scholarly journals Production of Oxidants by Ion Bombardment of Icy Moons in the Outer Solar System

2011 ◽  
Vol 2011 ◽  
pp. 1-10 ◽  
Author(s):  
Philippe Boduch ◽  
Enio Frota da Silveira ◽  
Alicja Domaracka ◽  
Oscar Gomis ◽  
Xue Yang Lv ◽  
...  
Keyword(s):  
Carbon Dioxide ◽  
Hydrogen Peroxide ◽  
Solar System ◽  
Ion Irradiation ◽  
Pure Water ◽  
Outer Solar System ◽  
Water Ice ◽  
Icy Moons ◽  
Different Temperatures ◽  
Frozen Gases

Our groups in Brazil, France and Italy have been active, among others in the world, in performing experiments on physical-chemical effects induced by fast ions colliding with solids (frozen gases, carbonaceous and organic materials, silicates, etc.) of astrophysical interest. The used ions span a very large range of energies, from a few keV to hundreds MeV. Here we present a summary of the results obtained so far on the formation of oxidants (hydrogen peroxide and ozone) after ion irradiation of frozen water, carbon dioxide and their mixtures. Irradiation of pure water ice produces hydrogen peroxide whatever is the used ion and at different temperatures. Irradiation of carbon dioxide and water frozen mixtures result in the production of molecules among which hydrogen peroxide and ozone. The experimental results are discussed in the light of the relevance they have to support the presence of an energy source for biosphere on Europa and other icy moons in the outer Solar System.

Electron-induced radiolysis and sputtering on the surface of icy moons: insights from laboratory experiments

2020 ◽  
Author(s):  
André Galli ◽  
Romain Cerubini ◽  
Martin Rubin ◽  
Antoine Pommerol ◽  
Audrey Vorburger ◽  
...  
Keyword(s):  
Grain Size ◽  
Solar System ◽  
Mass Spectrometer ◽  
Laboratory Experiments ◽  
Pure Water ◽  
Theoretical Modelling ◽  
Release Process ◽  
Water Ice ◽  
Icy Moons ◽  
Radiolysis Products

<p><strong>Abstract</strong></p> <p>The surfaces of Jupiter's icy moons are continually irradiated by charged particles from the Jovian plasma environment. This irradiation triggers chemical reactions in the surface ice and also acts as an atmospheric release process. Remote observations, theoretical modelling, and laboratory experiments must be combined to understand<br />this plasma-ice interaction. Here, we present new experiment results concerning the chemistry of irradiated water ice samples relevant for icy moons and other icy objects in the solar system. </p> <p><strong>Introduction</strong></p> <p>The University of Bern is developing the neutral gas mass spectrometer for ESA's Jupiter Icy moons Explorer (JUICE, Grasset et al. 2013), <br />planned to reach the Jupiter system in 2029. We therefore strive to fill knowledge gaps about the basic physics of the surfaces and atmospheres of Jupiter’s icy moons before the arrival of JUICE. We combine the available facilities for developing and calibrating mass spectrometers and ion/electron spectrometers (Marti et al. 2001) with the sample preparation techniques and diagnostics of the Planetary Imaging Group (Pommerol et al. 2019).</p> <p><strong>Experiment setup</strong></p> <p>To study the effects of electrons irradiating water ice, we subjected a variety of ice samples (thin amorphous ice films and macroscopic samples of porous ice with customizable grain size) to an electron beam of energies between 200 eV and 10 keV at pressures and temperatures representative for the surfaces of Jupiter's icy moons. The physical and optical properties of these macroscopic ice samples make them realistic analogues for planetary surfaces beyond the ice line. The effect of chemical impurities in the water ice, such as NaCl, can also be investigated. The particles released from the ice were monitored with a newly designed time-of-flight (TOF) mass spectrometer and (in the case of the water ice film) with a microbalance. </p> <p><strong>Preliminary results</strong></p> <p>Electron irradiation of pure water ice results mostly in the creation and release of H<sub>2</sub> and O<sub>2</sub> from H<sub>2</sub>O in a stoichiometric 2:1 ratio, which is in agreement with the results based on an older quadrupole mass spectrometer (Galli et al. 2018). This seems to hold true for any type of water ice sample, independent of grain size and crystallinity. We also derive upper limits for rare radiolysis products (such as OH and H<sub>2</sub>O<sub>2</sub>) and the time scales for the build-up and release of radiolysis products. The O<sub>2</sub> release lags behind the immediate H<sub>2</sub> release by typically ~ 10 s and is reminiscent of the time-dependent sputtering yield of O<sub>2</sub> from water ice upon ion irradiation (Teolis et al. 2005). This delayed O<sub>2</sub> release has implications for the O<sub>2</sub>/H<sub>2</sub>O ratio observed at the surface of icy objects in the solar system, such as Ganymede, Europa, Callisto (Calvin et al. 1996, Spencer and Calvin 2002), and 67P/Churyumov-Gerasimenko (Bieler et al. 2015).</p>

