scholarly journals The origin of inner Solar System water

2017 ◽  
Vol 375 (2094) ◽  
pp. 20150384 ◽  
Author(s):  
Conel M. O'D. Alexander
Keyword(s):  
Solar System ◽  
Classical Model ◽  
Terrestrial Planet ◽  
Asteroid Belt ◽  
Carbonaceous Chondrites ◽  
Outer Solar System ◽  
Isotopic Compositions ◽  
O Isotopes ◽  
N Isotopes

Of the potential volatile sources for the terrestrial planets, the CI and CM carbonaceous chondrites are closest to the planets' bulk H and N isotopic compositions. For the Earth, the addition of approximately 2–4 wt% of CI/CM material to a volatile-depleted proto-Earth can explain the abundances of many of the most volatile elements, although some solar-like material is also required. Two dynamical models of terrestrial planet formation predict that the carbonaceous chondrites formed either in the asteroid belt (‘classical’ model) or in the outer Solar System (5–15 AU in the Grand Tack model). To test these models, at present the H isotopes of water are the most promising indicators of formation location because they should have become increasingly D-rich with distance from the Sun. The estimated initial H isotopic compositions of water accreted by the CI, CM, CR and Tagish Lake carbonaceous chondrites were much more D-poor than measured outer Solar System objects. A similar pattern is seen for N isotopes. The D-poor compositions reflect incomplete re-equilibration with H 2 in the inner Solar System, which is also consistent with the O isotopes of chondritic water. On balance, it seems that the carbonaceous chondrites and their water did not form very far out in the disc, almost certainly not beyond the orbit of Saturn when its moons formed (approx. 3–7 AU in the Grand Tack model) and possibly close to where they are found today. This article is part of the themed issue ‘The origin, history and role of water in the evolution of the inner Solar System’.

scholarly journals Slow and Fast Diffusion in Asteroid-Belt Resonances: A Review

1999 ◽  
Vol 172 ◽  
pp. 25-37
Author(s):  
S. Ferraz-Mello
Keyword(s):  
Solar System ◽  
Chaotic Behaviour ◽  
Asteroid Belt ◽  
Fast Diffusion ◽  
Outer Solar System ◽  
Recent Advances ◽  
Short Period ◽  
Hecuba Gap

AbstractThis paper reviews recent advances in several topics of resonant asteroidal dynamics as the role of resonances in the transportation of asteroids and asteroidal debris to the inner and outer solar system; the explanation of the contrast of a depleted 2/1 resonance (Hecuba gap) and a high-populated 3/2 resonance (Hilda group); the overall stochasticity created in the asteroid belt by the short-period perturbations of Jupiter’s orbit, with emphasis in the formation of significant three-period resonances, the chaotic behaviour of the outer asteroid belt, and the depletion of the Hecuba gap.

scholarly journals Isotopic evidence for primordial molecular cloud material in metal-rich carbonaceous chondrites

2016 ◽  
Vol 113 (8) ◽  
pp. 2011-2016 ◽  
Author(s):  
Elishevah M. M. E. Van Kooten ◽  
Daniel Wielandt ◽  
Martin Schiller ◽  
Kazuhide Nagashima ◽  
Aurélien Thomen ◽  
...  
Keyword(s):  
Solar System ◽  
Thermal Processing ◽  
Molecular Cloud ◽  
Decay Product ◽  
Isotopic Signature ◽  
Carbonaceous Chondrites ◽  
Outer Solar System ◽  
Precursor Material ◽  
System Composition ◽  
Cloud Material

The short-lived 26Al radionuclide is thought to have been admixed into the initially 26Al-poor protosolar molecular cloud before or contemporaneously with its collapse. Bulk inner Solar System reservoirs record positively correlated variability in mass-independent 54Cr and 26Mg*, the decay product of 26Al. This correlation is interpreted as reflecting progressive thermal processing of in-falling 26Al-rich molecular cloud material in the inner Solar System. The thermally unprocessed molecular cloud matter reflecting the nucleosynthetic makeup of the molecular cloud before the last addition of stellar-derived 26Al has not been identified yet but may be preserved in planetesimals that accreted in the outer Solar System. We show that metal-rich carbonaceous chondrites and their components have a unique isotopic signature extending from an inner Solar System composition toward a 26Mg*-depleted and 54Cr-enriched component. This composition is consistent with that expected for thermally unprocessed primordial molecular cloud material before its pollution by stellar-derived 26Al. The 26Mg* and 54Cr compositions of bulk metal-rich chondrites require significant amounts (25–50%) of primordial molecular cloud matter in their precursor material. Given that such high fractions of primordial molecular cloud material are expected to survive only in the outer Solar System, we infer that, similarly to cometary bodies, metal-rich carbonaceous chondrites are samples of planetesimals that accreted beyond the orbits of the gas giants. The lack of evidence for this material in other chondrite groups requires isolation from the outer Solar System, possibly by the opening of disk gaps from the early formation of gas giants.

