peak ring at the Chicxulub impact crater

Peak rings are a feature of large impact craters on the terrestrial planets and are generally believed to be formed from deeply buried rocks that are uplifted during crater formation. The precise

Complex crater formation: Insights from combining observations of shock pressure distribution with numerical models at the West Clearwater Lake impact structure

Large impact structures have complex morphologies, with zones of structural uplift that can be expressed topographically as central peaks and/or peak rings internal to the crater rim. The formation

Lunar impact basins revealed by Gravity Recovery and Interior Laboratory measurements

Observations from the GRAIL mission indicate a marked change in the gravitational signature of lunar impact structures at the morphological transition, with increasing diameter, from complex craters to peak-ring basins, and a correlation between the diameter of the central Bouguer gravity high and the outer topographic ring diameter enables the identification and characterization of well-preserved basins.

Numerical simulations of impact crater formation with dilatancy

Impact‐induced fracturing creates porosity that is responsible for many aspects of the geophysical signature of an impact crater. This paper describes a simple model of dilatancy—the creation of

Hydrocode simulations of Chicxulub crater collapse and peak-ring formation

We use hydrocode modeling to investigate dynamic models for the collapse of the Chicxulub impact crater. Our aim is to integrate the results from numerical simulations with kinematic models derived