On the Effect of Giant Planets on the Scattering of Parent Bodies of Iron Meteorite From the Terrestrial Planet Region Into the Asteroid Belt: A Concept Study

Haghighipour, Nader; Scott, E. R. D.

doi:10.1088/0004-637x/749/2/113

Cited by 28 publications

(7 citation statements)

References 48 publications

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“…Their differentiation was a consequence of the early accretion and melting due to the decay of 26 Al. Numerical models estimate the accretion time as within 0.3–1.5 Ma after CAIs (Bland & Ciesla, ; Haghighipour & Scott, ; Kruijer et al, ; Qin et al, ). Despite the large number of differentiated parent bodies they are not observed in the asteroid belt.…”

Section: Differentiation Of Planetesimals and Previous Modelsmentioning

confidence: 99%

Multistage Core Formation in Planetesimals Revealed by Numerical Modeling and Hf‐W Chronometry of Iron Meteorites

et al. 2018

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Iron meteorites provide some of the most direct insights into the processes and timescales of core formation in planetesimals. Of these, group IVB irons stand out by having one of the youngest 182Hf‐182W model ages for metal segregation (2.9 ± 0.6 Ma after solar system formation), as well as the lowest bulk sulfur content and hence highest liquidus temperature. Here, using a new model for the internal evolution of the IVB parent body, we show that a single stage of metal‐silicate separation cannot account for the complete melting of pure Fe metal at the relatively late time given by the Hf‐W model age. Instead, a complex metal‐silicate separation scenario is required that includes migration of partial silicate melts, formation of a shallow magma ocean, and core formation in two distinct stages of metal segregation. In the first stage, a protocore formed at ≈1.5 Ma via settling of metal particles in a mantle magma ocean, followed by metal segregation from a shallow magma ocean at ≈5.4 Ma. As these stages of metal segregation occurred at different times, the two metal fractions had different 182W compositions. Consequently, the final 182W composition of the IVB core does not correspond to a single differentiation event, but represents the average composition of early‐ and late‐segregated core fractions. Our best fit model indicates an ≈100 km radius for the IVB parent body and provides an accretion age of ≈0.1–0.5 Ma after solar system formation. The computed solidification time is, furthermore, consistent with the Re‐Os age for crystallization of the IVB core.

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Section: Differentiation Of Planetesimals and Previous Modelsmentioning

confidence: 99%

Multistage Core Formation in Planetesimals Revealed by Numerical Modeling and Hf‐W Chronometry of Iron Meteorites

et al. 2018

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“…See Haghighipour & Scott (2012) for the possibility of scattering of planetesimals from inner orbits to outer regions.…”

Section: Numerical Simulationsmentioning

confidence: 99%

“…This could be attributed to the fact that in these simulations, the disk model B contains only planetary embryos which, unlike planetesimals, are not easily excited by Saturn's ν 6 secular resonance [the embryo-embryo interactions around 2.0-2.5 AU in these simulations neutralize the effect of the ν 6 resonance. See Levison & Agnor (2003) and Haghighipour et al (2012) for more details]. Since the embryos past 2.5 AU carry 5% water, a single collision with a proto-planet in HZ can deliver substantial amount of water to a planet in that region.…”

Section: Water Content Of the Final Planetsmentioning

confidence: 99%

“…secular resonance [the embryo-embryo interactions around 2.0-2.5 AU in these simulations neutralize the effect of the ν 6 resonance. See Levison & Agnor (2003) and Haghighipour et al (2012) for more details]. Since the embryos past 2.5 AU carry 5% water, a single collision with a proto-planet in HZ can deliver substantial amount of water to a planet in that region.…”

Section: Water Content Of the Final Planetsmentioning

confidence: 99%

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A Compound Model for the Origin of Earth's Water