scholarly journals Arrival and magnetization of carbonaceous chondrites in the asteroid belt before 4562 million years ago

2020 ◽  
Vol 1 (1) ◽  
Author(s):  
Timothy O’Brien ◽  
John A. Tarduno ◽  
Atma Anand ◽  
Aleksey V. Smirnov ◽  
Eric G. Blackman ◽  
...  
Keyword(s):  
Solar System ◽  
Arrival Time ◽  
Carbonaceous Chondrite ◽  
Parent Body ◽  
Asteroid Belt ◽  
Carbonaceous Chondrites ◽  
Early Solar System ◽  
Outer Disk ◽  
Main Asteroid Belt ◽  
Insight Into

AbstractMeteorite magnetizations can provide rare insight into early Solar System evolution. Such data take on new importance with recognition of the isotopic dichotomy between non-carbonaceous and carbonaceous meteorites, representing distinct inner and outer disk reservoirs, and the likelihood that parent body asteroids were once separated by Jupiter and subsequently mixed. The arrival time of these parent bodies into the main asteroid belt, however, has heretofore been unknown. Herein, we show that weak CV (Vigarano type) and CM (Mighei type) carbonaceous chondrite remanent magnetizations indicate acquisition by the solar wind 4.2 to 4.8 million years after Ca-Al-rich inclusion (CAI) formation at heliocentric distances of ~2–4 AU. These data thus indicate that the CV and CM parent asteroids had arrived near, or within, the orbital range of the present-day asteroid belt from the outer disk isotopic reservoir within the first 5 million years of Solar System history.

scholarly journals Earth’s water may have been inherited from material similar to enstatite chondrite meteorites

Science ◽  
2020 ◽  
Vol 369 (6507) ◽  
pp. 1110-1113 ◽  
Author(s):  
Laurette Piani ◽  
Yves Marrocchi ◽  
Thomas Rigaudier ◽  
Lionel G. Vacher ◽  
Dorian Thomassin ◽  
...  
Keyword(s):  
Solar System ◽  
Isotopic Composition ◽  
Carbonaceous Chondrite ◽  
Earth’S Crust ◽  
Outer Solar System ◽  
Volatile Elements ◽  
Earth’S Mantle ◽  
Isotopic Compositions ◽  
Enstatite Chondrite ◽  
Earth's Crust

The origin of Earth’s water remains unknown. Enstatite chondrite (EC) meteorites have similar isotopic composition to terrestrial rocks and thus may be representative of the material that formed Earth. ECs are presumed to be devoid of water because they formed in the inner Solar System. Earth’s water is therefore generally attributed to the late addition of a small fraction of hydrated materials, such as carbonaceous chondrite meteorites, which originated in the outer Solar System where water was more abundant. We show that EC meteorites contain sufficient hydrogen to have delivered to Earth at least three times the mass of water in its oceans. EC hydrogen and nitrogen isotopic compositions match those of Earth’s mantle, so EC-like asteroids might have contributed these volatile elements to Earth’s crust and mantle.

scholarly journals The Non-carbonaceous–Carbonaceous Meteorite Dichotomy

2020 ◽  
Vol 216 (4) ◽  
Author(s):  
T. Kleine ◽  
G. Budde ◽  
C. Burkhardt ◽  
T. S. Kruijer ◽  
E. A. Worsham ◽  
...  
Keyword(s):  
Solar System ◽  
Terrestrial Planet ◽  
Building Blocks ◽  
Asteroid Belt ◽  
Primitive Mantle ◽  
Volatile Species ◽  
Rapid Formation ◽  
History Of ◽  
Carbonaceous Meteorite ◽  
Siderophile Elements

Abstract The isotopic dichotomy between non-carbonaceous (NC) and carbonaceous (CC) meteorites indicates that meteorite parent bodies derive from two genetically distinct reservoirs, which presumably were located inside (NC) and outside (CC) the orbit of Jupiter and remained isolated from each other for the first few million years of the solar system. Here we review the discovery of the NC–CC dichotomy and its implications for understanding the early history of the solar system, including the formation of Jupiter, the dynamics of terrestrial planet formation, and the origin and nature of Earth’s building blocks. The isotopic difference between the NC and CC reservoirs is probably inherited from the solar system’s parental molecular cloud and has been maintained through the rapid formation of Jupiter that prevented significant exchange of material from inside (NC) and outside (CC) its orbit. The growth and/or migration of Jupiter resulted in inward scattering of CC bodies, which accounts for the co-occurrence of NC and CC bodies in the present-day asteroid belt and the delivery of presumably volatile-rich CC bodies to the growing terrestrial planets. Earth’s primitive mantle, at least for siderophile elements like Mo, has a mixed NC–CC composition, indicating that Earth accreted CC bodies during the final stages of its growth, perhaps through the Moon-forming giant impactor. The late-stage accretion of CC bodies to Earth is sufficient to account for the entire budget of Earth’s water and highly volatile species.

