Dynamical Evolution of Main Belt Meteoroids: Numerical Simulations Incorporating Planetary Perturbations and Yarkovsky Thermal Forces

Bottke, W. F.; Rubincam, David Parry; Burns, Joseph A.

doi:10.1006/icar.2000.6361

Cited by 130 publications

(109 citation statements)

References 69 publications

(115 reference statements)

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“…This implies that based on the cosmogenic nuclide records alone we can not constrain whether the first-stage irradiation of Pitts occurred early in the meteoroid's history on the IAB iron meteorite parent body or immediately prior to the recent collision that excavated Pitts from its parent meteoroid ∼0.7 Myr ago. Although future measurements of long-lived 53 Mn (t 1/2 = 3.7 Myr) may shed more light on this issue, we will argue below that irradiation on a large precursor meteoroid is the most plausible scenario in the light of current meteorite delivery models (Gladman et al 1997;Bottke et al 2000).…”

Section: Pittsmentioning

confidence: 96%

“…However, the long CRE ages of iron meteorites also imply that irons have longer "storage times" in the asteroid belt than stones (Gladman et al 1997). These long storage times are now understood in the framework of the Yarkovsky effect (Rubincam 1995), which predicts very slow orbital drift rates for irons relative to those of stones (Farinella et al 1998;Hartmann et al 1999;Bottke et al 2000). The delivery of meteorites from the asteroid belt to Earth thus involves two steps: a slow mechanism driven by the Yarkovsky effect which gradually moves meter-to kmsized collisional fragments from their parent bodies in the asteroid belt to one of the orbital resonances.…”

Section: Introductionmentioning

confidence: 99%

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The complex exposure histories of the Pitts and Horse Creek iron meteorites: Implications for meteorite delivery models

Welten

Nishiizumi

Lavielle

et al. 2008

Meteorit & Planetary Scien

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available online at http://meteoritics.org The complex exposure histories of the Pitts and Horse Creek iron meteorites:Implications for meteorite delivery models Abstract-The concentrations of cosmogenic radionuclides and noble gases in Pitts (IAB) and Horse Creek (ungrouped) provide unambiguous evidence that both irons have a complex exposure history with a first-stage irradiation of 100-600 Myr under high shielding, followed by a second-stage exposure of ∼1 Myr as small objects. The first-stage exposure ages of ∼100 Myr for Horse Creek and ∼600 Myr for Pitts are similar to cosmic-ray exposure ages of other iron meteorites, and most likely represent the Yarkovsky orbital drift times of irons from their parent bodies in the main asteroid belt to one of the nearby chaotic resonance zones. The short second-stage exposure ages indicate that collisional debris from recent impact events on their precursor objects was quickly delivered to Earth. The short delivery times suggests that the recent collision events occurred while the precursor objects of Horse Creek and Pitts were either very close to the chaotic resonance zones or already in Earthcrossing orbits. Since the cosmogenic noble gas records of Horse Creek and Pitts indicate a minimum radius of a few meters for the precursor objects, but do not exclude km-sized objects, we conclude that these irons may represent fragments of two near-Earth asteroids, 3103 Eger and 1986 DA, respectively. Finally, we used the cosmogenic nuclide concentrations in Horse Creek, which contains 2.5 wt% Si, to test current model calculations for the production of cosmogenic 10 Be, 26 Al, and neonisotopes from iron, nickel, and silicon.

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Section: Pittsmentioning

confidence: 96%

Section: Introductionmentioning

confidence: 99%

The complex exposure histories of the Pitts and Horse Creek iron meteorites: Implications for meteorite delivery models

Welten

Nishiizumi

Lavielle

et al. 2008

Meteorit & Planetary Scien

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“…Accordingly, it is plausible that collisional grinding among asteroids in the outer main belt produces numerous CM-like particles that evolve inward via non-gravitational forces (e.g., Poynting-Robertson drag; Yarkovsky effect; Burns et al 1979). If the debris is centimeter-size or smaller, it can drift inward rapidly enough to jump resonance after resonance (e.g., Bottke et al 2000) on its way across the main belt. In some cases, the fragments may evolve and become very similar to those of main-belt families.…”

Section: Scenario 1 the CM Clasts Formed On Ancient Familiesmentioning

confidence: 99%

On the origin of shocked and unshocked CM clasts in H‐chondrite regolith breccias

Rubin

Bottke

2009

Meteorit & Planetary Scien

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Abstract--CM chondrite clasts that have experienced different degrees of aqueous alteration occur in H-chondrite and HED meteorite breccias. Many clasts are fragments of essentially unshocked CM projectiles that accreted at low relative velocities to the regoliths of these parent bodies. A few clasts were heated and dehydrated upon impact; these objects most likely accreted at higher relative velocities. We examined three clasts and explored alternative scenarios for their formation. In the first scenario, we assumed that the H and HED parent bodies had diameters of a few hundred kilometers, so that their high escape velocities would effectively prevent soft landings of small CM projectiles. This would imply that weakly shocked CM clasts formed on asteroidal fragments (family members) associated with the H and HED parent bodies. In the second scenario, we assumed that weakly shocked CM clasts were spall products ejected at low velocities from larger CM projectiles when they slammed into the H and HED parent bodies. In both cases, if most CM clasts turn out to have ancient ages (e.g., ~3.4-4

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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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Dynamical Evolution of Main Belt Meteoroids: Numerical Simulations Incorporating Planetary Perturbations and Yarkovsky Thermal Forces

Cited by 130 publications

References 69 publications

The complex exposure histories of the Pitts and Horse Creek iron meteorites: Implications for meteorite delivery models

The complex exposure histories of the Pitts and Horse Creek iron meteorites: Implications for meteorite delivery models

On the origin of shocked and unshocked CM clasts in H‐chondrite regolith breccias

Smithsonian Institution

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