Solar system Nd isotope heterogeneity: Insights into nucleosynthetic components and protoplanetary disk evolution

2020 ◽  
Vol 281 ◽  
pp. 135-148
Author(s):  
Nikitha Susan Saji ◽  
Daniel Wielandt ◽  
Jesper Christian Holst ◽  
Martin Bizzarro
Keyword(s):  
Solar System ◽  
Protoplanetary Disk ◽  
Nd Isotope ◽  
Disk Evolution

scholarly journals The Grand Tack model: a critical review

2014 ◽  
Vol 9 (S310) ◽  
pp. 194-203 ◽  
Author(s):  
Sean N. Raymond ◽  
Alessandro Morbidelli
Keyword(s):  
Solar System ◽  
Building Blocks ◽  
Protoplanetary Disk ◽  
Giant Planets ◽  
Asteroid Belt ◽  
Terrestrial Planets ◽  
Saturn’S Satellites ◽  
Internal Inconsistency ◽  
Solar System Bodies ◽  
Gas Accretion

AbstractThe “Grand Tack” model proposes that the inner Solar System was sculpted by the giant planets' orbital migration in the gaseous protoplanetary disk. Jupiter first migrated inward then Jupiter and Saturn migrated back outward together. If Jupiter's turnaround or “tack” point was at ~ 1.5 AU the inner disk of terrestrial building blocks would have been truncated at ~ 1 AU, naturally producing the terrestrial planets' masses and spacing. During the gas giants' migration the asteroid belt is severely depleted but repopulated by distinct planetesimal reservoirs that can be associated with the present-day S and C types. The giant planets' orbits are consistent with the later evolution of the outer Solar System.Here we confront common criticisms of the Grand Tack model. We show that some uncertainties remain regarding the Tack mechanism itself; the most critical unknown is the timing and rate of gas accretion onto Saturn and Jupiter. Current isotopic and compositional measurements of Solar System bodies – including the D/H ratios of Saturn's satellites – do not refute the model. We discuss how alternate models for the formation of the terrestrial planets each suffer from an internal inconsistency and/or place a strong and very specific requirement on the properties of the protoplanetary disk.We conclude that the Grand Tack model remains viable and consistent with our current understanding of planet formation. Nonetheless, we encourage additional tests of the Grand Tack as well as the construction of alternate models.

A tandem-column extraction chromatography for Nd separation: minimizing mass-independent isotope fractionation for ultrahigh-precision Nd isotope-ratio analysis

2022 ◽  
Author(s):  
Da Wang ◽  
Richard Carlson
Keyword(s):  
Solar System ◽  
Extraction Chromatography ◽  
Isotope Ratio ◽  
Isotope Fractionation ◽  
Ratio Analysis ◽  
Nd Isotope ◽  
Planetary Differentiation ◽  
Isotope Ratio Analysis ◽  
Isotope System ◽  
Column Extraction

The short-lived 146Sm-142Nd isotope system traces key early planetary differentiation processes that occurred during the first 500 million-years of solar system history. The variations of 142Nd/144Nd in terrestrial samples, typically...

3. Beautiful theories, ugly facts

2021 ◽  
pp. 31-46
Author(s):  
Raymond T. Pierrehumbert
Keyword(s):  
Angular Momentum ◽  
Solar System ◽  
Planetary Systems ◽  
Protoplanetary Disk ◽  
Newtonian Gravity ◽  
The Sun ◽  
French Mathematician ◽  
Modern Form

‘Beautiful theories, ugly facts’ evaluates the theories on planetary systems, particularly the Solar System. In 1734, the Swedish polymath Emmanuel Swedenborg proposed that the Sun and all the planets condensed out of the same ball of gas, in what is probably the earliest statement of the nebular hypothesis. The nebular hypothesis entered something close to its modern form in the hands of the French mathematician Pierre-Simon Laplace, who in 1796 made the clear connection to Newtonian gravity. The angular momentum problem and the structure of a protoplanetary disk, the formation of rocky cores, and the gravitational accretion of gas in the disk also come under this topic.

