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

  title={3. Solar System Formation and Early Evolution: the First 100 Million Years},
  author={T. Montmerle and Jean Augereau and Marc Chaussidon and Matthieu Gounelle and Bernard Marty and Alessandro Morbidelli},
  journal={Earth, Moon, and Planets},
The solar system, as we know it today, is about 4.5 billion years old. It is widely believed that it was essentially completed 100 million years after the formation of the Sun, which itself took less than 1 million years, although the exact chronology remains highly uncertain. For instance: which, of the giant planets or the terrestrial planets, formed first, and how? How did they acquire their mass? What was the early evolution of the “primitive solar nebula” (solar nebula for short)? What is… Expand
The abundance of 26Al-rich planetary systems in the Galaxy
One of the most puzzling properties of the solar system is the high abundance at its birth of 26Al, a short-lived radionuclide with a mean life of 1 Myr. Now decayed, it has left its imprint inExpand
Water formation in early solar nebula: I. Quasi-stationary cloud core
Abstract An important condition for the habitability of rocky planets is the existence of water in or on their upper lithospheric layer. We will show that the available amount of this water dependsExpand
Origin and evolution of the atmospheres of early Venus, Earth and Mars
We review the origin and evolution of the atmospheres of Earth, Venus and Mars from the time when their accreting bodies were released from the protoplanetary disk a few million years after theExpand
A Perspective from Extinct Radionuclides on a Young Stellar Object: The Sun and Its Accretion Disk
Meteorites, which are remnants of solar system formation, provide a direct glimpse into the dynamics and evolution of a young stellar object (YSO), namely our Sun. Much of our knowledge about theExpand
Formation of the Proto-Earth in the Solar Nebula
In Chapter 2, formation of the solar system from a gas nebula is discussed. In geophysical models, our solar system is considered to have started from the gas cloud. Then it began to gather andExpand
Two Different Sources of Water for the Early Solar Nebula
The chemical mechanics for water formation and its expected abundance are explored by studying the parental cloud core of the solar nebula and its gravitational collapse and the dependence of the production of water on the initial abundance ratio between carbon and oxygen is analysed. Expand
Supernova Propagation and Cloud Enrichment: A new model for the origin of 60Fe in the early solar system
The radioactive isotope Fe-60 (T-1/2 = 1.5 Myr) was present in the early solar system. It is unlikely that it was injected directly into the nascent solar system by a single, nearby supernova (SN).Expand
Formation and Evolution of Protoatmospheres
The origin and evolution of planetary protoatmospheres in relation to the protoplanetary disk is discussed. The initial atmospheres of planets can mainly be related via two formation scenarios. If aExpand
The influence of melting on the thermo-chemical evolution of rocky planets' interiors
The last couple of years have seen a surge in the discovery of extra-solar terrestrial planets. Some of these planets orbit their stars within the so-called habitable zone, which has raised questionsExpand
The origin of short-lived radionuclides and the astrophysical environment of solar system formation
Based on early solar system abundances of short-lived radionuclides (SRs), such as Al-26 (T-1/2 = 0.74 Myr) and Fe-60 (T-1/2 1.5 Myr), it is often asserted that the Sun was born in a large stellarExpand


A short timescale for terrestrial planet formation from Hf–W chronometry of meteorites
Measurements of tungsten isotope compositions and hafnium–tungsten ratios of several meteorites indicate that the bulk of metal–silicate separation in the Solar System was completed within <30 Myr, completely consistent with other evidence for rapid planetary formation. Expand
The formation of planetesimals.
Four stages in the accretion of planetesimals are described. The initial stage is the condensation of dust particles from the gaseous solar nebula as it cools. These dust particles settle into a thinExpand
Short-Lived Nuclei in the Early Solar System: A Low Mass Stellar Source?
Abstract We discuss possible stellar origins of short-lived radioactive nuclei with meanlife τ ≤ 100 Myr, which were shown to be alive in the Early Solar System (ESS). We first review current ideasExpand
THE INTERIORS OF GIANT PLANETS: Models and Outstanding Questions
▪ Abstract We know that giant planets played a crucial role in the making of our Solar System. The discovery of giant planets orbiting other stars is a formidable opportunity to learn more aboutExpand
Planets in the asteroid belt
— The main asteroid belt has lost >99.9% of its solid mass since the time at which the planets were forming, according to models for the protoplanetary nebula. Here we show that the primordialExpand
Formation of the Giant Planets by Concurrent Accretion of Solids and Gas
New numerical simulations of the formation of the giant of the second phase. planets are presented, in which for the first time both the gas and The actual rates at which the giant planets accretedExpand
The Accretion, Composition and Early Differentiation of Mars
The early development of Mars is of enormous interest, not just in its own right, but also because it provides unique insights into the earliest history of the Earth, a planet whose origins have beenExpand
Hafnium–tungsten chronometry and the timing of terrestrial core formation
THE accretion of the Earth and Moon within the solar nebula is thought1–3 to have taken 50 to 100 million years. But the timing of formation of the Earth's core has been controversial, with some4,5Expand
Making More Terrestrial Planets
The results of 16 new 3D N-body simulations of the final stage of the formation of the terrestrial planets are presented. These Nbody integrations begin with 150‐160 lunar-to-Mars size planetaryExpand
Formation of the Earth
The origin of the earth is discussed in the context of the formation of the sun and the planets, and a standard model for such a formation assuming gravitational instability in a dense interstellarExpand