Cold compaction of water ice

Durham, W. B.; McKinnon, William B.; Stern, Laura A.

doi:10.1029/2005gl023484

Cited by 56 publications

(56 citation statements)

References 17 publications

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“…This is supported by theory (Weidenschilling 1997;Wahlberg Jansson & Johansen 2014), remote observations (Weissman & Lowry 2008;Baer et al 2011), meteorite samples (Consolmagno et al 2008;Macke 2010), and laboratory experiments (Leliwa-Kopystyński et al 1994;Durham et al 2005;Yasui & Arakawa 2009). Jura & Xu (2010) assume that the bulk density of Ceres (2.1 g cm −3 ) represents the typical bulk density of small or intermediate sized icy bodies.…”

Section: Previous Studiesmentioning

confidence: 74%

Post-Main Sequence Evolution of Icy Minor Planets: Implications for Water Retention and White Dwarf Pollution

Malamud

Perets

2016

ApJ

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Most observations of polluted white dwarf atmospheres are consistent with accretion of water depleted planetary material. Among tens of known cases, merely two cases involve accretion of objects that contain a considerable mass fraction of water. The purpose of this study is to investigate the relative scarcity of these detections. Based on a new and highly detailed model, we evaluate the retention of water inside icy minor planets during the high luminosity stellar evolution that follows the main sequence. Our model fully considers the thermal, physical, and chemical evolution of icy bodies, following their internal differentiation as well as water depletion, from the moment of their birth and through all stellar evolution phases preceding the formation of the white dwarf. We also account for different initial compositions and formation times. Our results differ from previous studies, that have either underestimated or overestimated water retention. We show that water can survive in a variety of circumstances and in great quantities, and therefore other possibilities are discussed in order to explain the infrequency of water detections. We predict that the sequence of accretion is such that water accretes earlier, and more rapidly than the rest of the silicate disk, considerably reducing the chance of its detection in H-dominated atmospheres. In He-dominated atmospheres, the scarcity of water detections could be observationally biased. It implies that the accreted material is typically intrinsically dry, which may be the result of inside-out depopulation sequence of minor planets.

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Section: Previous Studiesmentioning

confidence: 74%

Post-Main Sequence Evolution of Icy Minor Planets: Implications for Water Retention and White Dwarf Pollution

Malamud

Perets

2016

ApJ

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“…The compaction experiments have been conducted on water ice, quartz sand, and mixtures of water ice and silicate materials [ Maeno , 1982; Durham et al , 2005; Karner et al , 2003; Leliwa‐Kopystynski et al , 1994]. Maeno [1982] studied the snow compaction process of the south polar glacier on Earth and found that the compaction process can be divided into four stages on the basis of the slope of the density profile.…”

Section: Introductionmentioning

confidence: 99%

“…According to this theory, compaction depends on several factors such as temperature, stress, and grain size. Furthermore, Durham et al [2005] performed compaction experiments on water ice using icy grains of various sizes at temperatures of −153 and −196°C; they found that the compaction behavior, represented as the relationship between pressure and density, was explained by the failure of the ice grain and was independent of temperature and ice grain size. Karner et al [2003] performed hydrostatic compaction experiments of quartz sands and found that the compaction mechanisms changed with pressure; these mechanisms involve rearrangement, elastic deformation, and cracking and failure.…”

Section: Introductionmentioning

confidence: 99%

Compaction experiments on ice‐silica particle mixtures: Implication for residual porosity of small icy bodies

