Probabilities of collisions of bodies ejected from forming Earth with the terrestrial planets
arXiv:2411.04218 · doi:10.1016/j.icarus.2024.116341
Abstract
The motion of bodies ejected from the Earth was studied, and the probabilities of collisions of such bodies with the present terrestrial planets were calculated. The dependences of these probabilities on velocities, angles and points of ejection of bodies were studied. These dependences can be used in the models with different distributions of ejected material. On average, about a half and less than 10\% of initial ejected bodies remained moving in elliptical orbits in the Solar System after 10 and 100 Myr, respectively. A few ejected bodies collided with planets after 250 Myr. As dynamical lifetimes of bodies ejected from the Earth can reach hundreds of million years, a few percent of bodies ejected at the Chicxulub and Popigai events about 36-65 Myr ago can still move in the zone of the terrestrial planets and have small chances to collide with planets, including the Earth. The fraction of ejected bodies that collided with the Earth was greater for smaller ejection velocity. The fractions of bodies delivered to the Earth and Venus probably did not differ much for these planets and were about 0.2-0.3 each. Such obtained results testify in favour of that the upper layers of the Earth and Venus can contain similar material. The fractions of bodies ejected from the Earth that collided with Mercury and Mars did not exceed 0.08 and 0.025, respectively. The fractions of bodies collided with Jupiter were of the order of 0.001. In most calculations the fraction of bodies collided with the Sun was between 0.2 and 0.5. Depending on parameters of ejection, the fraction of bodies ejected into hyperbolic orbits could vary from 0 to 1. Small fractions of material ejected from the Earth can be found on other terrestrial planets and Jupiter, as the ejected bodies could collide with these planets. Bodies ejected from the Earth could deliver organic material to other celestial objects, e.g. to Mars.
arXiv comment24 pages, 4 figures
References in corpus (49)
- A low mass for Mars from Jupiter's early gas-driven migration
- Building Terrestrial Planets
- Making other Earths: Dynamical Simulations of Terrestrial Planet Formation and Water Delivery
- Building the Terrestrial Planets: Constrained Accretion in the Inner Solar System
- Accretion and differentiation of the terrestrial planets with implications for the compositions of early-formed Solar System bodies and accretion of water
- High-resolution simulations of the final assembly of Earth-like planets 1: terrestrial accretion and dynamics
- Dynamics of the giant planets of the solar system in the gaseous proto-planetary disk and relationship to the current orbital architecture
- Water Delivery and Giant Impacts in the 'Grand Tack' Scenario
- A Sawtooth-like Timeline for the First Billion Year of Lunar Bombardment
- Formation of Kuiper Belt Binaries by Gravitational Collapse
- Evidence from the asteroid belt for a violent past evolution of Jupiter's orbit
- Mars' Growth Stunted by an Early Giant Planet Instability
- From planetesimals to terrestrial planets: N-body simulations including the effects of nebular gas and giant planets
- Multiple Impact Origin for the Moon
- Lunar and Terrestrial Planet Formation in the Grand Tack Scenario
- Tidal evolution of the Moon from a high-obliquity, high-angular-momentum Earth
- Rummaging through Earth's attic for remains of ancient life
- The early instability scenario: terrestrial planet formation during the giant planet instability, and the effect of collisional fragmentation
- Terrestrial Planet Formation in a protoplanetary disk with a local mass depletion: A successful scenario for the formation of Mars
- On the Origin of Earth's Moon
- Mercurian impact ejecta: Meterorites and mantle
- The Role of Early Giant Planet Instability in the Terrestrial Planet Formation
- Modeling the Historical Flux of Planetary Impactors
- Early Bombardment of the Moon: Connecting the Lunar Crater Record to the Terrestrial Planet Formation
- The terrestrial planet formation paradox inferred from high-resolution N-body simulations
- Comet and Asteroid Hazard to the Terrestrial Planets
- Delivery of water and volatiles to the terrestrial planets and the Moon
- Migration processes in the Solar System and their role in the evolution of the Earth and planets
- Migration of Trans-Neptunian Objects to the Terrestrial Planets
- Dynamics of escaping Earth ejecta and their collision probability with different Solar System bodies
- Migration of Small Bodies and Dust to Near-Earth Space
- Migration of Jupiter-Family Comets and Resonant Asteroids to Near-Earth Space
- The early instability scenario: Mars' mass explained by Jupiter's orbit
- A race against the clock: Constraining the timing of cometary bombardment relative to Earth's growth
- Exogenous delivery of water to Mercury
- Collision Chains among the Terrestrial Planets. II. An Asymmetry between Earth and Venus
- Formation of Lunar Basins from Impacts of Leftover Planetesimals
- Migration of Interplanetary Dust
- Probabilities of collisions of planetesimals from different regions of the feeding zone of the terrestrial planets with the forming planets and the Moon
- Formation of the Earth and Moon: Influence of Small Bodies
- Formation of trans-Neptunian satellite systems at the stage of condensations
- Analytical formulation of lunar cratering asymmetries
- Formation of embryos of the Earth and the Moon from the common rarefied condensation and their subsequent growth
- Towards a theoretical determination of the geographical probability distribution of meteoroid impacts on Earth
- Number of near-Earth objects and formation of lunar craters over the last billion years
- Collision probabilities of migrating small bodies and dust particles with planets
- Growth of the Moon due to bodies ejected from the Earth
- Origin of the Moon and Lunar Water
- Formation of the four terrestrial planets in the Jupiter-Saturn chaotic excitation scenario: fundamental properties and water delivery