Atmospheric Mass Loss During Planet Formation: The Importance of Planetesimal Impacts
arXiv:1406.6435 · doi:10.1016/j.icarus.2014.09.053
Abstract
We quantify the atmospheric mass loss during planet formation by examining the contributions to atmospheric loss from both giant impacts and planetesimal accretion. Giant impacts cause global motion of the ground. Using analytic self-similar solutions and full numerical integrations we find (for isothermal atmospheres with adiabatic index () that the local atmospheric mass loss fraction for ground velocities is given by , where is the escape velocity from the target. Yet, the global atmospheric mass loss is a weaker function of the impactor velocity and mass and given by (isothermal atmosphere) and (adiabatic atmosphere), where . Atmospheric mass loss due to planetesimal impacts proceeds in two different regimes: 1) Large enough impactors (25~km for the current Earth), are able to eject all the atmosphere above the tangent plane of the impact site, which is of the whole atmosphere, where , and are the atmospheric scale height, radius of the target, and its atmospheric density at the ground. 2) Smaller impactors, but above (1~km for the current Earth) are only able to eject a fraction of the atmospheric mass above the tangent plane. We find that the most efficient impactors (per unit impactor mass) for atmospheric loss are planetesimals just above that lower limit and that the current atmosphere of the Earth could have resulted from an equilibrium between atmospheric erosion and volatile delivery to the atmosphere from planetesimals. We conclude that planetesimal impacts are likely to have played a major role in atmospheric mass loss over the formation history of the terrestrial planets. (Abridged)
Submitted to Icarus, 39 pages, 16 figures
References in corpus (1)
Cited by in corpus (30)
- Make Super-Earths, Not Jupiters: Accreting Nebular Gas onto Solid Cores at 0.1 AU and Beyond
- Formation of planetary systems by pebble accretion and migration: How the radial pebble flux determines a terrestrial-planet or super-Earth growth mode
- A water budget dichotomy of rocky protoplanets from Al-heating
- A giant impact as the likely origin of different twins in the Kepler-107 exoplanet system
- The structure of terrestrial bodies: Impact heating, corotation limits and synestias
- Kepler-21b: A rocky planet around a V = 8.25 magnitude star
- Atmospheric Regimes and Trends on Exoplanets and Brown Dwarfs
- Impact bombardment chronology of the terrestrial planets from 4.5 Ga to 3.5 Ga
- Connecting planet formation and astrochemistry: Refractory carbon depletion leading to super-stellar C/O in giant planetary atmospheres
- Loss and fractionation of noble gas isotopes and moderately volatile elements from planetary embryos and early Venus, Earth and Mars
- Susceptibility of planetary atmospheres to mass loss and growth by planetesimal impacts: the impact shoreline
- Evolution of the Water Snow Line in Magnetically Accreting Protoplanetary Disks
- Reduced atmospheres of post-impact worlds: The early Earth
- Atmosphere loss in planet-planet collisions
- Validation of 13 Hot and Potentially Terrestrial TESS Planets
- Transfer, loss and physical processing of water in hit-and-run collisions of planetary embryos
- Numerous chondritic impactors and oxidized magma ocean set Earth's volatile depletion
- A Volatile-Poor Formation of LHS 3844b based on its Lack of Significant Atmosphere
- Realistic collisional water transport during terrestrial planet formation: Self-consistent modeling by an N-body--SPH hybrid code
- Planetary formation and water delivery in the habitable zone around solar-type stars in different dynamical environments
- On the formation of the Kepler-10 planetary system
- Did Mars possess a dense atmosphere during the first ~400 million years?
- Examining the Radius Valley: a Machine Learning Approach
- Fate of the runner in hit-and-run collisions
- Unified simulations of planetary formation and atmospheric evolution II: Rapid disk clearing by photoevaporation yields low-mass super-Earth atmospheres
- The Exosphere as a Boundary: Origin and Evolution of Airless Bodies in the Inner Solar System and Beyond Including Planets with Silicate Atmospheres
- Mars in the aftermath of a colossal impact
- YOUNG Star detrending for Transiting Exoplanet Recovery (YOUNGSTER) II: Using Self-Organising Maps to explore young star variability in Sectors 1-13 of TESS data
- Effects of Self-gravity on Mass-loss of the Post-impact Super-Earths
- The effect of late giant collisions on the atmospheres of protoplanets and the formation of cold sub-Saturns