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Solar System Ices and Icy Bodies
Researchers in this field conduct space-based observations and computational models to study the surfaces, interiors and atmospheres of the icy bodies. Research is performed in laboratory studies, space-based observations, theoretical modeling, data analysis, and instrumentation development with trials in terrestrial environments where possible.
Scientists are all but certain that Europa has an ocean underneath its icy surface, but they do not know how thick this ice might be. This artist concept illustrates two possible cut-away views through Europa's ice shell.
Ices are found in numerous locations in the universe and play a key role in the chemistry, physics and evolution of bodies within planetary systems. Researchers at JPL who study this field have with diverse backgrounds who investigate icy solar system bodies such as the outer planet icy moons, such as Europa, Ganymede, Enceladus, Titan, and Triton. Also of interest are comets along with the Martian and Earth polar regions as they assist in the understanding the formation and evolution of these solar and planetary systems.
Researchers conduct space-based observations to and computational models to study the surfaces, interiors and atmospheres of the icy bodies. Research is performed in laboratory studies, space-based observations, theoretical modeling, data analysis, and instrumentation development with trials in terrestrial environments where possible. Recently an NASA Astrobiology Institute (NAI) hyperlink to team lead by JPL was selected to study icy bodies in the solar system, including Europa, which has a sizable liquid ocean under an outer ice sheet. Liquid water is a key to life, which makes Europa a key object of exploration in the solar system.
Selected Research Efforts
Thermophysical, Rheological and Mechanical Measurements on Icy Compositions with Application to Solar System Ices
The purpose of the research project is to experimentally determine the thermophysical, rheological, and mechanical properties of icy materials (ices and candidate cryolavas) over a cryogenic temperature range (80 K < T < 300 K), which is applicable to outer solar system objects such as Jupiter’s and Saturn’s satellites, as well as Mars polar caps and terrestrial ice sheets. Using these material properties, modeling of satellites’ thermophysical, dynamical, and geological evolution was conducted, in order to support the following science objectives: (1) to model the physical mechanisms that are responsible for the cryovolcanic activity observed on Titan or inferred on other outer-planet icy worlds; (2) to model, for the first time, the geophysical response of icy satellites to tidal excitation; (3) to model the geological processes of icy satellites; and, (4) to determine the spectroscopic properties of ice samples in order to match the laboratory data with spacecraft observations. The research strives to understand the evolutionary history of planetary ices, in terms of the geophysical and geologic processes that have occurred in icy worlds around the solar system.
An Interdisciplinary Approach to the Evolutionary History of Planetary Ices
The outer solar system is populated by ice-rich bodies: comets, Kuiper Belt Objects, centaurs, “primitive” asteroids, and icy planetary satellites. The research objectie in this project is to study and develop an understanding of the physical chemistry of ices of the outer solar system.
Infrared spectra of unirradiated (blue) and irradiated (red) water-ice film containing isobutane. Note production of alcohols and CO2.
The outer-planet-satellite bulk surface icy compositions are predominantly water ice, with small amounts of co-condensed simple molecules such as NH3, CO2, CO, N2 and CH4, depending upon the condensation distance from the sun in the primordial solar nebula. It is these outer surfaces that respond to particle and photon bombardment from the sun, the solar wind, and charged particles trapped in local planetary magnetospheres, in addition to thermal cycling. The focus is on larger bodies of the outer solar system such as the Jovian and Saturnian icy moons. Inorganic, organic and biological compounds may be present on/in surface ices. Such species could be delivered to icy surfaces through meteoric impacts or, on bodies such as Europa and Enceladus, potentially through active chemistry in subsurface liquid water. The research investigates the temperature-dependant chemical pathways available to mixtures of ices and inorganic/organic compounds subjected to energetic stimuli relevant to the outer solar system.
This investigation includes performing a series of coordinated and synergistic laboratory experiments designed to elucidate the physical chemistry within ices relevant to icy solar system objects. The basic experimental approach is to engineer ice analogs constrained by model predictions and observations of solar system ices (composition, temperature, phase, structure, etc.). Once formed, the ices are systematically and quantitatively subjected to thermal cycling, UV photon irradiation and electron irradiation. A number of analytical methods are applied to unravel the chemical and physical changes occurring in the samples. The investigation directly addresses the objectives of JPL’s strategic initiative “Evolutionary History of Planetary Ices.” It addresses relevant questions such as: What are the essential chemical/physical properties of ices under conditions relevant to outer solar system ices? What kind of chemistry can occur in these ices? This project is providing precise, accurate, and quantitative descriptions of the physical chemistry that occurs in outer solar system ice analogs in order to lay a solid foundation for ground-truth understanding of observations obtained by JPL/NASA missions, e.g., Galileo ISS, UVS, NIMS & Cassini ISS, VIMS and UVIS observations.
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