Solar System Formation and Early Evolution: the First 100 Million Years

Montmerle, T.; Augereau, Jean-Charles; Chaussidon, M.; Gounelle, M.; Marty, Bernard; Morbidelli, Alessandro

doi:10.1007/978-0-387-45083-4_3

Cited by 12 publications

(14 citation statements)

References 133 publications

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“…An important constraint on the formation of giant planets is that the disk gas probably dissipated in less than ∼10 Myr, implying that Jupiter and Saturn acquired their massive atmospheres within this time span. A similar argument is valid for the existence of the (thinner) atmospheres of Uranus and Neptune, suggesting that the formation of these planets was accomplished a short time after the dissipation of the disk gas (e.g., Montmerle et al, 2006).…”

Section: Introductionmentioning

confidence: 82%

“…Later, it would have been transported outwards by resonant interactions and scattering with Neptune. Thus, this scenario follows the idea of a hypothetical resident planetoid in the scattered disk, and the time t = 0 for the model is set at the late stages of giant planet formation, a few tens of Myr after the birth of the solar system (e.g., Montmerle et al, 2006).…”

Section: The Origin and Evolution Of The Transneptunian Belt With Thementioning

confidence: 99%

“…After that, these small grains grew further in a few million years (Myr) to kmsized planetesimals through mutual accreting collisions, or alternatively as large clumps in local instability niches (e.g., Morbidelli et al, 2009a). Shortly after the formation of such planetesimals, planetary-sized ones grew quickly (during the so-called runaway+oligarchic growth) leading to the formation of terrestrial planets and the core of the giant planets on ten-million-year timescales (Hayashi et al, 1985;Pollack et al, 1996;Montmerle et al, 2006). An important constraint on the formation of giant planets is that the disk gas probably dissipated in less than ∼10 Myr, implying that Jupiter and Saturn acquired their massive atmospheres within this time span.…”

Section: Introductionmentioning

confidence: 99%

“…Nevertheless, all these objects originated from the same protoplanetary disk of gas and dust that existed billions of years (Gyr) ago. Based on the oldest collected meteorites on Earth, it is well known that the solar system is almost 4.6 Gyr old (e.g., Montmerle et al, 2006 and references therein). Therefore, the solar system represents the outcome of a complex structure that has been evolving chemically, collisionally, and dynamically over the last ∼4.6 Gyr.…”

Section: Introductionmentioning

confidence: 99%

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Trans-Neptunian Objects as Natural Probes to the Unknown Solar System

Lykawka¹

2012

Monogr. Environ. Earth Planets

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Citation: Lykawka, P. S. (2012), Trans-Neptunian objects as natural probes to the unknown solar system, Monogr. Environ. Earth Planets, 1, 121-186, doi:10.5047/meep.2012.00103.0121. Abstract Trans-Neptunian objects (TNOs) are icy/rocky bodies that move beyond the orbit of Neptune in a region known as the trans-Neptunian belt (or Edgeworth-Kuiper belt). TNOs are believed to be the remnants of a collisionally, dynamically and chemically evolved protoplanetary disk composed of billions of planetesimals, the building blocks from which the planets formed during the early solar system. Consequently, the study of the physical and dynamical properties of TNOs can reveal important clues about the properties of that disk, planet formation, and other evolutionary processes that likely occurred over the last 4.5 Gyr. In contrast to the predictions of accretion models that feature protoplanetary disk planetesimals evolving on dynamically cold orbits (with both very small eccentricities, e, and inclinations, i), in reality TNOs exhibit surprisingly wide ranges of orbital eccentricities and inclinations, from nearly circular to very eccentric orbits (putting some objects at aphelia beyond 1000 AU!) and ranging up to ∼50 deg of inclination with respect to the fundamental plane of the solar system. We can group TNOs into several distinct dynamical classes: (1) Resonant: TNOs currently locked in external Neptunian mean motion resonances; (2) Classical: non-resonant TNOs concentrated with semimajor axes in the range 37 < a < 45-50 AU on relatively stable orbits (which typically feature only minor orbital changes over time); (3) Scattered: TNOs on orbits that suffer(ed) notable gravitational perturbations by Neptune, yielding macroscopic orbital changes over time; (4) Detached: TNOs typically possessing perihelia, q > 40 AU, a > 45-50 AU and orbits stable over the age of the solar system. Several theoretical models have addressed the origin and orbital evolution of the main dynamical classes of TNOs, but none have successfully reproduced them all. In addition, none have explained several objects on peculiar orbits, or provided insightful predictions, without which a model cannot be tested properly against observations. Based on extensive simulations of planetesimal disks with the presence of the four giant planets and huge numbers of modeled planetesimals (reaching up to a million test particles or several thousand massive objects), I explore in detail the dynamics of the TNOs, in particular their (un)stable regions over timescales comparable to the age of the solar system, and the role of resonances across the entire trans-Neptunian region. I also propose that, along with the orbital history of the giant planets, the orbital evolution of primordial embryos (massive planetesimals comparable to Mars-Earth masses) can explain the fine orbital structure of the trans-Neptunian belt, the orbits of Jovian and Neptunian Trojans (objects moving about the L4/L5 Lagrange points of Jupiter and Neptune, respectively), and possibly the curr...

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Section: Introductionmentioning

confidence: 82%

Section: The Origin and Evolution Of The Transneptunian Belt With Thementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Trans-Neptunian Objects as Natural Probes to the Unknown Solar System

Lykawka¹

2012

Monogr. Environ. Earth Planets

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“…formulated, especially explaining the accretion mechanism that could have led to the formation of a terrestrial-like planet (Montmerle et al, 2006). The formation of Earth is quite precisely dated at 4 56 Ga ago, based on the dating of a particular type of meteorites called "ordinary chondrites."…”

mentioning

confidence: 99%

The origin of modern terrestrial life

Forterre

Gribaldo

2007

HFSP Journal

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The study of the origin of life covers many areas of expertise and requires the input of various scientific communities. In recent years, this research field has often been viewed as part of a broader agenda under the name of "exobiology" or "astrobiology." In this review, we have somewhat narrowed this agenda, focusing on the origin of modern terrestrial life. The adjective "modern" here means that we did not speculate on different forms of life that could have possibly appeared on our planet, but instead focus on the existing forms "cells and viruses…. We try to briefly present the state of the art about alternative hypotheses discussing not only the origin of life per se, but also how life evolved to produce the modern biosphere through a succession of steps that we would like to characterize as much as possible.

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