Nitrogen condensation on water ice

2003 ◽  
Vol 81 (1-2) ◽  
pp. 217-224 ◽  
Author(s):  
M E Palumbo ◽  
G Strazzulla
Keyword(s):  
Narrow Band ◽  
Ion Irradiation ◽  
Pure Water ◽  
Kuiper Belt ◽  
Outer Solar System ◽  
Infrared Absorption Spectroscopy ◽  
Dangling Bonds ◽  
Warm Up ◽  
Water Ice ◽  
Water Band

We studied, by infrared absorption spectroscopy, icy samples (16 K) of pure water, a mixture N2:H2O=100:1, and a sample made of N2 condensed on water ice and diffused in it after warm up to 30 K. We concentrated our efforts in two spectral regions around 3700 cm–1 where the feature due to the O–H dangling bonds in porous amorphous water falls and around 5000 cm–1 where a broad water band is present. We found that in the N2:H2=100:1 mixture the profile of the broad water feature at about 5000 cm–1 dramatically changed to a very narrow band at about 5300 cm–1. When N2 diffuses in water ice a feature at about 5300 cm–1 appears along with the broad 5000 cm–1 band. We also studied some of the effects of ion irradiation (Ar++, 60 keV ions) on these icy samples. We found that after processing the feature due to the O–H dangling bonds it reduced in intensity and eventually disappeared. Here we present the experimental results, discuss their astrophysical relevance and suggest that a band at about 5300 cm–1 (1.88 µm) should be searched for on icy surfaces in the outer Solar System, namely Pluto, Triton, Edgeworth–Kuiper Belt Objects, and Centaurs. PACS No.: 68.43Pg

Radiation Effects in Water Ice in the Outer Solar System

2012 ◽  
pp. 527-549 ◽  
Author(s):  
R. A. Baragiola ◽  
M. A. Famá ◽  
M. J. Loeffler ◽  
M. E. Palumbo ◽  
U. Raut ◽  
...  
Keyword(s):  
Solar System ◽  
Radiation Effects ◽  
Outer Solar System ◽  
Water Ice

Radiolysis of N2-rich astrophysical ice by swift oxygen ions: implication for space weathering of outer solar system bodies

2017 ◽  
Vol 19 (35) ◽  
pp. 24154-24165 ◽  
Author(s):  
F. A. Vasconcelos ◽  
S. Pilling ◽  
W. R. M. Rocha ◽  
H. Rothard ◽  
P. Boduch
Keyword(s):  
Solar System ◽  
Ion Irradiation ◽  
Space Weathering ◽  
Outer Solar System ◽  
Oxygen Ions ◽  
Solar System Bodies

We reported results for ion irradiation of N2-rich ices with implications for space weathering of outer solar bodies.

Ammonia–water ice laboratory studies relevant to outer Solar System surfaces

Icarus ◽  
2007 ◽  
Vol 190 (1) ◽  
pp. 260-273 ◽  
Author(s):  
M.H. Moore ◽  
R.F. Ferrante ◽  
R.L. Hudson ◽  
J.N. Stone
Keyword(s):  
Solar System ◽  
Outer Solar System ◽  
Laboratory Studies ◽  
Ammonia Water ◽  
Water Ice

Ion irradiation of acetylene ice in the ISM and the outer Solar system: laboratory simulations

2020 ◽  
Vol 495 (1) ◽  
pp. 40-57
Author(s):  
R C Pereira ◽  
A L F de Barros ◽  
C A P da Costa ◽  
P R B Oliveira ◽  
D Fulvio ◽  
...  
Keyword(s):  
Solar System ◽  
Cross Section ◽  
Cross Sections ◽  
Ion Irradiation ◽  
Galactic Cosmic Rays ◽  
Young Stellar Objects ◽  
Outer Solar System ◽  
Stellar Objects ◽  
Important Species ◽  
H Beam

