Collisional Models and Scaling Laws: A New Interpretation of the Shape of the Main-Belt Asteroid Size Distribution

Durda, D. D.; Greenberg, R.; Jedicke, Robert

doi:10.1006/icar.1998.5960

Cited by 172 publications

(205 citation statements)

References 21 publications

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“…The t = 0 My timestep shows our initial conditions. The t = 3 My timestep shows a bump developing near D ∼ 2-3 km for both N rem and N dep ; this is a by-product of the "V"-shaped Q * D function (Campo Bagatin et al 1994;Durda et al 1998;Davis et al 2002). Self-gravity among D > 200 m objects makes them increasingly difficult to disrupt.…”

Section: Initial Conditions and A Sample Coddem Runmentioning

confidence: 99%

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The origin and evolution of stony meteorites

et al. 2004

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Abstract. The origin of stony meteorites landing on Earth today is directly linked to the history of the main belt, which evolved both through collisional evolution and dynamical evolution/depletion. In this paper, we focus our attention on the main belt dynamical evolution scenario discussed in Petit et al. (2001). According to Petit et al., during the planet formation epoch, the primordial main belt contained several Earth masses of material, enough to allow the asteroids to accrete on relatively short timescales.After a few My, the accretion of planetary embryos in the main belt zone dynamically stirred the remaining planetesimals to high enough velocities to initiate fragmentation. After a short interval, perhaps as long as 10 My, the primordial main belt was dynamically depleted of > 99% of its material via the combined perturbations of the planetary embryos and a newly-formed Jupiter. The small percentage of objects that survived in the main belt zone became the asteroid belt. It has been shown that the wavy-shaped size-frequency distribution of the main belt is a "fossil" left over from this violent period .Using a collisional/dynamical model of this scenario, we tracked the evolution of stony meteoroids produced by catastrophic disruption events over the last several Gy. We show that most stony meteoroids are a byproduct of a collisional cascade derived from large and ancient asteroid families or smaller, more recent breakup events. The meteoroids are then delivered to Earth by drifting in semimajor axis via Yarkovsky thermal drag forces until they reach a resonance powerful enough to place them on an Earth-crossing orbit.

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Section: Initial Conditions and A Sample Coddem Runmentioning

confidence: 99%

“…4 (Durda et al 1998;Bottke et al 2004a,b). The size distribution that provided the best fit for N rem followed the observed main belt for D > 200 km bodies, an incremental power law index of -4.5 for 110 < D < 200 km bodies, and an incremental power law index of -1.2 for D < 110 km bodies (Bottke et al 2004b).…”

Section: Initial Conditions and A Sample Coddem Runmentioning

confidence: 99%

The origin and evolution of stony meteorites

et al. 2004

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“…For small objects, Q D is determined solely by the material strength, while for objects larger than ∼100 m, the gravitational binding energy dominates. As a result, Q D is commonly described by the sum of two power laws (see, e.g., Davis et al 1985;Holsapple 1994;Paolicchi et al 1996;Durda & Dermott 1997;Durda et al 1998;Benz & Asphaug 1999;Kenyon & Bromley 2004b) , and P-R time (short-dashed). The collisional time is an average over the grain orbits with all possible pericentric distances q and eccentricities e, weighted with the amounts of those particles in the disk.…”

Section: Dynamical and Collisional Evolutionmentioning

confidence: 99%

The Debris Disk of Vega: A Steady-State Collisional Cascade, Naturally

Müller

Löhne

Krivov

2009

ApJ

102

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The archetypical debris disk around Vega has been observed intensively over the past 25 years. It has been argued that the resulting photometric data and images may be in contradiction with a standard, steady-state collisional scenario of the disk evolution. In particular, the emission in the mid-infrared (mid-IR) appears to be in excess of what is expected from a "Kuiper belt" at ∼100 AU, which is evident in the submillimeter images and inferred from the majority of photometric points. Here we re-address the question of whether or not the Vega disk observations are compatible with a continuous dust production through a collisional cascade. Instead of seeking a size and spatial distribution of dust that provide the best fit to observations, our approach involves physical modeling of the debris disk "from the sources." We assume that dust is maintained by a belt of parent planetesimals, and employ our collisional and radiative transfer codes to consistently model the size and radial distribution of the disk material and then thermal emission of dust. In doing so, we vary a broad set of parameters, including the stellar properties, the exact location, extension, and dynamical excitation of the planetesimal belt, chemical composition of solids, and the collisional prescription. We are able to reproduce the spectral energy distribution in the entire wavelength range from the near-IR to millimeter, as well as the mid-IR and submillimeter radial brightness profiles of the Vega disk. Thus, our results suggest that the Vega disk observations are not in contradiction with a steady-state collisional dust production, and we put important constraints on the disk parameters and physical processes that sustain it. The total disk mass in 100 km-sized bodies is estimated to be ∼10 Earth masses. Provided that collisional cascade has been operating over much of the Vega age of ∼350 Myr, the disk must have lost a few Earth masses of solids during that time. We also demonstrate that using an intermediate luminosity of the star between the pole and the equator, as derived from its fast rotation, is required to reproduce the debris disk observations. Finally, we show that including cratering collisions into the model is mandatory.

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“…If the most sophisticated sizefrequency distribution models (e.g., Durda et al, 1998) are correct, Bottke et al (2000) found that the flux of meteorite-sized ejecta produced by the largest asteroids (with the largest collisional cross sections) should dominate the flux produced by the smaller asteroids (which lose nearly all their ejecta due to low escape velocities). Hence, many of the chondrites and HEDs falling on Earth today may ultimately be derived from a few large source objects (e.g., 4 Vesta and 6 Hebe), despite that fact that nearly all mainbelt asteroids can potentially provide meteorite samples to Earth.…”

Section: Asteroids To Earth: the Dynamic Connectionmentioning

confidence: 99%

Smithsonian Institution

2009

Encyclopedia of United States Indian Policy and Law

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Extensive collection efforts in Antarctica and the Sahara in the past 10 years have greatly increased the number of known meteorites. Groupings of meteorites according to petrologic, mineralogical, bulk-chemical, and isotopic properties suggest the existence of 100-150 distinct parent bodies. Dynamical studies imply that most meteorites have their source bodies in the main belt and not among the near-Earth asteroids. Spectral observations of asteroids are currently the primary way of determining asteroid mineralogies. Linkages between ordinary chondrites and S asteroids, CM chondrites and C-type asteroids, the HEDs and 4 Vesta, and iron meteorites, enstatite chondrites, and M asteroids are discussed. However, it is difficult to conclusively link most asteroids with particular meteorite groups due to the number of asteroids with similar spectral properties and the uncertainties in the optical, chemical, and physical properties of the asteroid regolith.

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Collisional Models and Scaling Laws: A New Interpretation of the Shape of the Main-Belt Asteroid Size Distribution

Cited by 172 publications

References 21 publications

The origin and evolution of stony meteorites

The origin and evolution of stony meteorites

The Debris Disk of Vega: A Steady-State Collisional Cascade, Naturally

Smithsonian Institution

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