Origin, internal structure and evolution of 4 vesta

Maria T. Zuber, Harry Y. McSween, Richard P. Binzel, Linda Elkins-Tanton, Alexander S. Konopliv, Carle M. Pieters, David E. Smith

Research output: Chapter in Book/Report/Conference proceedingChapter

1 Citation (Scopus)

Abstract

Asteroid 4 Vesta is the only preserved intact example of a large, differentiated protoplanet like those believed to be the building blocks of terrestrial planet accretion. Vesta accreted rapidly from the solar nebula in the inner asteroid belt and likely melted due to heat released due to the decay of 26Al. Analyses of meteorites from the howardite-eucrite-diogenite (HED) suite, which have been both spectroscopically and dynamically linked to Vesta, lead to a model of the asteroid with a basaltic crust that overlies a depleted peridotitic mantle and an iron core. Vesta's crust may become more mafic with depth and might have been intruded by plutons arising from mantle melting. Constraints on the asteroid's moments of inertia from the long-wavelength gravity field, pole position and rotation, informed by bulk composition estimates, allow tradeoffs between mantle density and core size; cores of up to half the planetary radius can be consistent with plausible mantle compositions. The asteroid's present surface is expected to consist of widespread volcanic terrain, modified extensively by impacts that exposed the underlying crust or possibly the mantle. Hemispheric heterogeneity has been observed by poorly resolved imaging of the surface that suggests the possibility of a physiographic dichotomy as occurs on other terrestrial planets. Vesta might have had an early magma ocean but details of the early thermal structure are far from clear owing to model uncertainties and paradoxical observations from the HEDs. Petrological analysis of the eucrites coupled with thermal evolution modeling recognizes two possible mechanisms of silicate-metal differentiation leading to the formation of the basaltic achondrites: equilibrium partial melting or crystallization of residual liquid from the cooling magma ocean. A firmer understanding the plethora of complex physical and chemical processes that contribute to melting and crystallization will ultimately be required to distinguish among these possibilities. The most prominent physiographic feature on Vesta is the massive south polar basin, whose formation likely re-oriented the body axis of the asteroid's rotation. The large impact represents the likely major mechanism of ejection of fragments that became the HEDs. Observations from the Dawn mission hold the promise of revolutionizing our understanding of 4 Vesta, and by extension, the nature of collisional, melting and differentiation processes in the nascent solar system.

Original languageEnglish (US)
Title of host publicationThe Dawn Mission to Minor Planets 4 Vesta and 1 Ceres
PublisherSpringer New York
Pages77-93
Number of pages17
Volume9781461449034
ISBN (Print)9781461449034, 1461449022, 9781461449027
DOIs
StatePublished - Oct 1 2012
Externally publishedYes

Fingerprint

asteroid
mantle
eucrite
melting
crust
crystallization
planet
diogenite
magma
howardite
achondrite
thermal evolution
ocean
thermal structure
gravity field
basin evolution
chemical process
inertia
meteorite
solar system

Keywords

  • Asteroid
  • Core
  • Crust
  • Evolution
  • Impact
  • Mantle
  • Vesta

ASJC Scopus subject areas

  • Earth and Planetary Sciences(all)

Cite this

Zuber, M. T., McSween, H. Y., Binzel, R. P., Elkins-Tanton, L., Konopliv, A. S., Pieters, C. M., & Smith, D. E. (2012). Origin, internal structure and evolution of 4 vesta. In The Dawn Mission to Minor Planets 4 Vesta and 1 Ceres (Vol. 9781461449034, pp. 77-93). Springer New York. https://doi.org/10.1007/978-1-4614-4903-4_6

Origin, internal structure and evolution of 4 vesta. / Zuber, Maria T.; McSween, Harry Y.; Binzel, Richard P.; Elkins-Tanton, Linda; Konopliv, Alexander S.; Pieters, Carle M.; Smith, David E.

The Dawn Mission to Minor Planets 4 Vesta and 1 Ceres. Vol. 9781461449034 Springer New York, 2012. p. 77-93.

Research output: Chapter in Book/Report/Conference proceedingChapter

Zuber, MT, McSween, HY, Binzel, RP, Elkins-Tanton, L, Konopliv, AS, Pieters, CM & Smith, DE 2012, Origin, internal structure and evolution of 4 vesta. in The Dawn Mission to Minor Planets 4 Vesta and 1 Ceres. vol. 9781461449034, Springer New York, pp. 77-93. https://doi.org/10.1007/978-1-4614-4903-4_6
Zuber MT, McSween HY, Binzel RP, Elkins-Tanton L, Konopliv AS, Pieters CM et al. Origin, internal structure and evolution of 4 vesta. In The Dawn Mission to Minor Planets 4 Vesta and 1 Ceres. Vol. 9781461449034. Springer New York. 2012. p. 77-93 https://doi.org/10.1007/978-1-4614-4903-4_6
Zuber, Maria T. ; McSween, Harry Y. ; Binzel, Richard P. ; Elkins-Tanton, Linda ; Konopliv, Alexander S. ; Pieters, Carle M. ; Smith, David E. / Origin, internal structure and evolution of 4 vesta. The Dawn Mission to Minor Planets 4 Vesta and 1 Ceres. Vol. 9781461449034 Springer New York, 2012. pp. 77-93
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