Signatures of hit-and-run collisions

Erik Asphaug

Research output: Chapter in Book/Report/Conference proceedingChapter

1 Citation (Scopus)

Abstract

Introduction Terrestrial planets grew in a series of similar-sized collisions (SSCs) that swept up most of the next-largest bodies (NLBs; see Box 2.1). Theia was accreted by the Earth to form the Moon according to the theory. Planetesimals likewise might have finished their accretion in a sequence of “junior giant impacts,” scaled down in size and velocity. Here we consider the complicated physics of pairwise accretion, as planetesimals collide and grow to planetary scales, and show how the inefficiency of that process is a foundation for the origin of planetesimals and the diversity of meteorites and primary asteroids. Detailed simulations show that planetary collisions are inefficient mergers. Accretion inefficiency gets concentrated, as it were, in the unaccreted bits and pieces, giving asteroids and meteorites their distinctive record, according to the arguments below. The impact axis is well off-center in a typical collision, relative to the combined center of mass, with dire consequences to the less massive object M2. The target M1 serves both as an “anvil” into which M2 collides, and decelerates, and as a gravitational pivot around which it gets swung, causing it to be shredded. The post-collision system can be gravitationally bound or not, depending on the projectile mass γ = M2/(M 1 + M2) normalized to the total mass, the relative velocity vrel normalized to the escape velocity v esc, which scales with size, the impact angle θ with median value 45°, and composition, differentiation, rotation, and thermal tate. Outcomes of SSCs are diverse throughout this large parameter space, segregating what is gravitationally bound from what is not, thereby causing the disruption and compositional segregation of planetesimals and growing planets. For example, the standard model of Moon formation involves a graze-and-merge collision (GMC) where a Mars-size planet Theia is mostly accreted (ξ ~ 1) by a ~45° impact into proto-Earth at close to the mutual escape velocity vesc (Canup and Asphaug, 2001), leaving a silicate protolunar disk. The Mars hemispheric dichotomy might have been caused by a faster (up to 2vesc) collision (Marinova et al., 2008), in which case the impactor was not accreted by M1.

Original languageEnglish (US)
Title of host publicationPlanetesimals
Subtitle of host publicationEarly Differentiation and Consequences for Planets
PublisherCambridge University Press
Pages7-37
Number of pages31
ISBN (Electronic)9781316339794
ISBN (Print)9781107118485
DOIs
StatePublished - Jan 1 2017

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signatures
protoplanets
collisions
escape velocity
meteorites
moon
asteroids
mars
planets
pivots
dichotomies
impactors
terrestrial planets
anvils
center of mass
boxes
projectiles
silicates
physics
simulation

ASJC Scopus subject areas

  • Physics and Astronomy(all)

Cite this

Asphaug, E. (2017). Signatures of hit-and-run collisions. In Planetesimals: Early Differentiation and Consequences for Planets (pp. 7-37). Cambridge University Press. https://doi.org/10.1017/9781316339794.002

Signatures of hit-and-run collisions. / Asphaug, Erik.

Planetesimals: Early Differentiation and Consequences for Planets. Cambridge University Press, 2017. p. 7-37.

Research output: Chapter in Book/Report/Conference proceedingChapter

Asphaug, E 2017, Signatures of hit-and-run collisions. in Planetesimals: Early Differentiation and Consequences for Planets. Cambridge University Press, pp. 7-37. https://doi.org/10.1017/9781316339794.002
Asphaug E. Signatures of hit-and-run collisions. In Planetesimals: Early Differentiation and Consequences for Planets. Cambridge University Press. 2017. p. 7-37 https://doi.org/10.1017/9781316339794.002
Asphaug, Erik. / Signatures of hit-and-run collisions. Planetesimals: Early Differentiation and Consequences for Planets. Cambridge University Press, 2017. pp. 7-37
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