Hydrodynamical simulations of giant impacts find lower post-impact CMB pressures due to thermal and rotational effects, common full mantle melting, and conditions favoring metal-silicate equilibration near the CMB.
Collisions Between Gravity-Dominated Bodies: 1. Outcome Regimes and Scaling Laws
3 Pith papers cite this work. Polarity classification is still indexing.
3
Pith papers citing it
abstract
Collisions are the core agent of planet formation. In this work, we derive an analytic description of the dynamical outcome for any collision between gravity-dominated bodies. We conduct high-resolution simulations of collisions between planetesimals; the results are used to isolate the effects of different impact parameters on collision outcome. During growth from planetesimals to planets, collision outcomes span multiple regimes: cratering, merging, disruption, super-catastrophic disruption, and hit-and-run events. We derive equations (scaling laws) to demarcate the transition between collision regimes and to describe the size and velocity distributions of the post-collision bodies. The scaling laws are used to calculate maps of collision outcomes as a function of mass ratio, impact angle, and impact velocity, and we discuss the implications of the probability of each collision regime during planet formation. The analytic collision model presented in this work will significantly improve the physics of collisions in numerical simulations of planet formation and collisional evolution. (abstract abridged)
fields
astro-ph.EP 3years
2026 3verdicts
UNVERDICTED 3representative citing papers
Simulations of giant impacts between 0.2-4 Earth-mass planets yield post-impact luminosities of 5e-5 to 0.1 L_sun cooling over 1-2000 days, predicting 0-14 detections in Gaia DR4 and a comparable number in LSST.
Analysis of SPH simulations and collision velocity models predicts that collisionally-produced super-Mercuries have higher densities at low mass and short period, identifying GJ 367b as the strongest observed candidate.
citing papers explorer
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Thermal and rotational effects of giant impacts during terrestrial planet accretion
Hydrodynamical simulations of giant impacts find lower post-impact CMB pressures due to thermal and rotational effects, common full mantle melting, and conditions favoring metal-silicate equilibration near the CMB.
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Can giant impacts be directly detected in other star systems?
Simulations of giant impacts between 0.2-4 Earth-mass planets yield post-impact luminosities of 5e-5 to 0.1 L_sun cooling over 1-2000 days, predicting 0-14 detections in Gaia DR4 and a comparable number in LSST.
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The Maximum Density of a Collisionally-Produced Planet is A Function of its Mass and Orbital Period
Analysis of SPH simulations and collision velocity models predicts that collisionally-produced super-Mercuries have higher densities at low mass and short period, identifying GJ 367b as the strongest observed candidate.