Water detection on atmosphereless celestial bodies: Alternative explanations of the observations

Starukhina, L. V.

doi:10.1029/2000je001307

Cited by 98 publications

(91 citation statements)

References 40 publications

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“…Particularly, an extremely low temperature is neither a necessary nor a sufficient condition for low dielectric loss and high radar brightness and may be explained by differences in silicate material properties (activation energy) between surface regions. Starukhina (2001) also points out that the considerably larger (a factor of ∼2.5) circular polarization ratios for polar craters of Mercury compared to the value for the lunar poles, as well as the lack of radar-bright polar craters on the Moon, is consistent with a difference in surface composition between the two bodies as the temperature within permanently shaded craters are expected to be similar. The non-necessity of water being responsible for the backscattering property of the mercurian regolith is fully consistent with the findings in this paper, since the spectral slope-emission angle dependence is of the same order of magnitude for albedo features from all measured latitudes and both (bright and dark) feature types, indicating that silicates are globally distributed.…”

Section: Discussionmentioning

confidence: 73%

Properties of the Hermean Regolith II. Disk-Resolved Multicolor Photometry and Color Variations of the “Unknown” Hemisphere

Warell¹

2002

Icarus

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Section: Discussionmentioning

confidence: 73%

Properties of the Hermean Regolith II. Disk-Resolved Multicolor Photometry and Color Variations of the “Unknown” Hemisphere

Warell¹

2002

Icarus

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“…While the quantitative results have not been borne out (for instance, Vesta has a 3-µm band depth ~2% at its deepest , compared to the ~20-70% depth predicted by Starukhina), it was one of the first treatments attempting to predict the effects of space weathering in that spectral region. Thoughts on how the spectrum of airless bodies might change near 3 µm with exposure to typical regolith processes have varied from a prediction of dehydration (Pieters, personal communication) to the creation of bands (e.g., Starukhina, 2001) to no appreciable effect (Rivkin et al, 2003).…”

mentioning

confidence: 99%

“…Starukhina (2001), modeling the interaction of solar wind protons with regolith, predicted that OH and its diagnostic 3-µm absorption band should always be present on airless bodies. While the quantitative results have not been borne out (for instance, Vesta has a 3-µm band depth ~2% at its deepest , compared to the ~20-70% depth predicted by Starukhina), it was one of the first treatments attempting to predict the effects of space weathering in that spectral region.…”

mentioning

confidence: 99%

Astronomical Observations of Volatiles on Asteroids

Rivkin¹,

Campins²,

Emery³

et al. 2015

Asteroids IV

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We have long known that water and hydroxyl are important components in meteorites and asteroids. However, in the time since the publication of Asteroids III, evolution of astronomical instrumentation, laboratory capabilities, and theoretical models have led to great advances in our understanding of H 2 O/OH on small bodies, and spacecraft observations of the Moon and Vesta have important implications for our interpretations of the asteroidal population. We begin this chapter with the importance of water/OH in asteroids, after which we will discuss their spectral features throughout the visible and near-infrared. We continue with an overview of the findings in meteorites and asteroids, closing with a discussion of future opportunities, the results from which we can anticipate finding in Asteroids V. Because this topic is of broad importance to asteroids, we also point to relevant in-depth discussions elsewhere in this volume.1 Water ice sublimation and processes that create, incorporate, or deliver volatiles to the asteroid belt Accretion/Solar system formation 1.1The concept of the "snow line" (also known as "water-frost line") is often used in discussing the water inventory of small bodies in our solar system. The snow line is the heliocentric distance at which water ice is stable enough to be accreted into planetesimals. The placement of the snow line has varied in different models. A location just inside Jupiter helps explain the greater mass of the giant planets as they accrete a larger fraction of the mass in the solar nebula. Although the location of the snow line before and during planet formation is uncertain, some studies show it may have fallen within the asteroid belt (Lunine, 2006). The location of the snow line in our solar system coinciding with the asteroid belt is consistent with observations of disks around other stars (e.g., Su et al., 2013), where planetesimal rings tend to coincide with the snow line around those stars. However, it seems the relatively simple concept of a static snow line requires revisions in light of new results on several fronts. For instance, the snow line likely moved with time as the Sun's luminosity changed early in solar system history (e.g., Martin and Livio, 2012). Even though there is no agreement on the details of planetesimal formation and growth, some models favor the growth of ~100 km-scale planetesimals directly from cm-scale pieces Cuzzi et al., 2010; for a dissenting view see Weidenschilling, 2011). Hence, the timing of those assemblies as conditions change could have a strong influence on the amount of radioactive elements present in a planetesimal's interior and on its rock-to-ice ratio, further complicating the concept of a snow line. Recent observations also point to a more complex picture. For example, the concept of an asteroid-comet continuum, where there is no clear boundary between primitive asteroids and cometary nuclei (e.g., Gounelle, 2011) is gaining support and is consistent with the intermittent cometary behavior of some main belt and near-E...

