Map of Hydrated Minerals on Vesta
This map from NASA's Dawn mission indicates the presence of hydrated minerals on the giant asteroid Vesta. Hydrated minerals are seen in white, with areas of high concentrations circled with a yellow dotted line in the annotated version. The data were obtained by Dawn's visible and infrared mapping spectrometer in August 2011, from an altitude of 1,700 miles (2,700 kilometers). Image credit: NASA/JPL-Caltech/UCLA/INAF
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The mechanism that incorporates water into the terrestrial planets is a matter of extensive debate for planetary scientists. Now, observations of the giant asteroid Vesta by NASA's Dawn mission suggest that hydrated materials were delivered to it mainly through a buildup of small particles during an epoch when the solar system was rich in dust. This is a radically different process from the way hydrated materials have been deposited on the moon and may have implications for the formation of terrestrial planets, including the delivery of the water that formed Earth's ocean. Maria Cristina De Sanctis and the Dawn team present the scenarios today at the European Planetary Science Congress in Madrid, Spain.

"Vesta's surface shows distinct areas enriched with hydrated materials," said De Sanctis, of the Italian National Institute for Astrophysics in Rome. "These regions are not dependent on solar illumination or temperature, as we find in the case of the moon. The uneven distribution is unexpected and indicates ancient processes that differ from those believed to be responsible for delivering water to other airless bodies, like the moon."

A team led by De Sanctis studied data from Dawn's visible and infrared mapping spectrometer, which complement recently reported data on hydrogen distribution from Dawn's gamma ray and neutron detector. Their analysis showed large regional concentrations of hydroxyl - a hydrogen and an oxygen atom bound together - clearly associated with geological features, including ancient, highly-cratered terrains and a crater named Oppia. 

Hydroxyl on the surface of the moon is thought to be created continuously by the interaction of protons from the solar wind with the top 10 feet (few meters) of the lunar surface, or regolith. Highest concentrations are found in areas near the lunar poles and in permanently shadowed craters where it is very cold. By contrast, the distribution of hydroxyl on Vesta is not dependent on significant shadowing or unusual cold temperatures. It is also stable over time, so its origin does not appear to be due to short-term processes.

The hydroxyl-rich regions on Vesta broadly correspond to its oldest surfaces. Around relatively large and young impact craters, hydroxyl detections are weak or absent, suggesting that the delivery of the substance is not an ongoing process.

The evidence from Dawn's visible and infrared mapping spectrometer suggests that much of Vesta's hydroxyl was delivered by small particles of primitive material, less than a few centimeters in diameter, over a time-limited period. This period may have occurred during the primordial solar system, around the time water is believed to have accumulated on Earth, or during the Late Heavy Bombardment, when collisions with space rocks would have produced a significant amount of dust.

However, this is not the whole story of hydrated materials on Vesta. The Oppia Crater is hydroxyl-rich, but not covered with the primitive dark material. This suggests there is more than one mechanism at work for depositing hydroxyl on Vesta's surface.

"The origin of Vesta's hydroxyl is certainly complex and possibly not unique: there could be various sources, like formation of hydroxyl actually on Vesta, in addition to the primordial impactors," said De Sanctis. "Vesta is providing new insights into the delivery of hydrous materials in the main asteroid belt, and may offer new scenarios on the delivery of hydrous minerals in the inner solar system, suggesting processes that may have played a role in the formation of terrestrial planets."

Following more than a year at Vesta, Dawn departed in September 2012 for the dwarf planet Ceres, where it will arrive in 2015. Dawn's mission to Vesta and Ceres is managed by NASA's Jet Propulsion Laboratory, Pasadena, Calif., for NASA's Science Mission Directorate in Washington. JPL is a division of the California Institute of Technology in Pasadena. Dawn is a project of the directorate's Discovery Program, managed by NASA's Marshall Space Flight Center in Huntsville, Ala. UCLA is responsible for overall Dawn mission science. Orbital Sciences Corp. in Dulles, Va., designed and built the spacecraft. The Dawn visible and infrared (VIR) mapping spectrometer was built by Selex Galileo and the Italian National Institute for Astrophysics.

For more information about Dawn, visit and .