Localized sources of water vapour on the dwarf planet (1) Ceres

  title={Localized sources of water vapour on the dwarf planet (1) Ceres},
  author={Michael K{\"u}ppers and Laurence O'Rourke and Dominique Bockel{\'e}e-Morvan and Vladimir V. Zakharov and Seungwon Lee and Paul von Allmen and Beno{\^i}t Carry and David Teyssier and A. P. Marston and Thomas G. M{\"u}ller and Jacques Crovisier and Maria Antonietta Barucci and Raphael Moreno},
The ‘snowline’ conventionally divides Solar System objects into dry bodies, ranging out to the main asteroid belt, and icy bodies beyond the belt. Models suggest that some of the icy bodies may have migrated into the asteroid belt. Recent observations indicate the presence of water ice on the surface of some asteroids, with sublimation a potential reason for the dust activity observed on others. Hydrated minerals have been found on the surface of the largest object in the asteroid belt, the… 
Sublimation in bright spots on (1) Ceres
It is concluded that Ceres must have accreted material from beyond the ‘snow line’, which is the distance from the Sun at which water molecules condense, and is consistent with hydrated magnesium sulfates mixed with dark background material.
Dwarf planet Ceres and the ingredients of life
Recent spacecraft studies of Comet 67P/Churyumov-Gerasimenko with Rosetta and of Ceres provide evidence that complex organic molecules and even amino acids are ubiquitous on small bodies in the solar system and that water ice is abundant in the asteroid belt.
The Radiation Environment of Ceres and Implications for Surface Sampling.
Ceres is a large water-rich dwarf planet located within the asteroid belt. Its surface displays evidence of material sourced from a deep subsurface liquid brine layer within recent geologic time,
On the possible origin of the asteroid (1) Ceres
The last three decades the asteroid (1) Ceres is an object of the intensive ground-and space-based observations. A new unusual contributing to these studies represents the recent detection of
Short-term variability on the surface of (1) Ceres - A changing amount of water ice?
Context. The dwarf planet (1) Ceres ‐ next target of the NASA Dawn mission ‐ is the largest body in the asteroid main belt. Although several observations of this body have been performed so far, the
Detection of local H2O exposed at the surface of Ceres
Dawn VIR infrared observations of Oxo crater on Ceres demonstrate the detection of H2O at the surface, and theories predict a water ice-rich mantle, and water vapor emissions have been observed, yet no water (H2O) has been observed.
Search for water outgassing of (1) Ceres near perihelion
Context. (1) Ceres is the largest body in the main asteroid belt and one of the most intriguing objects in the solar system, in part because of the discovery of water outgassing by the Herschel Space
Oxo Crater on (1) Ceres: Geological History and the Role of Water-ice
Dwarf planet Ceres (empty set similar to 940 km) is the largest object in the main asteroid belt. Investigations suggest that Ceres is a thermally evolved, volatile-rich body with potential
Water Reservoirs in Small Planetary Bodies: Meteorites, Asteroids, and Comets
The nature and probable origins of asteroids and comets are discussed based on data from remote observations, in situ measurements by spacecraft, and laboratory analyses of meteorites derived from asteroids.


A Search for Water Vaporization on Ceres
There are hints that the dwarf planet (1) Ceres may contain a large amount of water ice. Some models and previous observations suggest that ice could be close enough to the surface to create a flux
Brucite and carbonate assemblages from altered olivine-rich materials on Ceres
The mineralogy of the dwarf planet Ceres has long remained uncertain. The infrared spectral features of this planetary body are indicative of minerals derived from the aqueous alteration of
Differentiation of the asteroid Ceres as revealed by its shape
C Ceres has a shape and smoothness indicative of a gravitationally relaxed object that is significantly less flattened than that expected for a homogeneous object, but is consistent with a central mass concentration indicative of differentiation.
Water ice and organics on the surface of the asteroid 24 Themis
Infrared spectra of the asteroid 24 Themis show that ice and organic compounds are not only present on its surface but also prevalent, and their identification agrees with independent results that rule out other compounds as possible sources of the observed spectral structure.
The water regime of asteroid (1) Ceres
The Active Asteroids
Some asteroids eject dust, unexpectedly producing transient, comet-like comae and tails. First ascribed to the sublimation of near-surface water ice, mass losing asteroids (also called "main-belt
Detection of ice and organics on an asteroidal surface
The spectroscopic detection of water ice and organic material on the asteroid 24 Themis is reported, a detection that has been independently confirmed and concludes that water ice is more common on asteroids than was previous thought and may be widespread in asteroidal interiors at much smaller heliocentric distances than was previously expected.
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
Asteroid 65 Cybele: Detection Of Small Silicate Grains, Water-Ice And Organics
Context. (65) Cybele is the most representative member of a population of primitive asteroids in the outer edge of the main belt, the Cybele asteroids. Recent dynamical models suggest that a