Cosmic-Ray Exposure History of Ordinary Chondrites

Marti, K.; Graf, Thomas

doi:10.1146/annurev.ea.20.050192.001253

Cited by 201 publications

(115 citation statements)

References 46 publications

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“…In such a scenario, the different petrologic types would have formed on separate parent bodies (Yomogida & Matsui 1984), which is in contradiction with the cosmic-ray exposure (CRE) ages of individual OCs. The latter shows that, for some classes (mainly H chondrites), several petrologic types (mainly types 4 and 5 in the H case; Marti & Graf 1992;Graf & Marti 1994;Graf & Marti 1995) show similar peaks in their CRE age distribution, and thus suggest that the different petrologic types do originate from the same parent body.…”

Section: Introductionmentioning

confidence: 90%

Multiple and Fast: The Accretion of Ordinary Chondrite Parent Bodies

Vernazza

Zanda

Binzel

et al. 2014

ApJ

125

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Although petrologic, chemical, and isotopic studies of ordinary chondrites and meteorites in general have largely helped establish a chronology of the earliest events of planetesimal formation and their evolution, there are several questions that cannot be resolved via laboratory measurements and/or experiments alone. Here, we propose the rationale for several new constraints on the formation and evolution of ordinary chondrite parent bodies (and, by extension, most planetesimals) from newly available spectral measurements and mineralogical analysis of main-belt S-type asteroids (83 objects) and unequilibrated ordinary chondrite meteorites (53 samples). Based on the latter, we suggest that spectral data may be used to distinguish whether an ordinary chondrite was formed near the surface or in the interior of its parent body. If these constraints are correct, the suggested implications include that: (1) large groups of compositionally similar asteroids are a natural outcome of planetesimal formation and, consequently, meteorites within a given class can originate from multiple parent bodies; (2) the surfaces of large (up to ∼200 km) S-type main-belt asteroids mostly expose the interiors of the primordial bodies, a likely consequence of impacts by small asteroids (D < 10 km) in the early solar system; (3) the duration of accretion of the H chondrite parent bodies was likely short (instantaneous or in less than ∼10 5 yr, but certainly not as long as 1 Myr); (4) LL-like bodies formed closer to the Sun than H-like bodies, a possible consequence of the radial mixing and size sorting of chondrules in the protoplanetary disk prior to accretion.

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Section: Introductionmentioning

confidence: 90%

Multiple and Fast: The Accretion of Ordinary Chondrite Parent Bodies

Vernazza

Zanda

Binzel

et al. 2014

ApJ

125

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show abstract

“…Constraints that can be used to test our model include various meteorite CRE age distributions (e.g., H, L, and LL chondrites; Marti & Graf 1992;Morbidelli & Gladman 1998;Vokrouhlický & Farinella 2000;Eugster 2003). Our model implies that the wide range of CRE ages observed among the H, L, and LL meteorite classes (∼ 10-100 My) are unlikely to come from multiple cratering events on a single parent body (e.g., .…”

Section: The Evolution Of Asteroid Families and Stony Meteoroidsmentioning

confidence: 97%

“…CRE ages measure the time interval spent in space between the meteoroid's formation as a D < 3 m body (following removal from a shielded location within a larger object) and its arrival at Earth (e.g., Morbidelli and Gladman 1998). The CRE ages of most stony meteorites are between ∼ 10-100 My, while iron meteorites have CRE ages between ∼ 0.1-1.0 Gy (Caffee et al 1988;Marti & Graf 1992;Eugster 2003). Because these timescales are longer than the average dynamical lifetime of near-Earth asteroids (∼ 4 My; Bottke et al 2002a), we infer that many meteoroids, particularly iron meteoroids, had to obtain considerable damage from cosmic rays while drifting in the main belt as a meter-sized body.…”

Section: Introductionmentioning

confidence: 99%

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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“…A study of the stability of organic species in a relevant space environment is crucial to constrain the amount of organic material that might have been imported to the primitive Earth, especially on small particles such as IDPs in which the organic content is much less protected from radiations than in the larger bodies where only the surface is affected by radiation (Muñoz Caro et al 2006). In addition cosmic rays change the elemental and isotopic composition in meteorites (Marti and Graf 1992). However, certain minerals protect organic molecules against degradation by radiation (i.e.…”

Section: Small Bodies and Exogeneous Sources Of Organic Compounds mentioning

confidence: 99%

Space as a Tool for Astrobiology: Review and Recommendations for Experimentations in Earth Orbit and Beyond

et al. 2017

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The space environment is regularly used for experiments addressing astrobiology research goals. The specific conditions prevailing in Earth orbit and beyond, notably the radiative environment (photons and energetic particles) and the possibility to conduct long-duration measurements, have been the main motivations for developing experimental concepts to expose chemical or biological samples to outer space, or to use the reentry of a spacecraft on Earth to simulate the fall of a meteorite. This paper represents an overview of past and current research in astrobiology conducted in Earth orbit and beyond, with a special focus on ESA missions such as Biopan, STONE (on Russian FOTON capsules) and EXPOSE facilities (outside the International Space Station). The future of exposure platforms is discussed, notably how they can be improved for better science return, and how to incorporate the use of small satellites such as those built in cubesat format.

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Cosmic-Ray Exposure History of Ordinary Chondrites

Cited by 201 publications

References 46 publications

Multiple and Fast: The Accretion of Ordinary Chondrite Parent Bodies

Multiple and Fast: The Accretion of Ordinary Chondrite Parent Bodies

The origin and evolution of stony meteorites

Space as a Tool for Astrobiology: Review and Recommendations for Experimentations in Earth Orbit and Beyond

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