Impacts Cause Atmospheric Loss During Planetary Formation

Atmospheric mass loss during planet formation: The importance of planetesimal impacts

Authors:

Schlichting et al

Abstract:

Quantifying the atmospheric mass loss during planet formation is crucial for understanding the origin and evolution of planetary atmospheres. We examine 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 γ=5/3γ=5/3) that the local atmospheric mass loss fraction for ground velocities vg≲0.25vescvg≲0.25vesc is given by χloss=(1.71vg/vesc)4.9χloss=(1.71vg/vesc)4.9, where vescvesc is the escape velocity from the target. Yet, the global atmospheric mass loss is a weaker function of the impactor velocity vImpvImp and mass mImpmImp and given by Xloss≃0.4x+1.4x2-0.8x3Xloss≃0.4x+1.4x2-0.8x3 (isothermal atmosphere) and Xloss≃0.4x+1.8x2-1.2x3Xloss≃0.4x+1.8x2-1.2x3 (adiabatic atmosphere), where x=(vImpm/vescM)x=(vImpm/vescM). Atmospheric mass loss due to planetesimal impacts proceeds in two different regimes: (1) large enough impactors View the MathML sourcem≳2ρ0(πhR)3/2 (25 km for the current Earth), are able to eject all the atmosphere above the tangent plane of the impact site, which is h/2Rh/2R of the whole atmosphere, where View the MathML sourceh,R and ρ0ρ0 are the atmospheric scale height, radius of the target, and its atmospheric density at the ground. (2) Smaller impactors, but above m greater than 4πρ0h3m greater than 4πρ0h3 (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 (2 km for the current Earth). For impactor flux size distributions parametrized by a single power law, N( greater than r)∝r-q+1N( greater than r)∝r-q+1, with differential power law index q , we find that for 1 less than q less than 31 less than q less than 3 the atmospheric mass loss proceeds in regime (1) whereas for q grater than 3q greater than 3 the mass loss is dominated by regime (2). Impactors with m≲4πρ0h3m≲4πρ0h3 are not able to eject any atmosphere. Despite being bombarded by the same planetesimal population, we find that the current differences in Earth’s and Venus’ atmospheric masses can be explained by modest differences in their initial atmospheric masses and that the current atmosphere of the Earth could have resulted from an equilibrium between atmospheric erosion and volatile delivery to the atmosphere from planetesimal impacts. 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.