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“…In addition to covering previously implanted regions of the grains, the amorphous rims could themselves contain OH transported with the vaporized materials [Crider and Vondrak, 2000] or formed from solar wind implantation, thus potentially creating regions hundreds of nm thick of OH and H2O containing material. As a result of meteorite gardening burying implanted grains and exposing fresh soil, the predicted solar wind hydrogen implantation could produce as much as 1% of water in the upper ~40 cm of the lunar regolith [Starukhina, 2001], consistent with epithermal neutron measurements from the Lunar Prospector of hydrogen concentration in the lunar regolith [Feldman et al, 2000].…”

Section: Astrophysical Motivationsupporting

confidence: 50%

“…Using materials of known composition and monitoring changes during irradiation allow precise production rates and upper limits on hydroxyl concentration in lunar soils to be determined. These results are applicable to the Moon and also to other airless bodies such as Mercury, main belt asteroids [Starukhina, 2001], and in protoplanetary silicate grains [Djouadi et al, 2011] subject to stellar proton irradiation. Though measurements on SiO2 and olivine allow for estimates of hydroxyl production on silicate bodies, they are only a small sampling of the variety of extant minerals in space and composed of only a single mineral type whereas extraterrestrial materials (e.g.…”

Section: Astrophysical Motivationmentioning

confidence: 76%

The Role of Solar Wind in the Formation of Hydroxyl on Airless Silicate Bodies in Space

Schaible

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Dedicated to all individuals who work for the betterment of themselves, their world, and their connection with the oneness that binds us all. To all my family and friends that have seen my needs and helped me to the position I am in, thank you. AbstractStudies of the interaction of solar radiation with the surfaces of moons, asteroids and comets can provide fundamental information about the early history of our solar system and help elucidate the ways in which such systems evolve. Airless bodies in space such as the Moon, asteroids and interplanetary dust particles are subject to bombardment from energetic solar wind electrons and ions, ultraviolet photons, micrometeorites and cosmic rays. This process is known as space weathering and the cumulative effect of the radiation modifies the chemical and physical nature of the ices and minerals that make up such surfaces. The work presented here investigates the interaction of solar wind hydrogen and helium with analog minerals and lunar soil using infrared spectroscopy (FTIR), mass spectrometry (SIMS), and optical photometry. Experiments were performed under Ultra High Vacuum (UHV) pressures and over a temperature range of 15 K to 400 K to simulate lunar surface conditions, and radiation was performed using a mass analyzed ion accelerator that allowed samples to be irradiated with specific ions at energies in the range of the solar wind.

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Water detection on atmosphereless celestial bodies: Alternative explanations of the observations

Cited by 98 publications

References 40 publications

Properties of the Hermean Regolith II. Disk-Resolved Multicolor Photometry and Color Variations of the “Unknown” Hemisphere

Properties of the Hermean Regolith II. Disk-Resolved Multicolor Photometry and Color Variations of the “Unknown” Hemisphere

Astronomical Observations of Volatiles on Asteroids

The Role of Solar Wind in the Formation of Hydroxyl on Airless Silicate Bodies in Space

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