Water worlds in N-body simulations with fragmentation in systems without gaseous giants
arXiv:2008.03594 · doi:10.1051/0004-6361/202037619
Abstract
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 study is based on a comparative study between N-body simulations that include fragmentation and others that consider all collisions as perfect mergers. 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. The systems produced in N-body simulations with and without fragmentation are broadly similar, with some differences. In runs with fragmentation, the formed planets have lower masses since part it is distributed amongst collisional fragments. Additionally, those planets presented lower eccentricities, presumably due to dynamical friction with the generated fragments. 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. The fragments' contribution to their mass and water content is negligible. Finally, the individual minimum mass for fragments may play an important role in the planets' collisional history. 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.
References in corpus (51)
- Habitable Zones Around Main-Sequence Stars: New Estimates
- Towards a Deterministic Model of Planetary Formation I: a Desert in the Mass and Semi Major Axis Distributions of Extra Solar Planets
- The Keck Planet Search: Detectability and the Minimum Mass and Orbital Period Distribution of Extrasolar Planets
- Rapid growth of gas-giant cores by pebble accretion
- The effect of gas drag on the growth of protoplanets -- Analytical expressions for the accretion of small bodies in laminar disks
- Extrasolar planet population synthesis I: Method, formation tracks and mass-distance distribution
- Abundances of the elements in the solar system
- Building the Terrestrial Planets: Constrained Accretion in the Inner Solar System
- Particle Clumping and Planetesimal Formation Depend Strongly on Metallicity
- Protoplanetary Disk Structures in Ophiuchus II: Extension to Fainter Sources
- Collisions between Gravity-Dominated Bodies: 2. The Diversity of Impact Outcomes during the End Stage of Planet Formation
- Collisions Between Gravity-Dominated Bodies: 1. Outcome Regimes and Scaling Laws
- Breaking the Chains: Hot Super-Earth systems from migration and disruption of compact resonant chains
- High-resolution simulations of the final assembly of Earth-like planets 1: terrestrial accretion and dynamics
- On the diversity and statistical properties of protostellar discs
- The structure of protoplanetary discs around evolving young stars
- Super-Earth Atmospheres: Self-Consistent Gas Accretion and Retention
- Formation of planetary systems by pebble accretion and migration: How the radial pebble flux determines a terrestrial-planet or super-Earth growth mode
- The Ophiuchus DIsc Survey Employing ALMA (ODISEA) - I : project description and continuum images at 28 au resolution
- Toward a Deterministic Model of Planetary Formation VII: Eccentricity Distribution of Gas Giants
- Observed Properties of Extrasolar Planets
- Challenges in Planet Formation
- The radial dependence of pebble accretion rates: A source of diversity in planetary systems I. Analytical formulation
- Merging Criteria for Giant Impacts of Protoplanets
- Physical properties of dusty protoplanetary disks in Lupus: evidence for viscous evolution?
- Super-Earth masses sculpted by pebble isolation around stars of different masses
- The Frequency of Giant impacts on Earth-like Worlds
- Migration-driven diversity of super-Earth compositions
- The early instability scenario: terrestrial planet formation during the giant planet instability, and the effect of collisional fragmentation
- Erosion and the limits to planetesimal growth
- Compositional evolution during rocky protoplanet accretion
- Rocky super-Earths or waterworlds: the interplay of planet migration, pebble accretion and disc evolution
- A Collisional Origin to Earth's Non-chondritic Composition?
- Water/Icy Super-Earths: Giant Impacts and Maximum Water Content
- Planetesimals to Terrestrial Planets: collisional evolution amidst a dissipating gas disk
- Formation of solar system analogs I: looking for initial conditions through a population synthesis analysis
- Forming Circumbinary Planets: N-body Simulations of Kepler-34
- A new and simple prescription for planet orbital migration and eccentricity damping by planet-disc interactions based on dynamical friction
- Realistic On-The-Fly Outcomes of Planetary Collisions: Machine Learning Applied to Simulations of Giant Impacts
- Transfer, loss and physical processing of water in hit-and-run collisions of planetary embryos
- Dynamical Constraints on Mercury's Collisional Origin
- Giant planet effects on terrestrial planet formation and system architecture
- Constraining the Formation of the Four Terrestrial Planets in the Solar System
- Planetary formation and water delivery in the habitable zone around solar-type stars in different dynamical environments
- The dynamical evolution of transiting planetary systems including a realistic collision prescription
- Role of gaseous giants in the dynamical evolution of terrestrial planets and water delivery in the habitable zone
- Diversity of planetary systems in low-mass disks: Terrestrial-type planet formation and water delivery
- Collisional Fragmentation is Not a Barrier to Close-in Planet Formation
- Migrating Jupiter up to the habitable zone: Earth-like planet formation and water delivery
- Importance of Giant Impact Ejecta for Orbits of Planets Formed during the Giant Impact Era
- Physical properties of terrestrial planets and water delivery in the habitable zone using N-body simulations with fragmentation