scholarly journals Cometary Chemistry and the Origin of Icy Solar System Bodies: The View After Rosetta

2019 ◽  
Vol 57 (1) ◽  
pp. 113-155 ◽  
Author(s):  
Kathrin Altwegg ◽  
Hans Balsiger ◽  
Stephen A. Fuselier
Keyword(s):  
Solar System ◽  
Protoplanetary Disk ◽  
Isotopic Ratios ◽  
Parent Species ◽  
Rosetta Mission ◽  
Solar System Bodies ◽  
Diverse Origin ◽  
Life On Earth ◽  
Collapsing Cloud

In situ research of cometary chemistry began when measurements from the Giotto mission at Comet 1P/Halley revealed the presence of complex organics in the coma. New telescopes and space missions have provided detailed remote and in situ measurements of the composition of cometary volatiles. Recently, the Rosetta mission to Comet 67P/Churyumov–Gerasimenko (67P) more than doubled the number of parent species and the number of isotopic ratios known for comets. Forty of the 71 parent species have also been detected in pre- and protostellar clouds. Most isotopic ratios are nonsolar. This diverse origin is in contrast to that of the Sun, which received its material from the bulk of the collapsing cloud. The xenon isotopic ratios measured in 67P can explain the long-standing question about the origin of terrestrial atmospheric xenon. These findings strengthen the notion that comets are indeed an important link between the ISM and today's solar system including life on Earth. ▪ Nonsolar isotopic ratios for species such as Xe, N, S, and Si point to a nonhomogenized protoplanetary disk from which comets received their material. ▪ The similarity of the organic inventories of comets and presolar and protostellar material makes it plausible that this material was accreted almost unaltered by comets from the presolar stage. ▪ Large variations in the deuterium-to-hydrogen ratio in water for comets indicate a large range in the protoplanetary disk from which comets formed. ▪ The amount of organics delivered by comets to Earth may be highly significant.

scholarly journals Dynamics of the Giant Planets of the Solar System in the Gaseous Protoplanetary Disk and Their Relationship to the Current Orbital Architecture

2007 ◽  
Vol 134 (5) ◽  
pp. 1790-1798 ◽  
Author(s):  
Alessandro Morbidelli ◽  
Kleomenis Tsiganis ◽  
Aurélien Crida ◽  
Harold F. Levison ◽  
Rodney Gomes
Keyword(s):  
Solar System ◽  
Protoplanetary Disk ◽  
Giant Planets

scholarly journals The Mg/Fe ratio of silicate minerals in the meteoritic materials and in the circumstellar environment: A case study for the chondritic-like composition

2021 ◽  
Vol 30 (1) ◽  
pp. 45-55
Author(s):  
Péter Futó ◽  
József Vanyó ◽  
Irakli Simonia ◽  
János Sztakovics ◽  
Mihály Nagy ◽  
...  
Keyword(s):  
Solar System ◽  
Crystallization Process ◽  
Planet Formation ◽  
Methodological Approach ◽  
Optical Microscope ◽  
Protoplanetary Disk ◽  
Early Solar System ◽  
System A ◽  
Circumstellar Environment

Abstract Kaba meteorite as a reference material (one of a least metamorphosed and most primitive carbonaceous chondrites fell on Earth) was chosen for this study providing an adequate background for study of the protoplanetary disk or even the crystallization processes of the Early Solar System. Its olivine minerals (forsterite and fayalite) and their Mg/Fe ratio can help us to understand more about the planet formation mechanism and whether or not the metallic constitutes of the disk could be precursors for the type of planets in the Solar System. A multiple methodological approach such as a combination of the scanning electron microscope, optical microscope, Raman spectroscopy and electron microprobe of the olivine grains give the Fe/Mg ratio database. The analyses above confirmed that planet formation in the protoplanetary disk is driven by the mineralogical precursors of the crystallization process. On the other hand, four nebulae mentioned in this study provide the astronomical data confirming that the planet formation in the protoplanetary disk is dominated or even driven by the metallic constituents.

