The ammonia-water phase diagram and its implications for icy satellites

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National Aeronautics and Space Administration, National Technical Information Service, distributor , [Washington, D.C, Springfield, Va
Other titlesAmmonia water phase diagram and its implications for icy satellites
StatementMary L. Johnson and Malcolm Nicol
SeriesNASA contractor report -- NASA CR-179881
ContributionsNicol, Malcolm F, United States. National Aeronautics and Space Administration
The Physical Object
Pagination1 v
ID Numbers
Open LibraryOL18007211M

Full text of "The ammonia-water phase diagram and its implications for icy satellites" See other formats The Ammoni* - W*t«r Ph*««Di*9r»m and Its Implications -for Icy Satel 1 i t»s Mary L. Johnson and Malcolm Nicol Department o-f Chemistry and Biochemistry, University o-f Cali-fornia, Los Angeles, CA {N&SA-CE) IHE aMMONIA-WATEE PHASE N DIAGRAM AND IIS.

Get this from a library. The ammonia-water phase diagram and its implications for icy satellites. [Mary L Johnson; Malcolm F Nicol; United States. National Aeronautics and Space Administration.]. () described parts of the ammonia-water phase diagram and their implications for icy satellites. This report was based on experimental obse:Ivations of (~)x(H20)1.x mixtures for 0 $ X $ in diamond-anvil cells at pressures from 0 GPa to GPa and at temperatures from K to K When.

We performed high-pressure experiments on the crystallization of water ice I and III in the ammonia–water (NH 3) x (H 2 O) (1−x) system, and apply the results to the interiors of icy bodies in the Solar System. Phase equilibrium lines between an entirely liquid solution and a liquid solution in which water ice forms (liquidus lines) were determined for ammonia The ammonia-water phase diagram and its implications for icy satellites book by mass X equal Cited by: The (NH_3)x(H_20)_(1.x) phase diagram for 0 ≤ X ≤ has been reexamined at temperatures from K to K and at pressures to GPa using diamond-anvil cells.

By electroplating the gasket materials with gold, complicated reactions between sample solutions and gasket materials, which affected earlier studies, have been avoided. Sample pressures were determined using the ruby. The Ammonia–Water System and the Chemical Differentiation of Icy Satellites M.

NicolThe ammonia–water phase diagram and its implications for icy satellites. Geophys. Res., 92 (), pp. J.S. KargelAmmonia–water volcanism on icy satellites: Phase relations at 1 atmosphere. Icarus, (), pp. Cited by: After reviewing some important aspects of the internal dynamics of the large icy satellites of Jupiter and Saturn, this paper describes the phase diagram of water ice and its variations due to the presence of other chemical compounds.

Values of the elastic parameters Cited by: We report the discovery of the first high-pressure polymorphs of ammonia hydrates: ammonia monohydrate II and ammonia dihydrate II.

The subsolidus transitions and melting curves of these substances are shown by their volume-temperature functions; uncalibrated calorimetry corroborates these phase changes. From 20 to MPa ammonia dihydrate and ice melt at a eutectic to form. phase diagram of ammonia–water mi xtures in order to verify the many detai ls of the plot.

They might in this way find that the phase beha vior of this system has been discussed. Phase diagram of the AsS system. CaGeO3-SrSiO3 by methods of physicochemical analysis and its phase diagram was constructed.

this new model for thermal and evolution models of icy satellites. Ammonia–water ice laboratory studies relevant to outer Solar System radiation-processing, and phase (crystalline or amorphous) of the components were examined. Ammonia ice and icy satellites Table 1 Estimated particle radiation doses for selected icy File Size: KB.

Figure 4 C/MR 2 as a function of fractional core radius x at fixed J 2 / q = for the exactly solvable model of a core of density A and radius x, overlain by an envelope of density 1 between radius x and radius 1. Models to the left correspond to cores of extremely high density (but finite envelope density); models to the right end point correspond to models where the density of the.

Water- and ammonia-ices have been observed or postulated as important components of the icy surfaces of planetary satellites and KBO objects in the outer Solar System.

A feature in the near-infrared, near microns, is attributed to NH3 in the spectra of Charon, Quaoar, and Miranda, a possible source being cryomagma brought up to cold. An ammonia-water slurry may swirl below Pluto’s icy surface A geologically active surface that buries craters and raises mountains means the mantle that lies below is moving.

One of the most interesting properties of ammonia for a planetary context is its profound anti-freezing effect. As shown in the equilibrium phase diagram (), the liquidus on the H 2 O–NH 3 phase diagram is the temperature-versus-composition curve above which the solution is entirely solidus is, in the case of this simple binary system, the horizontal line, or isotherm, below which Author: Christine McCarthy, Michael A.

Nielson, Allie N. Coonin, Jessica Shea Minker, Armando A. Domingos.

