Daniel D. Durda (Southwest Research Institute)

Slides:



Advertisements
Similar presentations
Proto-Planetary Disk and Planetary Formation
Advertisements

Diffusion (continued)
CLASTIC TRANSPORT AND FLUID FLOW
Granular Jets Alexander BarnaveliGeorgia If a steel ball is dropped onto a bed of dry sand, a "splash" will be observed that may be followed by the ejection.
Origins of Regular and Irregular Satellites ASTR5830 March 21, :30-1:45 pm.
The scaling of LWFA in the ultra-relativistic blowout regime: Generation of Gev to TeV monoenergetic electron beams W.Lu, M.Tzoufras, F.S.Tsung, C. Joshi,
Griffith Cracks Flaws Make the World Beautiful! Were it not for the flaws, rocks and mountains would have been perfectly boring.
Simple Harmonic Motion
Distribution of Microcracks in Rocks Uniform As in igneous rocks where microcrack density is not related to local structures but rather to a pervasive.
 The strength of dispersion forces between molecules can affect physical properties of the substances they make up.  In other words… the amount of energy.
Asteroid Rotations and Binaries
Catastrophic Disruption of Meteorites: Implications for Asteroids and Interplanetary Dust G. J. Flynn and T. VanVeghten SUNY - Plattsburgh D. D. Durda.
15. Physics of Sediment Transport William Wilcock (based in part on lectures by Jeff Parsons) OCEAN/ESS
Quantum Mechanics 101 Waves? or Particles? Interference of Waves and the Double Slit Experiment  Waves spreading out from two points, such as waves.
Lecture 11: Growth of Cloud Droplet in Warm Clouds
Observations and models of size distribution of KBOs (summarize several articles) Yeh, Lun-Wen
Higher Order Multipole Transition Effects in the Coulomb Dissociation Reactions of Halo Nuclei Dr. Rajesh Kharab Department of Physics, Kurukshetra University,
Modeling Impacts on Icy Bodies: Applications to Saturn’s Moons Vanessa Lauburg TERPS Conference: December 7, 2004 Tethys Mimas Rhea.
« Debris » discs A crash course in numerical methods Philippe Thébault Paris Observatory/Stockholm Observatory.
Spectra of Gravity Wave Turbulence in a Laboratory Flume S Lukaschuk 1, P Denissenko 1, S Nazarenko 2 1 Fluid Dynamics Laboratory, University of Hull 2.
Measurement of Kinematics Viscosity Purpose Design of the Experiment Measurement Systems Measurement Procedures Uncertainty Analysis – Density – Viscosity.
Physics of fusion power Lecture 7: particle motion.
Trends in characteristics of small NEA and MBA binaries Petr Pravec Astronomical Institute AS CR, Czech Republic Workshop on Binaries in the Solar System.
Vibrations and Waves Chapter 12.
Mechanical Properties
Spins and Satellites: Probes of Asteroid Interiors Alan W. Harris and Petr Pravec Sixth Catastrophic Disruption Workshop Cannes, 9-11 June 2003.
Timothy Reeves: Presenter Marisa Orr, Sherrill Biggers Evaluation of the Holistic Method to Size a 3-D Wheel/Soil Model.
Brookhaven Science Associates U.S. Department of Energy MUTAC Review April , 2004, LBNL Target Simulation Roman Samulyak, in collaboration with.
Cratering on Nix and Hydra William Bottke (SwRI).
Robustness of complex networks with the local protection strategy against cascading failures Jianwei Wang Adviser: Frank,Yeong-Sung Lin Present by Wayne.
Week 4 Fracture, Toughness, Fatigue, and Creep
Accelerating Precursory Activity in Statistical Fractal Automata Dion Weatherley and Peter Mora QUAKES, Univ. of Qld., Australia.
Internal Wave Interactions with Time-Dependent Critical Levels Brian Casaday and J. C. Vanderhoff Department of Mechanical Engineering Brigham Young University,
David Nesvorny (Southwest Research Institute) David Nesvorny (Southwest Research Institute) Capture of Irregular Satellites during Planetary Encounters.
Alice Quillen University of Rochester Department of Physics and Astronomy Oct, 2005 Submillimet er imaging by Greaves and collaborato rs.
The PSI Planet-building Code: Multi-zone, Multi-use S. J. Weidenschilling PSI Retreat August 20, 2007.
15. Physics of Sediment Transport William Wilcock (based in part on lectures by Jeff Parsons) OCEAN/ESS 410.
WHY DO WE WANT TO MODEL THE COLLISIONAL EVOLUTION OF MBPs? SOLAR SYSTEM FORMATION : what was the primordial distribution of the minor body population.
Evolution of clusters M. Arnaud CEA - service d’astrophysique Saclay Assuming favored cosmology  =0.3  =0.7.
Are transition discs much commoner in M stars? Recent claim that 50% of discs around M stars are in transition (Sicilia-Aguilar et al 2008) CAREFUL! For.
EQUILIBRIUM BEACH PROFILE Conceptually the result of balancing constructive and destructive forces. Really a misnomer because equilibrium never reached.
Week 4 Fracture, Toughness, Fatigue, and Creep
Lawrence Berkeley National Laboratory Earth Sciences Division 1 Cyclotron Road, MS Berkeley, CA D modeling of fault reactivation.
Materials Science Metals and alloys.
U NIVERSITY OF S CIENCE AND T ECHNOLOGY OF C HINA Influence of ion orbit width on threshold of neoclassical tearing modes Huishan Cai 1, Ding Li 2, Jintao.
Cassini UVIS Observations and the History of Saturn’s Rings Larry W. Esposito, Joshua E. Colwell, Glen R. Stewart LASP, University of Colorado 24 August.
Gravity Wave Turbulence in Wave Tanks S Lukaschuk 1, S Nazarenko 2 1 Fluid Dynamics Laboratory, University of Hull 2 Mathematics Institute, University.
Simple Harmonic and non harmonic Motion
Asteroids.
Craters on Comets J.-B. Vincent, N. Oklay, S. Marchi, S. Höfner, H. Sierks 33 (6 outlines) -> 27.
Capture of Irregular Satellites during Planetary Encounters
Theoretical Particle Physics Group (TPP)
Computational Prediction of Mechanical Performance of Particulate-Reinforced Al Metal-Matrix Composites (MMCs) using a XFEM Approach Emily A. Gerstein.
Hypervelocity Impact Measurements and Simulations
Daniel D. Durda, William F. Bottke, and Brian L. Enke
Diffusion how atoms move in solids
Poisons Ratio Poisons ratio = . w0 w Usually poisons ratio ranges from
6th Grade Change Over Time
Faculty of Engineering and Physical Sciences
OCEAN/ESS Physics of Sediment Transport William Wilcock (based in part on lectures by Jeff Parsons)
Describe Gravity in terms of force, mass, and distance
The spectral evolution of impulsive solar X-ray flares
The Formation of Planetesimals – the Laboratory Perspective
Regolith Growth and Darkening of Saturn’s Ring Particles
Presentation: Natural disasters
Lab8: Fatigue Testing Machine
Lab8: Fatigue Testing Machine
Althea V. Moorhead, University of Michigan
Shipping Support Post Analysis
Electric Force Unit 11.2.
Presentation transcript:

