The Primordial Excitation and Clearing of the Asteroid Belt

Petit, Jean-Marc; Morbidelli, Alessandro; Chambers, John E.

doi:10.1006/icar.2001.6702

Cited by 223 publications

(230 citation statements)

References 17 publications

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“…One of the features of the MB frequently mentioned in the literature is a dynamical excitation of its objects (e.g., Petit et al 2001;O'Brien et al 2007). Indeed, the current theories of planet formation assume that, initially, the eccentricities and inclinations of the primordial MB objects were low enough for the accretion processes to occur.…”

Section: Dynamical Excitationmentioning

confidence: 99%

“…This is something that must not be overlooked when trying to compare the result of migration/accretion models to the present day MB. Petit et al (2001), for example, claim that this characteristics of the MB is a byproduct of a dynamical removal mechanism associated with the late stages of planet formation. Their model shows that Jupiter's formation could have produced sweeping resonances and/or the scattering and excitation of large planetary embryos within the MB, thereby eliminating most of the bodies from the primordial MB shortly after Jupiter reached full size (i.e., presumably some 10 Myr.…”

Section: Dynamical Excitationmentioning

confidence: 99%

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On the current distribution of main belt objects: Constraints for evolutionary models

Michtchenko

Lazzaro

Carvano

2016

A&A

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Context. It is widely accepted that the current distribution of material in the main asteroidal belt (MB) is a product of the evolutionary history of the solar system during its whole lifetime of ∼4.5 billions of years and is, consequently, a major witness of the diverse stages of this evolution. Aims. The purpose of this paper is twofold: first, we study the principal aspects of the distribution of the asteroids in proper element space, mass, and, physical composition for a complete picture of the current MB. Second, we analyze if and how these current distributions can be explained by the long-lasting dynamical effects of the planets on this region of the solar system. Methods. We studied the distribution in the proper element space for the sample that consists of about 350 000 objects whose proper orbital elements are available from the database AstDyS. We studied the distribution in size and physical composition using the most recent and large available datasets. We constructed the dynamical portrait of the MB in form of the dynamical and averaged maps via the spectral analysis method. Results. The main properties of the current distributions of MB objects are identified. A comparison of the distributions of real objects with dynamical maps allows us to detect principal mechanisms of the diffusive transportation of the objects. These mechanisms are related to mean-motion resonances (MMRs) and secular resonances (SRs), overlaying with the slow dissipative Yarkovsky/Yorp drift. Conclusions. We identify the most relevant distributions of the material in the MB and show that many of the current features of the MB can be explained by the interplay of diverse dynamical mechanisms due to the planetary perturbations over 4 Gyr with nongravitational effects, without the need of 'catastrophic' events or 'ad hoc' migration mechanisms during the early stages of the solar system. In this sense, the obtained distributions can provide relevant constraints for modeling the origin and evolution of the MB.

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Section: Dynamical Excitationmentioning

confidence: 99%

Section: Dynamical Excitationmentioning

confidence: 99%

On the current distribution of main belt objects: Constraints for evolutionary models

Michtchenko

Lazzaro

Carvano

2016

A&A

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“…Fast migration and slow migration scenarios and between the no migration scenario and solar abundances (data from [21]), where the captured mass is homogeneously mixed into a 5000 km thick outer molecular shell of initial solar composition scatter planetesimals inside the now-depleted locations of the orbital resonances with the giant planets. This phase has been studied, in the Solar System, to investigate the mass depletion of the asteroid belt [6,36,40,58]. During this phase, the population of planetesimals in the affected regions decays exponentially, decreasing by about two orders of magnitude in about 100 Ma (see e.g.…”

Section: Post-formation Evolution Late Accretion and Protoplanetary mentioning

confidence: 99%

The role of planetary formation and evolution in shaping the composition of exoplanetary atmospheres

2014

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Over the last twenty years, the search for extrasolar planets has revealed the rich diversity of outcomes from the formation and evolution of planetary systems. In order to fully understand how these extrasolar planets came to be, however, the orbital and physical data we possess are not enough, and they need to be complemented with information about the composition of the exoplanets. Ground-based and space-based observations provided the first data on the atmospheric composition of a few extrasolar planets, but a larger and more detailed sample is required before we can fully take advantage of it. The primary goal of a dedicated space mission like the Exoplanet Characterization Observatory (EChO) proposal is to fill this gap and to expand the limited data we possess by performing a systematic survey of extrasolar planets. The full exploitation of the data that space-based and ground-based facilities will provide in the near future, however, requires knowledge about the sources and sinks of the chemical species and molecules that will be observed. Luckily, the study of the past history of the Solar System provides several indications about the effects of processes like migration, late accretion and secular impacts, and on the time they occur in the life of planetary systems. In this work we will review what is

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“…To compare the planetesimal distribution obtained in our simulations with the "real" asteroid population, we focus on asteroids larger than ∼50 km in diameter, as in previous works (Petit et al 2001;Minton & Malhotra 2009;Morbidelli et al 2010). These bodies are a reliable tracer of the structure of the asteroid belt that resulted from the primordial sculpting process(es), as they are too large to have their orbits altered significantly by the thermal Yarkovsky effect or by collisions (see Fig.…”

Section: The Asteroid Beltmentioning

confidence: 99%

The effect of an early planetesimal-driven migration of the giant planets on terrestrial planet formation

Walsh

Morbidelli

2011

A&A

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The migration of the giant planets due to the scattering of planetesimals causes powerful resonances to move through the asteroid belt and the terrestrial planet region. Exactly when and how the giant planets migrated is not well known. In this paper we present results of an investigation of the formation of the terrestrial planets during and after the migration of the giant planets. The latter is assumed to have occurred immediately after the dissipation of the nebular disk -i.e. "early" with respect to the timing of the late heavy bombardment (LHB). The presumed cause of our modeled early migration of the giant planets is angular mometum transfer between the planets and scattered planetesimals. Our model forms the terrestrial planets from a disk of material which stretchs from 0.3-4.0 AU, evenly split in mass between planetesimals and planetary embryos. Jupiter and Saturn are initially at 5.4 and 8.7 AU respectively, on orbits with eccentricities comparable to the current ones, and migrate to 5.2 and 9.4 AU with an e-folding time of 5 Myr. Unfortunately, the terrestrial planets formed in the simulations are not good analogs for the current solar system, with Mars typically being much too massive. Moreover, the final distribution of the planetesimals remaining in the asteroid belt is inconsistent with the observed distribution of asteroids. This argues that, even if giant planet migration had occurred early, the real evolution of the giant planets would have to have been of the "jumping-Jupiter" type, i.e. the increase in orbital separation between Jupiter and Saturn had to be dominated by encounters between Jupiter and a third, Neptune-mass planet. This result was already demonstrated for late migrations occuring at the LHB time by previous work, and this paper shows those conclusions hold for early migration as well.

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The Primordial Excitation and Clearing of the Asteroid Belt

Cited by 223 publications

References 17 publications

On the current distribution of main belt objects: Constraints for evolutionary models

On the current distribution of main belt objects: Constraints for evolutionary models

The role of planetary formation and evolution in shaping the composition of exoplanetary atmospheres

The effect of an early planetesimal-driven migration of the giant planets on terrestrial planet formation

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