Differentiation of the asteroid Ceres as revealed by its shape

  title={Differentiation of the asteroid Ceres as revealed by its shape},
  author={Peter C. Thomas and Joel Wm. Parker and Lucy A. McFadden and Christopher T. Russell and S. Alan Stern and Mark V. Sykes and Eliot F. Young},
The accretion of bodies in the asteroid belt was halted nearly 4.6 billion years ago by the gravitational influence of the newly formed giant planet Jupiter. The asteroid belt therefore preserves a record of both this earliest epoch of Solar System formation and variation of conditions within the solar nebula. Spectral features in reflected sunlight indicate that some asteroids have experienced sufficient thermal evolution to differentiate into layered structures. The second most massive… 
The Origin and Evolution of the Asteroid Belt—Implications for Vesta and Ceres
Vesta and Ceres are the largest members of the asteroid belt, surviving from the earliest phases of Solar System history. They formed at a time when the asteroid belt was much more massive than it is
The missing large impact craters on Ceres
The results indicate that a significant population of large craters has been obliterated, implying that long-wavelength topography viscously relaxed or that Ceres experienced protracted widespread resurfacing.
Asteroids 1 ceres and 4 vesta: Objects of the Dawn space mission
The Dawn spacecraft of the NASA space mission to asteroids 1 Ceres and 4 Vesta was launched in September 2007. The choice of these two asteroids is deeply grounded: they are the largest and most
Oxygen and Asteroids
Hundreds of thousands of asteroids have been discovered in the asteroid belt and in near-Earth space. Oxygen is an abundant element in meteorites and presumably in most asteroids. Spectral
True polar wander of Ceres due to heterogeneous crustal density
Ceres is the largest body in the main asteroid belt. It was recently explored by the Dawn mission to uncover strong similarities with other icy bodies. The morphological features observed on the


A Thermal Model for the Differentiation of Asteroid 4 Vesta, Based on Radiogenic Heating☆
A finite element code has been developed to model the thermal history of Asteroid 4 Vesta. This is the first attempt to model the thermal history of a differentiated asteroid through core and crust
Ceres: Evolution and current state
[1] We modeled several thermal evolution scenarios for Ceres to explore the nature of large, wet protoplanets and to predict current-day evidence that might be found by close inspection, such as by
A comprehensive model for the changes in asteroid spin rates due to large collisions was developed by combining the theoretical results of Cellino et al. (1990) with previously published work on spin
The water regime of asteroid (1) Ceres
Crater formation and modification on the icy satellites of Uranus and Saturn: Depth/diameter and central peak occurrence
Depth/diameters (d/D) for fresh craters on the intermediate-sized icy satellites of Uranus and Saturn have been determined using photoclinometry and shadow lengths, and are compared with similar
Gravity, Tides, and Topography on Small Satellites and Asteroids: Application to Surface Features of the Martian Satellites
Abstract The influence of gravitational potential on the disposition of loose material on the surfaces of small satellites is investigated using the martian satellites as examples. "Gravity" on small
Impact excavation on Asteroid 4 Vesta: Hubble Space Telescope results
Hubble Space Telescope images of asteroid 4 Vesta obtained during the favorable 1996 apparition show an impact crater 460 kilometers in diameter near the south pole. Color measurements within the
Asteroid Vesta: Spectral Reflectivity and Compositional Implications
Comparison with laboratory measurements on meteorites and Apollo 11 samples indicates that the surface of Vesta has a composition very similar to that of certain basaltic achondrites.