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

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.

scholarly journals Search for water and life's building blocks in the Universe

2015 ◽  
Vol 11 (A29B) ◽  
pp. 375-375
Author(s):  
Sun Kwok ◽  
Edwin Bergin ◽  
Pascale Ehrenfreund
Keyword(s):  
Solar System ◽  
Common Ground ◽  
Kuiper Belt ◽  
Building Blocks ◽  
Planetary Science ◽  
Dust Particles ◽  
Outer Solar System ◽  
Water Ice ◽  
Solar System Bodies ◽  
Solid Bodies

Water is the common ground between astronomy and planetary science as the presence of water on a planet is universally accepted as essential for its potential habitability. Water assists many biological chemical reactions leading to complexity by acting as an effective solvent. It shapes the geology and climate on rocky planets, and is a major or primary constituent of the solid bodies of the outer solar system. Water ice seems universal in space and is by far the most abundant condensed-phase species in our universe. Water-rich icy layers cover dust particles within the cold regions of the interstellar medium and molecular ices are widespread in the solar system. The poles of terrestrial planets (e.g. Earth, Mars) and most of the outer-solar-system satellites are covered with ice. Smaller solar system bodies, such as comets and Kuiper Belt Objects (KBOs), contain a significant fraction of water ice and trace amounts of organics. Beneath the ice crust of several moons of Jupiter and Saturn liquid water oceans probably exist.

ION IRRADIATION OF H2-LADEN POROUS WATER-ICE FILMS: IMPLICATIONS FOR INTERSTELLAR ICES

2015 ◽  
Vol 811 (2) ◽  
pp. 120 ◽  
Author(s):  
U. Raut ◽  
E. H. Mitchell ◽  
R. A. Baragiola
Keyword(s):  
Ion Irradiation ◽  
Water Ice ◽  
Ice Films ◽  
Interstellar Ices

scholarly journals Water Ice on the Satellite of Kuiper Belt Object 2003 EL 61

2006 ◽  
Vol 640 (1) ◽  
pp. L87-L89 ◽  
Author(s):  
K. M Barkume ◽  
M. E. Brown ◽  
E. L. Schaller
Keyword(s):  
Kuiper Belt ◽  
Kuiper Belt Object ◽  
Water Ice

Formation of CO and CO2Molecules by Ion Irradiation of Water Ice–covered Hydrogenated Carbon Grains

2004 ◽  
Vol 615 (2) ◽  
pp. 1073-1080 ◽  
Author(s):  
V. Mennella ◽  
M. E. Palumbo ◽  
G. A. Baratta
Keyword(s):  
Ion Irradiation ◽  
Water Ice

Crystalline water ice on the Kuiper belt object (50000) Quaoar

Nature ◽  
2004 ◽  
Vol 432 (7018) ◽  
pp. 731-733 ◽  
Author(s):  
David C. Jewitt ◽  
Jane Luu
Keyword(s):  
Kuiper Belt ◽  
Kuiper Belt Object ◽  
Water Ice ◽  
Crystalline Water

scholarly journals Parameterisations of interior properties of rocky planets

2020 ◽  
Vol 638 ◽  
pp. A129 ◽  
Author(s):  
Lena Noack ◽  
Marine Lasbleis
Keyword(s):  
Thermodynamic Properties ◽  
Scaling Laws ◽  
Thermal State ◽  
Thermal Evolution ◽  
Pure Water ◽  
Mass Composition ◽  
Temperature Profiles ◽  
Interior Structure ◽  
Water Ice ◽  
Simple Mass

Context. Observations of Earth-sized exoplanets are mostly limited to information on their masses and radii. Simple mass-radius relationships have been developed for scaled-up versions of Earth or other planetary bodies such as Mercury and Ganymede, as well as for one-material spheres made of pure water(-ice), silicates, or iron. However, they do not allow a thorough investigation of composition influences and thermal state on a planet’s interior structure and properties. Aims. In this work, we investigate the structure of a rocky planet shortly after formation and at later stages of thermal evolution assuming the planet is differentiated into a metal core and a rocky mantle (consisting of Earth-like minerals, but with a variable iron content). Methods. We derived possible initial temperature profiles after the accretion and magma ocean solidification. We then developed parameterisations for the thermodynamic properties inside the core depending on planet mass, composition, and thermal state. Results. We provide the community with robust scaling laws for the interior structure, temperature profiles, and core- and mantle-averaged thermodynamic properties for planets composed of Earth’s main minerals but with variable compositions of iron and silicates. Conclusions. The scaling laws make it possible to investigate variations in thermodynamic properties for different interior thermal states in a multitude of applications such as deriving mass-radius scaling laws or estimating magnetic field evolution and core crystallisation for rocky exoplanets.

Effects of the Subsequent Ion Irradiation on the Formation Process of β-SiC from Si-C Mixtures Fabricated on Si by Ion Implantation

1987 ◽  
Vol 97 ◽  
Author(s):  
Tadamasa Kimura ◽  
Hiroyuki Yamaguchi ◽  
Shigemi Yugo ◽  
Yoshio Adachi
Keyword(s):  
Activation Energy ◽  
Ion Implantation ◽  
Infrared Absorption ◽  
Formation Process ◽  
Room Temperature ◽  
Ion Irradiation ◽  
Infrared Absorption Spectroscopy ◽  
Energetic Ions ◽  
Mixed Layers ◽  
Post Implantation

ABSTRACTThe β-SiC formation process through post-implantation annealing of Si-C mixtures fabricated on Si by C-ion implantation at room temperature is studied by means of infrared absorption spectroscopy. It is shown that the formation of B-SiC from the Si-C mixtures is greatly enhanced by the subsequent irradiation of other energetic ions prior to the thermal annealing. The continuous amorphization of the Si-C mixed layers is considered to be the dominant cause for the enhancement of the B-SiC formation. The activation energy of the β-SiC formation process which is 5.3 eV without irradiation is reduced to 4.0 eV by the irradiation of 150 keV, 1 × 1017/cm2 Ar ions.

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
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