Internal structure of Europa and Callisto

Kuskov, O. L.; Kronrod, V. A.

doi:10.1016/j.icarus.2005.04.014

Cited by 117 publications

(81 citation statements)

References 73 publications

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“…3). Deep ocean waters of Pluto, and an at least partly differentiated Callisto, would also exceed 0.2 GPa (Spohn and Schubert, 2003;Kuskov and Kronrod, 2005;Hammond et al, 2016). As in Europa, the existence of a thick saline subsurface ocean in Callisto is indicated by a conductive layer at a depth of less than about 300 km inferred from magnetic field perturbations observed by the Galileo spacecraft (Zimmer et al, 2000).…”

Section: Implications For Planetary Oceans and Interiorsmentioning

confidence: 99%

“…The salts of planetary oceans are acquired chiefly from sub-seafloor weathering reactions (Zolotov and Shock, 2001). About 75 % of the salts produced by low-temperature aqueous alteration of chondrite under oxidising conditions are magnesium sulphate hydrates (Hogenboom et al, 1995 et al, 2012), Europa (Spohn and Schubert, 2003;Hand and Chyba, 2007;Valenti et al, 2012), Ganymede (Vance et al, 2014;Saur et al, 2015), and Callisto (Kuskov and Kronrod, 2005) with approximate depths of the subsurface ocean boundaries in km. The shadowed band is the pressure range of the LDW-HDW transition at about 20 °C (Fanetti et al, 2014).…”

Section: Implications For Planetary Oceans and Interiorsmentioning

confidence: 99%

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Pressure-induced ion pairing in MgSO4 solutions: Implications for the oceans of icy worlds

Schmidt¹,

Manning²

2016

Geochem. Persp. Let.

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At ambient temperature, liquid water transforms from a low-density to a high-density dynamic structure at ~0.2 GPa. The transition persists in electrolyte solutions; however, its effects on solute properties are unknown. We obtained Raman spectra of 0.5-2.0 molal MgSO 4 solutions at 21 °C and 10 -4 to ~1.6 GPa. Above about 0.4 GPa, we observed an increase in the MgSO 4 contact ion pair abundance with pressure, regardless of concentration. This phenomenon contravenes the general rule that dissolved salts dissociate upon compression, and is likely caused by the structural collapse in the solvent with pressure due to increased hydrogen-bond breaking. Increasing ion association in high-pressure aqueous solutions implies that, at a given salinity, high-density water in deep, cold planetary oceans and pore waters will possess lower ionic strength and electric conductivity than previously thought. This behaviour will also lead to higher ocean salinity in the interiors of Pluto and the largest icy moons of Jupiter and Saturn, Ganymede, Callisto, and Titan, or in exoplanet water-worlds, through enhancement of submarine silicate weathering.

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Section: Implications For Planetary Oceans and Interiorsmentioning

confidence: 99%

Section: Implications For Planetary Oceans and Interiorsmentioning

confidence: 99%

Pressure-induced ion pairing in MgSO4 solutions: Implications for the oceans of icy worlds

Schmidt¹,

Manning²

2016

Geochem. Persp. Let.

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“…In fact, we need look no further than our own solar system, where we might have two cases. Both Jupiter's moon Europa (e.g., Kuskov and Kronrod, 2005), and more recently Saturn's moon Enceladus (Spencer et al, 2006), show evidence of liquid water underneath their ice crusts, produced by tidal heating due to their host planets. Potentially, there could be more bizarre cases: for example, imagine a hypothetical rocky planet inside the inner boundary of the HZ and tidally locked to the star.…”

Section: Water and Lifementioning

confidence: 99%

Transit Spectroscopy of the Extrasolar Planet HD 209458b: The Search for Water

Rojo

Harrington²,

Zeehandelaar³

et al. 2004

AIP Conference Proceedings

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This dissertation describes an attempt to detect water in the atmosphere of the extrasolar planet HD 209458b using transit spectroscopy. It first discusses the importance of water detection and reviews the state of knowledge about extrasolar planets. This review discusses the main statistical trends and describes the detection methods employed to this date. The importance of the transiting planets and the many measurements of the known ones are also discussed.A radiative transfer model designed and built specifically for this project predicts, given a planetary temperature/pressure/composition profile, the dependence in wavelength of the stellar spectrum modulation due to a transiting planet. A total of 352 spectra around 1.8 µm were obtained on four nights (three in transit) of observations on August 3-4, September 26, and October 3 of 2002 using ISAAC at the Very Large Telescope.Correlating the modeled modulation with the infrared spectra yields a nondetection of water in the atmosphere of HD 209458b. It is found that the nondetection is due to an unfortunate choice of observing parameters and conditions that made it impossible to reach the required sensitivity. Nonetheless, the results are scaled with synthetic spectra to place strong limits on the planetary system configurations for which the observing parameters and telluric conditions would have yielded a successful detection. None of the 10 other known transiting planets would be detectable with the choice of parameters and conditions for this observation.A quantitative model of an improved observing strategy for future observations of this kind is developed. The improvements include: airmass and timing constraints, the simultaneous observation of a calibrator star, and a new method to find the optimal wavelength range.The data-reduction process includes several original techniques that were developed during this work, such as a method to remove fringes from flat fields and several methods to correct for telluric absorption, among others.

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“…Ganymede can be differentiated as an iron core, rock mantle, and icy mantle (Showman and Malhotra, 1999). On the other hand, only a partial differentiation between ice and rock can be made for Callisto (Kuskov and Kronrod, 2005). The most probable scenario for ice-rock differentiation is the gravitational settling of silicate particles after the melting of the silicate-ice mixture in the object.…”

Section: Introductionmentioning

confidence: 99%

Differentiation of silicates from H2O ice in an icy body induced by ripening

Sirono

2013

Earth Planet Sp

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One of the probable scenarios of differentiation between silicate-ice in an icy object is the settling of a silicate particle in water after the melting of the object. In order for settling to proceed or occur, the size of the particle should be sufficiently large such that the settling velocity of the particle exceeds the background flow velocity induced by thermal convection. The sizes of the particles change because of dissolution and precipitation. This process is called ripening. In this study, the critical particle sizes required for settling, and the timescales for the growth of the particles to these sizes through ripening, are analytically derived. It is observed that settling is possible if the silicate particles coagulate with each other to form a network in water. If the particles do not coagulate, the probability of the occurrence of settling is low, because the time duration required for the particle growth to the critical size is large. The coagulation of silicate particles strongly depends on the pH of the water.

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Internal structure of Europa and Callisto

Cited by 117 publications

References 73 publications

Pressure-induced ion pairing in MgSO4 solutions: Implications for the oceans of icy worlds

Pressure-induced ion pairing in MgSO4 solutions: Implications for the oceans of icy worlds

Transit Spectroscopy of the Extrasolar Planet HD 209458b: The Search for Water

Differentiation of silicates from H2O ice in an icy body induced by ripening

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