ABSTRACT)3 Acetylene, C2H2, has been observed in the interstellar medium, mostly around young stellar objects, as well as in molecular clouds and cometary comae, representing an important species of astrophysical interest. In this work, we present a laboratory study of the C2H2 radiolysis at 45 K for three different beams and energies: 1.0 MeV H+ and He+, and 1.0 and 1.5 MeV N+ beams. Fourier transform infrared spectroscopy was used for monitoring the molecular changes induced by the ion processing. Two different sample thicknesses were irradiated; for the thicker one, implantation had occurred. Spectra and absorbance evolutions for the thin and thick films are qualitatively different. Four C2H2 bands are observed at 3225, 1954, 1392, and 763 cm−1. The C2H2 compaction and apparent destruction cross-sections are determined. For the case of the H+ beam, the compaction cross-section dominates. Concerning molecular synthesis by irradiation, New product bands were not observed in the thin ice irradiations; for the thicker film ice, the daughter species CH4, C2H4, C3H6, and C4H4 have been identified and their destruction and formation cross-sections determined. The apparent destruction cross-section was found to be a function of the electronic stopping power (Se) as σd ∝ S$_\mathrm{ e}^{3/2}$. The half-life of the C2H2 bombarded by galactic cosmic rays is estimated. The current findings are a contribution to the understanding of how the molecules synthesized upon irradiation of Interstellar and outer Solar system ices participate to the molecular enrichment and to the physicochemical evolution of the Universe.

scholarly journals Organic chemistry in planetary satellites of gas giants and implications for habitability

2015 ◽  
Vol 11 (A29B) ◽  
pp. 421-425
Author(s):  
Athena Coustenis
Keyword(s):  
Organic Chemistry ◽  
Solar System ◽  
Outer Solar System ◽  
Icy Moons ◽  
Planetary Satellites

AbstractWe look at the icy moons in our outer solar system in which we find organics and the possibility for habitabile conditions therein.

scholarly journals Neptune’s Triton: A Moon Rich in Dry Ice and Carbon?

1990 ◽  
Vol 8 (04) ◽  
pp. 364-367 ◽  
Author(s):  
A. J. R. Prentice
Keyword(s):  
Chemical Composition ◽  
Solar System ◽  
Catalytic Synthesis ◽  
Outer Solar System ◽  
Solid Carbon ◽  
Convective Turbulence ◽  
Water Ice ◽  
Large Satellite ◽  
Unique Composition ◽  
Crucial Test

AbstractThe encounter of the spacecraftVoyager 2with Neptune and its large satellite Triton in August 1989 will provide a crucial test of ideas regarding the origin and chemical composition of the outer solar system. In this pre-encounter paper we quantify the possibility that Triton is a captured moon which, like Pluto and Charon, originally condensed as a major planetesimal within the gas ring that was shed by the contracting protosolar cloud at Neptune’s orbit. Ideas of supersonic convective turbulence are used to compute the gas pressure, temperature and rate of catalytic synthesis of CH4, CO2and solid carbon within the protosolar cloud, assuming that all C is initially present as CO. The calculations lead to a unique composition for Triton, Pluto, and Charon: each body consists of, by mass, 18.5% solid CO2ice, 4% graphite, 0.5% CH4ice, 29% methanated water ice and 48% anhydrous rock. This mix has a density consistent with that of the Pluto-Charon system and yields a predicted mean density for Triton of 2.20±0.05 g cm−3, for satellite radius equal to 1750 km.

Structural and Thermal Icy Satellite Models: Preliminary Results

1984 ◽  
Vol 5 (4) ◽  
pp. 487-489
Author(s):  
P. J. Thomas
Keyword(s):  
Melting Point ◽  
Solar System ◽  
Methane Hydrates ◽  
Outer Solar System ◽  
Water Ice ◽  
Preliminary Results

The satellites of the outer solar system appear to be composed principally of water ice and silicates, with the presence of ammonia and methane hydrates (Lewis 1971). Although these bodies are small (with radii typically < 1000 km) they can exhibit very active evolutionary histories, due to the low melting point of water ice.

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