Terrestrial planets in high-mass disks without gas giants

Elía, G. C. de; Guilera, O. M.; Brunini, A.

doi:10.1051/0004-6361/201321304

Cited by 22 publications

(34 citation statements)

References 60 publications

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“…This work complements that developed by de Elía et al (2013), which indicated that systems without gas giants that harbor super-Earths or Neptune-mass planets on wide orbits around solar-type stars are of astrobiological interest. These theoretical works offer a relevant contribution for current and future observational surveys because they allow us to determine which planetary systems are of special interest.…”

Section: Discussionsupporting

confidence: 79%

“…For example, planets with very eccentric orbits may pass most of their periods outside the HZ, not allowing long times of permanent liquid water on their surfaces. To avoid this problem we considered that a planet is in the HZ and can hold liquid water if it has a perihelion q ≥ 0.8 AU and a aphelion Q ≤ 1.5 AU (de Elía et al 2013). These criteria allowed us to distinguish potentially habitable planets.…”

Section: Resultsmentioning

confidence: 99%

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Diversity of planetary systems in low-mass disks

Ronco

Elía

2014

A&A

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Context. Several studies, observational and theoretical, suggest that planetary systems with only rocky planets are the most common in the Universe. Aims. We study the diversity of planetary systems that might form around Sun-like stars in low-mass disks without gas-giant planets. We focus especially on the formation process of terrestrial planets in the habitable zone (HZ) and analyze their water contents with the goal to determine systems of astrobiological interest. In addition, we study the formation of planets on wide orbits because they can be detected with the microlensing technique. Methods. N-body simulations of high resolution were developed for a wide range of surface density profiles. A bimodal distribution of planetesimals and planetary embryos with different physical and orbital configurations was used to simulate the planetary accretion process. The surface density profile combines a power law for the inside of the disk of the form r −γ , with an exponential decay to the outside. We performed simulations adopting a disk of 0.03 M and values of γ = 0.5, 1 and 1.5. Results. All our simulations form planets in the HZ with different masses and final water contents depending on the three different profiles. For γ = 0.5, our simulations produce three planets in the HZ with masses ranging from 0.03 M ⊕ to 0.1 M ⊕ and water contents between 0.2 and 16 Earth oceans (1 Earth ocean = 2.8 × 10 −4 M ⊕ ). For γ = 1, three planets form in the HZ with masses between 0.18 M ⊕ and 0.52 M ⊕ and water contents from 34 to 167 Earth oceans. Finally, for γ = 1.5, we find four planets in the HZ with masses ranging from 0.66 M ⊕ to 2.21 M ⊕ and water contents between 192 and 2326 Earth oceans. This profile shows distinctive results because it is the only one of those studied here that leads to the formation of water worlds. Conclusions. Since planetary systems with γ = 1 and 1.5 present planets in the HZ with suitable masses to retain a long-lived atmosphere and to maintain plate tectonics, they seem to be the most promising candidates to be potentially habitable. Particularly, these systems form Earths and Super-Earths of at least 3 M ⊕ around the snow line, which can be discovered by the microlensing technique.

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Section: Discussionsupporting

confidence: 79%

Section: Resultsmentioning

confidence: 99%

Diversity of planetary systems in low-mass disks

Ronco

Elía

2014

A&A

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“…Because super-Earths can form around Solar-type stars out to 5 au (de Elía et al 2013), formation of Earth-like planets around more massive stars should take place beyond 5 au. In fact, the snow or ice line -a concept often used to demarcate the formation of terrestrial from giant planets -changes distance with time, but can reach a distance of up to 10 au after 10 5 yr for the stellar masses we considered (Kennedy & Kenyon 2008).…”

Section: Planetary Mass and Orbitsmentioning

confidence: 99%

Detectable close-in planets around white dwarfs through late unpacking

Veras

Gänsicke

2014

Monthly Notices of the Royal Astronomical Society

119

129

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Although 25%-50% of white dwarfs (WDs) display evidence for remnant planetary systems, their orbital architectures and overall sizes remain unknown. Vibrant close-in (≃ 1R ⊙ ) circumstellar activity is detected at WDs spanning many Gyrs in age, suggestive of planets further away. Here we demonstrate how systems with 4 and 10 closely-packed planets that remain stable and ordered on the main sequence can become unpacked when the star evolves into a WD and experience pervasive inward planetary incursions throughout WD cooling. Our full-lifetime simulations run for the age of the Universe and adopt main sequence stellar masses of 1.5M ⊙ , 2.0M ⊙ and 2.5M ⊙ , which correspond to the mass range occupied by the progenitors of typical present-day WDs. These results provide (i) a natural way to generate an ever-changing dynamical architecture in post-main-sequence planetary systems, (ii) an avenue for planets to achieve temporary close-in orbits that are potentially detectable by transit photometry, and (iii) a dynamical explanation for how residual asteroids might pollute particularly old WDs.

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“…We applied the same methodology as in de Elía et al (2013). We determined the mass of the disk to be used in our simulations calculating the in situ formation of an embryo located just beyond the snow line (∼ 3 au) using our model of giant planet formation (Guilera et al 2010).…”

Section: Applicationmentioning

confidence: 99%

Migrating Jupiter up to the habitable zone: Earth-like planet formation and water delivery

Darriba

Elía

Guilera

et al. 2017

A&A

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Context. Several observational works have shown the existence of Jupiter-mass planets covering a wide range of semi-major axes around Sun-like stars. Aims. We aim to analyse the planetary formation processes around Sun-like stars that host a Jupiter-mass planet at intermediate distances ranging from ∼1 au to 2 au. Our study focusses on the formation and evolution of terrestrial-like planets and water delivery in the habitable zone (HZ) of the system. Our goal is also to analyse the long-term dynamical stability of the resulting systems. Methods. A semi-analytic model was used to define the properties of a protoplanetary disk that produces a Jupiter-mass planet around the snow line, which is located at ∼2.7 au for a solar-mass star. Then, it was used to describe the evolution of embryos and planetesimals during the gaseous phase up to the formation of the Jupiter-mass planet, and we used the results as the initial conditions to carry out N-body simulations of planetary accretion. We developed sixty N-body simulations to describe the dynamical processes involved during and after the migration of the gas giant. Results. Our simulations produce three different classes of planets in the HZ: 'water worlds', with masses between 2.75 M ⊕ and 3.57 M ⊕ and water contents of 58 % and 75 % by mass, terrestrial-like planets, with masses ranging from 0.58 M ⊕ to 3.8 M ⊕ and water contents less than 1.2 % by mass, and 'dry worlds', simulations of which show no water. A relevant result suggests the efficient coexistence in the HZ of a Jupiter-mass planet and a terrestrial-like planet with a percentage of water by mass comparable to the Earth. Moreover, our study indicates that these planetary systems are dynamically stable for at least 1 Gyr. Conclusions. Systems with a Jupiter-mass planet located at 1.5 au -2 au around solar-type stars are of astrobiological interest. These systems are likely to harbour terrestrial-like planets in the HZ with a wide diversity of water contents.

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Terrestrial planets in high-mass disks without gas giants

Cited by 22 publications

References 60 publications

Diversity of planetary systems in low-mass disks

Diversity of planetary systems in low-mass disks

Detectable close-in planets around white dwarfs through late unpacking

Migrating Jupiter up to the habitable zone: Earth-like planet formation and water delivery

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