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A preliminary phase diagram for the high pressure ammonia-water system is constructed using new data of Johnson et al. These results imply that 1) clathrate is stable throughout the interior of Oberon- and Rhea-sized icy satellites, and 2) clathrate incorporated in the inner-most icy regions of Titan would have decomposed, perhaps Cited by: 2.

An ammonia-water slurry may swirl below Pluto's icy surface November 9, WEST LAFAYETTE, Ind. — Researchers propose an ammonia-water slurry as the basis for Pluto's newly discovered geologic activity and possible volcanism, and offer a new method to predict planetary vigor.

The vast repertoire of metabolism and physiology allows different kinds of terrestrial microbes to colonize diverse environments. Because of niche competition, individual taxa have evolved to grow optimally under a limited range of conditions.

For example, microbes that grow optimally at –15°C do. Grasset O, Pargamin J () The ammonia-water system at high pressures: implications for the methane of Titan. Planet Space Sci – ADS Google Scholar Greve R, Mahajan RA () Influence of ice rheology and dust content on the dynamics of the north-polar cap of by: Solid lines represent pure H 2 O phase diagram, with different phases marked with Roman numerals.

Dashed lines represent melting curve of H 2 O plus 5% or 15% ammonia. Thin solid red and blue dashed lines show hypothetical thermal profiles, illustrating how a liquid layer may develop between low‐ and high‐pressure solid by: The phase of the Moon at the time of a solar eclipse: be new.

can be any phase, new, quarter, or full. ammonia, water vapor, and carbon dioxide in about equal amounts. d% nitrogen, and 21% oxygen.

chunks of water and methane ice ejected from the surface of the icy satellites of the outer planets by asteroid impacts. 4 A Geophysical Perspective and Inventory of Habitable Environments on Icy Bodies.

The geophysical context of solar system objects constrains the potential propagation of terrestrial organisms with known minimal nutritional requirements and environmental tolerances as outlined in Chapter outer solar system contains a broad diversity of icy bodies, ranging from co-accreted satellites.

The Microwave Opacity of Ammonia and Water Vapor: Application to Remote Sensing of the Atmosphere of Jupiter Paperback – Febru by Thomas R. Hanley (Author) See all formats and editions Hide other formats and editions.

Price New from Used from Cited by: 8. Hogenboom experimented with 6 concentration levels of ammonia/water (10, 20, and %), with pressures from 0 to 4, MPa and temperatures from to Kelvin. Additionally, ammonia extrudes from water ice differently when there are other minerals or salts present than when there is a simple ammonia water relationship.

While studying Moons of our Solar System you have the option to work towards gaining a digital badge. Badged courses are a key part of The Open University’s mission to promote the educational well-being of the courses also provide another way of.

Calculate online thermodynamic and transport properties of ammonia. Rent-To-Own program NEW. The value of each subscription you purchase (1 or more) can be applied as a discount towards a purchase of the full license of our related NH3 Tables desktop software (NH3Tables Excel Add-In).This also applies retroactively for all subscriptions since the beginning of Start studying Chapter 8: Jovian Planet Systems.

Learn vocabulary, terms, and more with flashcards, games, and other study tools. they differ in phase (such as liquid or gas) of their hydrogen. This moon may hide a hidden deep ocean of liquid water between its rocky mantle and its icy crust.

Description The ammonia-water phase diagram and its implications for icy satellites FB2

Europa. The largest moon in the solar system. Like the Moon and many satellites that orbit the other gas giants, its rotational period is identical to its orbital period.

Thus, Titan is tidally-locked and in a synchronous rotation with Saturn. The text accompanying the image used in this article clearly states Saturn's moon Enceladus is only kilometers ( miles) across, small enough to fit within the length of the United Kingdom, as illustrated here.

The intriguing icy moon also could fit comfortably within the states of Arizona or Colorado.

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This is a faithful reproduction of the text on the original NASA photo. Figure 5 is an icy moon of Uranus, km in diameter. It was discovered in by the same man who discovered Triton – William Lassell.

The straight-sided troughs that cross its surface are probably defined by pairs of faults, and the smooth material on their floors may have been erupted as flows of an ammonia–water mixture. Figure 5 Ariel. The Lewis dot drawing makes it clear that nitrogen has completed its octet with 3 covalent bonds with hydrogen and 1 lone pair.

Nitrogen now with its full octet of valence electrons is isoelectric with the noble gas neon. Hydrogen with 2 electrons in its outer shell is .ammonia and water ices – Due to pressure deep in the interior, hydrogen is compressed first into liquid, then into a liquid metal – Jupiter’s four largest moons range in size from slightly larger than Mercury (Ganymede) to about the size of Earth’s moon (Europa) • – Due to pressure deep in the interior, hydrogen is compressed first into liquid.ammonia-water mixture with different heat sources [17–21].

In this study, the layout was kept in a simple form with one separator and two recuperators as it was compared with the most basic Rankine cycle. With reference to Fig. 2, the working solution ammonia-water mixture entering the turbine (stream 1) .