scholarly journals PROTOPLANETARY DISK EVOLUTION AROUND THE TRIGGERED STAR-FORMING REGION CEPHEUS B

2009 ◽  
Vol 699 (2) ◽  
pp. 1454-1472 ◽  
Author(s):  
Konstantin V. Getman ◽  
Eric D. Feigelson ◽  
Kevin L. Luhman ◽  
Aurora Sicilia-Aguilar ◽  
Junfeng Wang ◽  
...  
Keyword(s):  
Protoplanetary Disk ◽  
Star Forming ◽  
Disk Evolution

scholarly journals Protoplanetary Disk Evolution and Influence of the Host Star

2013 ◽  
Vol 8 (S299) ◽  
pp. 374-375
Author(s):  
Kévin Baillié ◽  
Sébastien Charnoz
Keyword(s):  
Numerical Model ◽  
Surface Density ◽  
Accretion Rate ◽  
Protoplanetary Disk ◽  
Star Mass ◽  
Mass Accretion Rate ◽  
Disk Mass ◽  
Rate Versus ◽  
Self Consistent ◽  
Disk Evolution

AbstractBased on a self-consistent coupling between protoplanetary disk thermodynamics, photosphere geometry and dynamics we designed a 1D-hydrodynamical numerical model for the spreading of the disks as a function of the star characteristics. We found that the evolution timescale increases for more massive or for a steeper surface density disk, and decreases for bigger stars or less turbulent disks. We found a strong dependency of the mass accretion rate versus the disk mass and a weaker dependency versus the star mass. Coupled with observed similar conclusions, we derived that the disk mass is scaling as M*1.6.

The partitioning of the inner and outer solar system by a structured protoplanetary disk

2020 ◽  
Author(s):  
Ramon Brasser ◽  
Stephen Mojzsis
Keyword(s):  
Solar System ◽  
Protoplanetary Disk ◽  
Giant Planets ◽  
Iron Meteorites ◽  
Effective Barrier ◽  
Dynamical Simulations ◽  
Pressure Maximum ◽  
Ringed Structure ◽  
Isotopic Anomalies ◽  
Multiple Rings

<p>Mass-independent isotopic anomalies in planets and meteorites define two cosmochemically distinct regions: the carbonaceous and non-carbonaceous meteorites, implying that the non-carbonaceous (terrestrial) and carbonaceous (jovian) reservoirs were kept separate during and after planet formation. The iron meteorites show a similar dichotomy.</p><p>The formation of Jupiter is widely invoked to explain this compositional dichotomy by acting as an effective barrier between the two reservoirs. Jupiter’s solid kernel possibly grew to ~20 Mearth in ~1 Myr from the accretion of sub meter-sized objects (termed “pebbles”), followed by slower accretion via planetesimals. Subsequent gas envelope contraction is thought to have led to Jupiter’s formation as a gas giant.</p><p>We show using dynamical simulations that the growth of Jupiter from pebble accretion is not fast enough to be responsible for the inferred separation of the terrestrial and jovian reservoirs. We propose instead that the dichotomy was caused by a pressure maximum in the disk near Jupiter’s location, which created a ringed structure such as those detected by the Atacama Large Millimeter/submillimeter Array(ALMA). One or multiple such long-lived pressure maxima almost completely prevented pebbles from the jovian region reaching the terrestrial zone, maintaining a compositional partition between the two regions. We thus suggest that our young solar system’s protoplanetary disk developed at least one and likely multiple rings, which potentially triggered the formation of the giant planets [1].</p><p><br>[1] Brasser, R. and Mojzsis, S.J. (2020) Nature Astronomy doi: 10.1038/s41550-019-0978-6</p>

scholarly journals Fossilized condensation lines in the Solar System protoplanetary disk

Icarus ◽  
2016 ◽  
Vol 267 ◽  
pp. 368-376 ◽  
Author(s):  
A. Morbidelli ◽  
B. Bitsch ◽  
A. Crida ◽  
M. Gounelle ◽  
T. Guillot ◽  
...  
Keyword(s):  
Solar System ◽  
Protoplanetary Disk
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