A basin-free spherical shape as an outcome of a giant impact on asteroid Hygiea

@article{Vernazza2019ABS,
  title={A basin-free spherical shape as an outcome of a giant impact on asteroid Hygiea},
  author={Pierre Vernazza and L. Jord{\'a} and Pavel {\vS}eve{\vc}ek and Miroslav Bro{\vz} and M. Viikinkoski and Josef Hanu{\vs} and Beno{\^i}t Carry and Alexis Drouard and Marin Ferrais and Micha{\"e}l Marsset and F. Marchis and Mirel Birlan and Edyta Podlewska-Gaca and Emmanuel Jehin and Przemysław Bartczak and Grzegorz Dudziński and J{\'e}r{\^o}me Berthier and Julie C. Castillo‐Rogez and Fabrice Cipriani and Florent Colas and Francesca E. DeMeo and Christophe Dumas and Josef Ďurech and Romain F{\'e}tick and Thierry Fusco and J. Grice and Marika Kaasalainen and Agnieszka Kryszczyńska and Philippe Lamy and H. Le Coroller and Anna Marciniak and Tadeusz Michałowski and P. Michel and N. Rambaux and T Santana-Ros and P. Tanga and Fr{\'e}d{\'e}ric Vachier and Arthur Vigan and Olivier G. Witasse and B. Yang and Micha{\"e}l Gillon and Zouhair Benkhaldoun and R{\'o}bert Szak{\'a}ts and R. Hirsch and Ren{\'e} Duffard and A. Chapman and J. L. Maestre},
  journal={Nature Astronomy},
  year={2019},
  volume={4},
  pages={136-141}
}
(10) Hygiea is the fourth largest main belt asteroid and the only known asteroid whose surface composition appears similar to that of the dwarf planet (1) Ceres 1 , 2 , suggesting a similar origin for these two objects. Hygiea suffered a giant impact more than 2 Gyr ago 3 that is at the origin of one of the largest asteroid families. However, Hygeia has never been observed with sufficiently high resolution to resolve the details of its surface or to constrain its size and shape. Here, we report… 
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References

SHOWING 1-10 OF 91 REFERENCES
Dynamical evolution and chronology of the Hygiea asteroid family
The asteroid (10) Hygiea is the fourth largest asteroid of the main belt, by volume and mass, and it is the largest member of its own family. Previous works investigated the long-term effects of
The structure of the asteroid 4 Vesta as revealed by models of planet-scale collisions
TLDR
Three-dimensional simulations of Vesta’s global evolution under two overlapping planet-scale collisions closely reproduce its observed shape, and provide maps of impact excavation and ejecta deposition.
(16) Psyche: A mesosiderite-like asteroid?
Context. Asteroid (16) Psyche is the target of the NASA Psyche mission. It is considered one of the few main-belt bodies that could be an exposed proto-planetary metallic core and that would thus be
The impact crater at the origin of the Julia family detected with VLT/SPHERE?
Context. The vast majority of the geophysical and geological constraints (e.g., internal structure, cratering history) for main-belt asteroids have so far been obtained via dedicated interplanetary
Vesta’s Shape and Morphology
TLDR
Dawn observations confirm the large impact basin at Vesta's south pole and reveal evidence for an earlier, underlying large basin (Veneneia), underscoring Vesta’s unique role as a transitional solar system body.
The Shape of Gaspra
Abstract Images of Gaspra obtained during the October 1991 Galileo flyby have been used to derive a shape model of the asteroid. Gaspra is a highly irregular object with principal diameters of 18.2,
Astrometric masses of 21 asteroids, and an integrated asteroid ephemeris
We apply the technique of astrometric mass determination to measure the masses of 21 main-belt asteroids; the masses of 9 Metis (1.03 ± 0.24 × 10-11 M⊙), 17 Thetis (6.17 ± 0.64 × 10-13 M⊙), 19
Density of asteroids
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