Izidoro

Torres

Winter

et al. 2013

ApJ

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One of the most important subjects of debate in the formation of the solar system is the origin of Earth's water. Comets have long been considered as the most likely source of the delivery of water to Earth. However, elemental and isotopic arguments suggest a very small contribution from these objects. Other sources have also been proposed, among which, local adsorption of water vapor onto dust grains in the primordial nebula and delivery through planetesimals and planetary embryos have become more prominent. However, no sole source of water provides a satisfactory explanation for Earth's water as a whole. In view of that, using numerical simulations, we have developed a compound model incorporating both the principal endogenous and exogenous theories, and investigating their implications for terrestrial planet formation and water-delivery. Comets are also considered in the final analysis, as it is likely that at least some of Earth's water has cometary origin. We analyze our results comparing two different water distribution models, and complement our study using D/H ratio, finding possible relative contributions from each source, focusing on planets formed in the habitable zone. We find that the compound model play an important role by showing more advantage in the amount and time of water-delivery in Earth-like planets.

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“…As expected, similar to the classical model (section 2.2.3), the ν 5 resonance does not have a significant contribution in removing mass from its surrounding and the radial mixing of disk material. The scattering of objects in the region around this resonance is primarily due to their interactions with planetary embryos (Bottke et al 2006;Haghighipour and Scott 2012). Results of our simulations show that as Earthand Venus-analogs form and accrete protoplanetary bodies, the effect of this resonance becomes weaker till it finally disappears when Earth and Venus are fully formed.…”

Section: Disk-mass Removalmentioning

confidence: 83%

Formation of terrestrial planets in disks with different surface density profiles

Haghighipour

Winter

2015

Celest Mech Dyn Astr

Self Cite

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We present the results of an extensive study of the final stage of terrestrial planet formation in disks with different surface density profiles and for different orbital configurations of Jupiter and Saturn. We carried out simulations in the context of the classical model with disk surface densities proportional to r −0.5 , r −1 and r −1.5 , and also using partially depleted, non-uniform disks as in the recent model of Mars formation by Izidoro et al (2014). The purpose of our study is to determine how the final assembly of planets and their physical properties are affected by the total mass of the disk and its radial profile. Because as a result of the interactions of giant planets with the protoplanetary disk, secular resonances will also play important roles in the orbital assembly and properties of the final terrestrial planets, we will study the effect of these resonances as well. In that respect, we divide this study into two parts. When using a partially depleted disk (Part 1), we are particularly interested in examining the effect of secular resonances on the formation of Mars and orbital stability of terrestrial planets. When using the disk in the classical model (Part 2), our goal is to determine trends that may exist between the disk surface density profile and the final properties of terrestrial planets. In the context of the depleted disk model, results of our study show that in general, the ν 5 resonance does not have a significant effect on the dynamics of planetesimals and planetary embryos, and the final orbits of terrestrial planets. However, ν 6 and ν 16 resonances play important roles in clearing their affecting areas. While these resonances do not alter the orbits of Mars and other terrestrial planets, they strongly deplete the region of the asteroid belt ensuring that no additional mass will be scattered into the accretion zone of Mars so that it can maintain its mass and orbital stability. In the context of the classical model, the effects of these resonances are stronger in disks with less steep surface density profiles. Our results indicate that when considering the classical model (Part 2), the final planetary systems do not seem to show a trend between the disk surface density profile and the mean number of the final planets, their masses, time of formation, and distances to the central star. Some small correlations were observed where, for instance, in disks with steeper surface density profiles, the final planets were drier, or their water contents decreased when Saturn was added to the simulations. However, in general, the final orbital and physical properties of terrestrial planets seem to vary from one system to another and depend on the mass of the disk, the spatial distribution of protoplanetary bodies (i.e., disk surface density profile), and the initial orbital configuration of giant planets. We present results of our simulations and discuss their implications for the formation of Mars and other terrestrial planets, as well as the physical properties of these objects...

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On the Effect of Giant Planets on the Scattering of Parent Bodies of Iron Meteorite From the Terrestrial Planet Region Into the Asteroid Belt: A Concept Study

Cited by 28 publications

References 48 publications

Multistage Core Formation in Planetesimals Revealed by Numerical Modeling and Hf‐W Chronometry of Iron Meteorites

Multistage Core Formation in Planetesimals Revealed by Numerical Modeling and Hf‐W Chronometry of Iron Meteorites

A Compound Model for the Origin of Earth's Water

Formation of terrestrial planets in disks with different surface density profiles

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