Physical properties of terrestrial planets and water delivery in the habitable zone using <i>N</i>-body simulations with fragmentation

Dugaro, A.; Elía, G. C. de; Darriba, Luciano Ariel

doi:10.1051/0004-6361/201936061

Cited by 13 publications

(39 citation statements)

References 45 publications

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“…The authors compared two sets of identical initial conditions and performed a series of N-body simulations with and without fragmentation. The results derived in Dugaro et al (2019) are consistent with those obtained by Chambers (2013) and Genda et al (2012).…”

Section: Introductionsupporting

confidence: 90%

“…Recently, in Dugaro et al (2019), we presented an N-body code called D3 that allows planetary fragmentation for gravitydomain bodies based on the works of Chambers (1999Chambers ( , 2013, Leinhardt & Stewart (2012), Genda et al (2012), andMustill et al (2018). The authors studied terrestrial planet formation on a protoplanetary disk, hosted by a solar-type star, and the presence of Jupiter and Saturn analogs.…”

Section: Introductionmentioning

confidence: 99%

“…They concluded that the cumulative effect of several hit-and-run collisions could efficiently strip off volatile layers of protoplanets. Driven by this, Dugaro et al (2019) studied the water delivery in planets formed in the habitable zone (HZ), using the mantle stripping models derived by Marcus et al (2010) in their N-body simulations with fragmentation. The authors showed that fragmentation is not a barrier for the surviving of water worlds in the HZ, and fragments may be important in the final water content of the potentially habitable terrestrial planets formed in situ.…”

Section: Introductionmentioning

confidence: 99%

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Water worlds in N-body simulations with fragmentation in systems without gaseous giants

Dugaro

Elía

Darriba

2020

A&A

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Aims. We analyze the formation and evolution of terrestrial-like planets around solar-type stars in the absence of gaseous giants. In particular, we focus on the physical and dynamical properties of those that survive in the system’s habitable zone (HZ). This investigation is based on a comparative study between N-body simulations that include fragmentation and others that consider all collisions as perfect mergers. Methods. We use an N-body code, presented in a previous paper, that allows planetary fragmentation. We carry out three sets of 24 simulations for 400 Myr. Two sets are developed adopting a model that includes hit-and-run collisions and planetary fragmentation, each one with different values of the individual minimum mass allowed for the fragments. For the third set, we considered that all collisions lead to perfect mergers. Results. The planetary systems produced in N-body simulations with and without fragmentation are broadly similar, though with some differences. In simulations with fragmentation, the formed planets have lower masses since part of them is distributed among collisional fragments. Additionally, those planets presented lower eccentricities, presumably due to dynamical friction with the generated fragments. Lastly, perfect mergers and hit-and-run collisions are the most common outcome. Regardless of the collisional treatment adopted, most of the planets that survive in the HZ start the simulation beyond the snow line, having very high final water contents. Such planets are called water worlds. The fragments’ contribution to their final mass and water content is negligible. Finally, the individual minimum mass for fragments may play an important role in the planets’ collisional history. Conclusions. Collisional models that incorporate fragmentation and hit-and-run collisions lead to a more detailed description of the physical properties of the terrestrial-like planets formed. We conclude that planetary fragmentation is not a barrier to the formation of water worlds in the HZ. The results shown in this work suggest that further refinement is necessary to have a more realistic model of planetary formation.

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Section: Introductionsupporting

confidence: 90%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Water worlds in N-body simulations with fragmentation in systems without gaseous giants

Dugaro

Elía

Darriba

2020

A&A

Self Cite

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“…In agreement with our results, that study found that most Mars analogs accrete more slowly than the exponential growth curve of Dauphas & Pourmand (2011) and proposed various dynamical methods to make them grow more quickly. These include the implementation of non-perfect merging between colliding protoplanets, an effect which slightly prolongs Earth's accretion (e.g., Chambers, 2013;Dwyer et al, 2015) but could potentially form Mars more quickly via fragmentation (Kobayashi & Dauphas, 2013;Dugaro et al, 2019). N-body studies of "pebble accretion" disagree on whether that regime promotes (Levison et al, 2015;Matsumura et al, 2017) or discourages (Voelkel et al, 2021) the formation of small terrestrial planets.…”

Section: Other N-body Approachesmentioning

confidence: 99%

Timing of Martian Core Formation from Models of Hf–W Evolution Coupled with N-body Simulations

