A Compound model for the origin of Earth's water

Abstract

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.

Accepted for publication in The Astrophysical Journal

References in corpus (7)

• A low mass for Mars from Jupiter's early gas-driven migration
• The origins and concentrations of water, carbon, nitrogen and noble gases on Earth
• Constraints on the mass of a habitable planet with water of nebular origin
• Habitable Planet Formation in Binary-Planetary Systems
• The 16OH/18OH and OD/OH isotope ratios in comet C/2002 T7 (LINEAR)
• Water vapour and hydrogen in the terrestrial-planet-forming region of a protoplanetary disk
• 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 in corpus (41)

• Water Delivery and Giant Impacts in the 'Grand Tack' Scenario
• Interstellar Interlopers: Number Density and Origins of 'Oumuamua-like Objects
• The Delivery of Water During Terrestrial Planet Formation
• Terrestrial Planet Formation Constrained by Mars and the Structure of the Asteroid Belt
• Chemo-dynamical deuterium fractionation in the early solar nebula: The origin of water on Earth and in asteroids and comets
• The Feeding Zones of Terrestrial Planets and Insights into Moon Formation
• Terrestrial Planet Formation in a protoplanetary disk with a local mass depletion: A successful scenario for the formation of Mars
• Terrestrial Planet Formation in the Presence of Migrating Super-earths
• Correlations between the stellar, planetary and debris components of exoplanet systems observed by $\text{Herschel}$
• The effect of planet-planet scattering on the survival of exomoons
• Solar System Physics for Exoplanet Research
• A smooth particle hydrodynamics code to model collisions between solid, self-gravitating objects
• The Asteroid Belt as a Relic From a Chaotic Early Solar System
• The Chemical Inventory of the Inner Regions of Planet-forming Disks -- The JWST/MINDS Program
• Near-Earth asteroids spectroscopic survey at Isaac Newton Telescope
• Setting the Stage: Planet formation and Volatile Delivery
• Transfer, loss and physical processing of water in hit-and-run collisions of planetary embryos
• Realistic collisional water transport during terrestrial planet formation: Self-consistent modeling by an N-body--SPH hybrid code
• Asteroid flux towards circumprimary habitable zones in binary star systems: I. Statistical Overview
• Formation of Terrestrial Planets in Disks with Different Surface Density Profiles
• Earths in Other Solar Systems N-body simulations: the Role of Orbital Damping in Reproducing the Kepler Planetary Systems
• Formation of Terrestrial Planets
• Triggering Sublimation-Driven Activity of Main Belt Comets
• Direct measurement of decimeter-sized rocky material in the Oort cloud
• Warm dust surface chemistry in protoplanetary disks. Formation of phyllosilicates
• Asteroid triple system 2001 SN263 : surfaces characteristics and dynamical environment
• Asteroid impacts on terrestrial planets: The effects of super-Earths and the role of the ${\nu }_6$ resonance
• Properties of the single Jovian planet population and the pursuit of Solar system analogues
• Photometric survey of 67 near-Earth objects
• Stable habitable zones of single Jovian planet systems
• Explaining Mercury via a single giant impact is highly unlikely
• In Situ Models for Planet Assembly around Cool stars
• Terrestrial-type planet formation: Comparing different types of initial conditions
• Building Terrestrial Planets: Why results of perfect-merging simulations are not quantitatively reliable approximations to accurate modeling of terrestrial planet formation
• (121514) 1999 UJ7: A primitive, slow-rotating Martian Trojan
• Residual Neural Networks for the Prediction of Planetary Collision Outcomes
• HyperScout-H: the hyperspectral imager for the ESA Hera mission
• On the formation of terrestrial planets between two massive planets: The case of 55 Cancri
• Analysis of the dynamics of a spacecraft in the vicinity of an asteroid binary system with equal masses
• The when and where of water in the history of the universe
• Surface Properties, Orbital Dynamics, and Thermophysical Modeling of the Primitive Asteroid (269) Justitia