scholarly journals A scattered Uranus and Neptune, and implications for the asteroid belt

2004 ◽  
Vol 202 ◽  
pp. 241-243
Author(s):  
Edward W. Thommes ◽  
Martin J. Duncan ◽  
Harold F. Levison ◽  
John E. Chambers
Keyword(s):  
Solar System ◽  
Numerical Simulations ◽  
Initial Conditions ◽  
Asteroid Belt ◽  
Outer Solar System ◽  
Wide Range ◽  
Gas Giant ◽  
Gas Accretion ◽  
High Degree

It has been proposed that Uranus and Neptune originated interior to ∽ 10 AU, as potential gas giant cores which were scattered outward when Jupiter won the race to reach runaway gas accretion. We present further numerical simulations of this scenario, which show that it reproduces the present configuration of the outer Solar System with a high degree of success for a wide range of initial conditions. Also, we show that this mechanism may have simultaneously ejected planets from the asteroid belt.

scholarly journals An early dynamical instability among the Solar System’s giant planets triggered by the gas disk’s dispersal

2020 ◽  
Author(s):  
Beibei Liu ◽  
Sean Raymond ◽  
Seth Jacobson
Keyword(s):  
Solar System ◽  
Giant Planet ◽  
Terrestrial Planet ◽  
Small Mass ◽  
Giant Planets ◽  
Asteroid Belt ◽  
Dynamical Instability ◽  
Gaseous Disk ◽  
Orbital Configuration ◽  
A Chain

Abstract The Solar System’s orbital structure is thought to have been sculpted by a dynamical instability among the giant planets[1–4]. Yet the instability trigger and exact timing have proved hard to pin down[5–9]. The giant planets formed within a gas-dominated disk around the young Sun. Motivated by giant exoplanet systems found in mean motion resonance[10], hydrodynamical modeling has shown that while the disk was present the giant planets migrated into a compact orbital configuration, in a chain of resonances[2,11]. Here we use a suite of dynamical simulations to show that the giant planets’ instability was likely triggered by the dispersal of the Sun’s gaseous disk. As the disk evaporated from the inside-out, its inner edge swept successively across and dynamically perturbed each planet’s orbit in turn. Saturn and each ice giants’ orbits were torqued strongly enough to migrate outward. As a given planet migrated outward with the disk’s inner edge the orbital configuration of the exterior system was compressed, triggering dynamical instability. The final orbits of our simulated systems match those of the Solar System for a viable range of astrophysical parameters. Our results demonstrate that the giant planet instability happened as the gaseous disk dissipated, constrained by astronomical observations to be a few to ten million years after the birth of the Solar System [12]. Late-stage terrestrial planet formation would occur mostly after such an early giant planet instability [13,14], thereby avoiding the possibility of de-stabilizing the terrestrial planets [15] and naturally accounting for the small mass of Mars relative to Earth and the mass depletion of the main asteroid belt [16].

scholarly journals Shaping of the Inner Solar System by the Gas-Driven Migration of Jupiter

2012 ◽  
Vol 8 (S293) ◽  
pp. 204-211
Author(s):  
Kevin J. Walsh ◽  
Alessando Morbidelli ◽  
Sean N. Raymond ◽  
David P. O'Brien ◽  
Avi M. Mandell
Keyword(s):  
Solar System ◽  
Dynamical Behavior ◽  
Terrestrial Planet ◽  
Giant Planets ◽  
Asteroid Belt ◽  
Radial Migration ◽  
Migration History ◽  
Order Of Magnitude ◽  
History Of ◽  
Outward Migration

AbstractA persistent difficulty in terrestrial planet formation models is creating Mars analogs with the appropriate mass: Mars is typically an order of magnitude too large in simulations. Some recent work found that a small Mars can be created if the planetesimal disk from which the planets form has an outermost edge at 1.0 AU. However, that work and no previous work could produce a truncation of the planetesimal disk while also explaining the mass and structure of the asteroid belt. We show that gas-driven migration of Jupiter inward to 1.5 AU, before its subsequent outward migration, can truncate the disk and repopulate the asteroid belt. This dramatic migration history of Jupiter suggests that the dynamical behavior of our giant planets was more similar to that inferred for extra-solar planets than previously thought, as both have been characterised by substantial radial migration.

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