Daniel D. Durda (Southwest Research Institute) Discontinuities in Size-Strength Scaling Laws: Another Source of Wavy Size Distributions Daniel D. Durda (Southwest Research Institute)

Previously Identified Sources of Waves Fig. 8 from Durda and Dermott (1997) Small-size cutoff in the particle population: At small sizes, a particle cutoff may result from the rapid removal of bodies by non-gravitational forces such as Poynting-Robertson drag or the Yarkovsky effect.

Previously Identified Sources of Waves Fig. 4a from Durda et al. (1998) Distinct change in slope in a size-strength scaling law: Results from the transition from strength-scaling for small bodies to gravity-scaling for larger objects.

Discontinuous Scaling Laws Discontinuities in the size-strength scaling law, as might occur at small sizes when particles are no longer homogeneous over the scale of fragmentation, can also induce significant waves in evolved size distributions. Much attention has been focused on determining how Q*D varies with size for objects larger than the ~10-cm size targets typically studied in laboratory impact experiments. At size scales small enough that material inhomogeneities due to the presence of chondrules or Ni-Fe metal blebs or the effects of mineral grain boundaries become important, impact strengths may be dictated by the failure of internal flaws with a narrow range of critical tensile strengths. Q*D may still depend on size, but may change discontinuously at specific sizes and/or have a different size dependence in different size ranges.

Discontinuous Scaling Laws

Collisional Model Results The four hypothetical scaling laws were used within a numerical collision model to determine catastrophic disruption lifetimes and resulting evolved size distributions. Initial populations with a D = 200 km largest body and a power-law slope index of p = 2.7 (the number of bodies larger than D is proportional to D-p; for scaling laws with size-independent Q*D, equilibrium size distributions have p = 2.5) were followed through 4.5 Gyr of collisional evolution.

Collisional Model Results Scaling Law H2 An abrupt change in the slope of the log Q*D vs. log D relation (in this case from a strength-scaling-like D-0.4 size dependence to an energy-scaling, size-independent strength at smaller sizes) induces minor perturbations to the evolved size distribution. The equilibrium power-law slope index changes value at the size where the scaling law changes slope, and relatively minor wave-like perturbations propagate up the size distribution from that point.

Collisional Model Results Scaling Law H3 An abrupt change to stronger particles at smaller sizes leads to an immediate trough in the size distribution for particles just larger than that at which the strength properties change, since the stronger particles survive longer and represent an overabundant source of projectiles to break up larger bodies.

Collisional Model Results Scaling Law H4 An abrupt change to weaker particles at smaller sizes leads to an immediate crest in the size distribution, since the weaker particles do not survive as long and represent an underabundant source of projectiles.

Conclusion Now that we are beginning to understand the extent to which the details of small-particle removal mechanisms and the effects of changes in size-strength scaling relations can affect the evolved size distribution at even the largest sizes, the time has come for a better understanding of the impact properties of particles smaller than ~10 centimeters. Example: George Flynn and I have proposed to conduct a series of impact experiments at the Ames Vertical Gun Range to determine (and demonstrate experimentally) the nature and extent of slope changes and/or discontinuities in Q*D. We will simulate the effects of small-scale structural inhomogeneities that might be expected to occur within small natural targets by constructing centimeter- to decimeter-scale spherical targets of plaster with imbedded BB-like spheres composed of a different material.