Water transport throughout the TRAPPIST-1 system: the role of planetesimals
arXiv:2007.05366 · doi:10.1093/mnras/staa1833
Abstract
Observational data suggest that a belt of planetesimals is expected close to the snow line in protoplanetary disks. Assuming there is such a belt in TRAPPIST-1 system, we examine possibilities of water delivery to the planets via planetesimals from the belt. The study is accomplished by numerical simulations of dynamical evolution of a hypothetical planetesimal belt. Our results show that the inner part of the belt is dynamically unstable and planetesimals located in this region are quickly scattered away, with many of them entering the region around the planets. The main dynamical mechanism responsible for the instability are close encounters with the outermost planet Trappist-1h. A low-order mean-motion resonance 2:3 with Trappist-1h, located in the same region, also contributes to the objects transport. In our nominal model, the planets have received non-negligible amount of water, with the smallest amount of \% of the current Earth's water amount (EWA) being delivered to the planet 1b, while the planets Trappist-1e and Trappist-1g have received more than \% of the EWA. We have found that while the estimated efficiency of water transport to the planets is robust, the amount of water delivered to each planet may vary significantly depending on the initial masses and orbits of the planets. The estimated dynamical "half-lives" have shown that the impactors' source region should be emptied in less then 1~Myr. Therefore, the obtained results suggest that transport of planetesimals through the system preferably occurs during an early phase of the planetary system evolution.
arXiv comment12 pages, 8 figures; MNRAS, accepted for publication
References in corpus (58)
- Seven temperate terrestrial planets around the nearby ultracool dwarf star TRAPPIST-1
- The Mass Dependence Between Protoplanetary Disks and their Stellar Hosts
- Temperate Earth-sized planets transiting a nearby ultracool dwarf star
- A Major Asymmetric Dust Trap in a Transition Disk
- Core-Accretion Model Predicts Few Jovian-Mass Planets Orbiting Red Dwarfs
- A seven-planet resonant chain in TRAPPIST-1
- The nature of the TRAPPIST-1 exoplanets
- The Active Asteroids
- Detection of the Water Reservoir in a Forming Planetary System
- Water Delivery and Giant Impacts in the 'Grand Tack' Scenario
- Water loss from Earth-sized planets in the habitable zones of ultracool dwarfs: Implications for the planets of TRAPPIST-1
- Asteroid families classification: exploiting very large data sets
- A combined transmission spectrum of the Earth-sized exoplanets TRAPPIST-1 b and c
- Final Stages of Planet Formation
- Volatile carbon locking and release in protoplanetary disks. A study of TW Hya and HD 100546
- Modelling climate diversity, tidal dynamics and the fate of volatiles on TRAPPIST-1 planets
- N-body simulations of planetary accretion around M dwarf stars
- Growing the terrestrial planets from the gradual accumulation of sub-meter sized objects
- Formation of TRAPPIST-1 and other compact systems
- Evolved Climates and Observational Discriminants for the TRAPPIST-1 Planetary System
- On the Evolution of the Snow Line in Protoplanetary Discs
- Hybrid Symplectic Integrators for Planetary Dynamics
- Terrestrial Planet Formation in Disks with Varying Surface Density Profiles
- On the Age of the TRAPPIST-1 System
- The First Naked-Eye Superflare Detected from Proxima Centauri
- Volatile Delivery to Planets from Water-rich Planetesimals around Low Mass Stars
- Convergent Migration Renders TRAPPIST-1 Long-lived
- Predicting the Extreme Ultraviolet Radiation Environment of Exoplanets Around Low-Mass Stars: the TRAPPIST-1 System
- UV Surface Habitability of the TRAPPIST-1 System
- Pebble-driven planet formation for TRAPPIST-1 and other compact systems
- The Main Belt Comets and Ice in the Solar System
- Pebbles versus Planetesimals: The case of Trappist-1
- The TRAPPIST-1 system: Orbital evolution, tidal dissipation, formation and habitability
- Habitable Zones in the Universe
- Water delivery by pebble accretion to rocky planets in habitable zones in evolving disks
- Cometary impactors on the TRAPPIST-1 planets can destroy all planetary atmospheres and rebuild secondary atmospheres on planets f, g, h
- Planetesimal and Protoplanet Dynamics in a Turbulent Protoplanetary Disk: Ideal Unstratified Disks
- Asteroid Family Associations of Active Asteroids
- Tidal Heating and the Habitability of the TRAPPIST-1 Exoplanets
- Earth-like Habitats in Planetary Systems
- Secular Evolution of HD 12661: A System Caught at an Unlikely Time
- The habitability of stagnant-lid Earths around dwarf stars
- Chaotic Transport and Chronology of Complex Asteroid Families
- Reconstructing the size distribution of the primordial Main Belt
- Habitability in Different Milky Way Stellar Environments: a Stellar Interaction Dynamical Approach
- A dark asteroid family in the Phocaea region
- Updated Masses for the TRAPPIST-1 Planets
- A Coupled Analysis of Atmospheric Mass Loss and Tidal Evolution in XUV Irradiated Exoplanets: the TRAPPIST-1 Case Study
- Assessing the influence of the solar orbit on terrestrial biodiversity
- Water delivery to the TRAPPIST-1 planets
- Exploring plausible formation scenarios for the planet candidate orbiting Proxima Centauri
- Chaotic diffusion of the Vesta family induced by close encounters with massive asteroids
- Spectral properties and geology of bright and dark material on dwarf planet Ceres
- Advanced Aspects of the Galactic Habitability
- Astrometric Constraints on the Masses of Long-Period Gas Giant Planets in the TRAPPIST-1 Planetary System
- The Dynamical History Of 2060 Chiron And Its Proposed Ring System
- WASP-92, WASP-93 and WASP-118: Transit timing variations and long-term stability of the systems
- Exocomets in the 47 UMa System: Theoretical Simulations including Water Transport
Cited by in corpus (3)
- An upper limit on late accretion and water delivery in the Trappist-1 exoplanet system
- Mercury and OrbFit packages for the numerical integration of planetary systems: implementation of the Yarkovsky and YORP effects
- Habitable planet formation around low-mass stars: Rapid accretion, rapid debris removal and the essential contribution of external giants