Yasui

Arakawa

2009

J. Geophys. Res.

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[1] To evaluate the residual porosity of small icy bodies, we performed compaction experiments on ice-silica mixtures and studied the effects of silica content, temperature, and compaction time scale on residual porosity. To simulate the compositions of real icy bodies, we used ice-silica mixtures with different silica volume fractions (0-0.29). The mixtures were compacted at a constant compression speed of 0.2 or 2.0 mm/min and the temperature was set to À10°C or a lower temperature (from À55 to À67°C). For the À10°C case, the mixtures were compressed to pressures of 30 MPa, while the lower temperature measurements were compressed to 80 MPa. In both cases, the residual porosity was found to be larger for higher silica fractions. At À10°C and 30 MPa, the residual porosity varied from 0.01 to 0.14 for silica fractions of 0-0.29, whereas for the À55 to À67°C and 80 MPa case, the corresponding residual porosities were 2-10 times larger. A two-layer model was proposed to calculate the compaction curves of ice-silica mixtures from the curves of the corresponding pure materials. We estimated the residual porosity of small icy bodies using this two-layer model. From our calculations, we expect that icy bodies with diameters smaller than 700 km have residual porosity larger than 0.3 when the temperature is lower than À55°C.Citation: Yasui, M., and M. Arakawa (2009), Compaction experiments on ice-silica particle mixtures: Implication for residual porosity of small icy bodies,

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“…Orcus is then assumed to have a 475 km radius, a 19.9% albedo , and a bulk density of 1900 kg m −3 . By assuming a residual porosity of 10% (Durham et al 2005), this density leads to a mixture made of 77% of dust and 23% of water ice (mass fractions), the dust being homogeneously distributed within the ice matrix. The resulting thermal properties are: the thermal conductivity κ = 0.18 Wm −1 K −1 , the heat capacity c = 10 3 Jkg −1 K −1 .…”

Section: The Modelmentioning

confidence: 99%

Methane, ammonia, and their irradiation products at the surface of an intermediate-size KBO?

Delsanti¹,

Merlin²,

Guilbert-Lepoutre³

et al. 2010

A&A

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Orcus is an intermediate-size 1000 km-scale Kuiper belt object (KBO) in 3:2 mean-motion resonance with Neptune, in an orbit very similar to that of Pluto. It has a water-ice dominated surface with solar-like visible colors. We present visible and near-infrared photometry and spectroscopy obtained with the Keck 10 m-telescope (optical) and the Gemini 8 m-telescope (near-infrared). We confirm the unambiguous detection of crystalline water ice as well as absorption in the 2.2 μm region. These spectral properties are close to those observed for Pluto's larger satellite Charon, and for Plutino (208996) 2003 AZ 84 . Both in the visible and near-infrared Orcus' spectral properties appear to be homogeneous over time (and probably rotation) at the resolution available. From Hapke radiative transfer models involving intimate mixtures of various ices we find for the first time that ammonium (NH + 4 ) and traces of ethane (C 2 H 6 ), which are most probably solar irradiation products of ammonia and methane, and a mixture of methane and ammonia (diluted or not) are the best candidates to improve the description of the data with respect to a simple water ice mixture (Haumea type surface). The possible more subtle structure of the 2.2 μm band(s) should be investigated thoroughly in the future for Orcus and other intermediate size Plutinos to better understand the methane and ammonia chemistry at work, if any. We investigated the thermal history of Orcus with a new 3D thermal evolution model. Simulations over 4.5×10 9 yr with an input 10% porosity, bulk composition of 23% amorphous water ice and 77% dust (mass fraction), and cold accretion show that even with the action of long-lived radiogenic elements only, Orcus should have a melted core and most probably suffered a cryovolcanic event in its history which brought large amounts of crystalline ice to the surface. The presence of ammonia in the interior would strengthen the melting process. A surface layer of a few hundred meters to a few tens of kilometers of amorphous water ice survives, while most of the remaining volume underneath contains crystalline ice. The crystalline water ice possibly brought to the surface by a past cryovolcanic event should still be detectable after several billion years despite the irradiation effects, as demonstrated by recent laboratory experiments.

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Cold compaction of water ice

Cited by 56 publications

References 17 publications

Post-Main Sequence Evolution of Icy Minor Planets: Implications for Water Retention and White Dwarf Pollution

Post-Main Sequence Evolution of Icy Minor Planets: Implications for Water Retention and White Dwarf Pollution

Compaction experiments on ice‐silica particle mixtures: Implication for residual porosity of small icy bodies

Methane, ammonia, and their irradiation products at the surface of an intermediate-size KBO?

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