Brennan¹,

Fischer²,

Nimmo³

et al. 2022

Preprint

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Determining how and when Mars formed has been a long-standing challenge for planetary scientists. The size and orbit of Mars are difficult to reproduce in classical simulations of planetary accretion, and this has inspired models of inner solar system evolution that are tuned to produce Mars-like planets. However, such models are typically not coupled to geochemical constraints. Analyses of Martian meteorites using the extinct hafnium-tungsten (Hf-W) radioisotopic system, which is sensitive to the timing of core formation, have indicated that the Martian core formed within a few million years of the solar system itself. This has been interpreted to suggest that, unlike Earth's protracted accretion, Mars grew to its modern size very rapidly. These arguments, however, generally rely on simplified growth histories for Mars. Here, we combine realistic accretionary histories from a large number of N-body simulations with calculations of metal-silicate partitioning and Hf-W isotopic evolution during core formation to constrain the range of conditions that could have produced Mars.

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“…Such interactions produce orbits that cross each other, which results in successively close encounters between them which, in turn, lead to collisions among them, ejections from the system, and collisions with the central star. Several works have shown that collisions between gravity-domained bodies yield different outcomes depending on the target size, projectile size, impact velocity, and impact angle (Leinhardt & Stewart 2012;Chambers 2013;Quintana et al 2016;Dugaro et al 2019). In the present study, all collisions were treated as perfect mergers, conserving the total mass of the interacting bodies in each impact event.…”

Section: N-body Experiments: Characterisation Parameters and Initial Conditionsmentioning

confidence: 99%

GJ 273: on the formation, dynamical evolution, and habitability of a planetary system hosted by an M dwarf at 3.75 parsec

Pozuelos

Suárez

Elía

et al. 2020

A&A

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Context. Planets orbiting low-mass stars such as M dwarfs are now considered a cornerstone in the search for planets with the potential to harbour life. GJ 273 is a planetary system orbiting an M dwarf only 3.75 pc away, which is composed of two confirmed planets, GJ 273b and GJ 273c, and two promising candidates, GJ 273d and GJ 273e. Planet GJ 273b resides in the habitable zone. Currently, due to a lack of observed planetary transits, only the minimum masses of the planets are known: Mb sin ib = 2.89 M⊕, Mc sin ic = 1.18 M⊕, Md sin id = 10.80 M⊕, and Me sin ie = 9.30 M⊕. Despite its interesting character, the GJ 273 planetary system has been poorly studied thus far. Aims. We aim to precisely determine the physical parameters of the individual planets, in particular, to break the mass–inclination degeneracy to accurately determine the mass of the planets. Moreover, we present a thorough characterisation of planet GJ 273b in terms of its potential habitability. Methods. First, we explored the planetary formation and hydration phases of GJ 273 during the first 100 Myr. Secondly, we analysed the stability of the system by considering both the two- and four-planet configurations. We then performed a comparative analysis between GJ 273 and the Solar System and we searched for regions in GJ 273 which may harbour minor bodies in stable orbits, that is, the main asteroid belt and Kuiper belt analogues. Results. From our set of dynamical studies, we find that the four-planet configuration of the system allows us to break the mass–inclination degeneracy. From our modelling results, the masses of the planets are unveiled as: 2.89 ≤ Mb ≤ 3.03 M⊕, 1.18 ≤ Mc ≤ 1.24 M⊕, 10.80 ≤ Md ≤ 11.35 M⊕, and 9.30 ≤ Me ≤ 9.70 M⊕. These results point to a system that is likely to be composed of an Earth-mass planet, a super-Earth and two mini-Neptunes. Based on planetary formation models, we determine that GJ 273b is likely an efficient water captor while GJ 273c is probably a dry planet. We find that the system may have several stable regions where minor bodies might reside. Collectively, these results are used to offer a comprehensive discussion about the habitability of GJ 273b.

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Physical properties of terrestrial planets and water delivery in the habitable zone using N-body simulations with fragmentation

Cited by 13 publications

References 45 publications

Water worlds in N-body simulations with fragmentation in systems without gaseous giants

Water worlds in N-body simulations with fragmentation in systems without gaseous giants

Timing of Martian Core Formation from Models of Hf–W Evolution Coupled with N-body Simulations

GJ 273: on the formation, dynamical evolution, and habitability of a planetary system hosted by an M dwarf at 3.75 parsec

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