scholarly journals OSSOS

2019 ◽  
Vol 621 ◽  
pp. A102 ◽  
Author(s):  
Nahuel Cabral ◽  
Aurélie Guilbert-Lepoutre ◽  
Wesley C. Fraser ◽  
Michaël Marsset ◽  
Kathryn Volk ◽  
...  
Keyword(s):  
Solar System ◽  
Giant Planet ◽  
Orbital Evolution ◽  
Outer Solar System ◽  
The Sun ◽  
Point Spread Functions ◽  
Water Ice ◽  
Point Spread ◽  
Size Estimates ◽  
Cometary Activity

Context. Centaurs are icy objects in transition between the trans-Neptunian region and the inner solar system, orbiting the Sun in the giant planet region. Some centaurs display cometary activity, which cannot be sustained by the sublimation of water ice in this part of the solar system, and has been hypothesized to be due to the crystallization of amorphous water ice. Aims. In this work, we investigate centaurs discovered by the Outer Solar System Origins Survey (OSSOS) and search for cometary activity. Tentative detections would improve understanding of the origins of activity among these objects. Methods. We search for comae and structures by fitting and subtracting both point spread functions and trailed point-spread functions from the OSSOS images of each centaur. When available, Col-OSSOS images were used to search also for comae. Results. No cometary activity is detected in the OSSOS sample. We track the recent orbital evolution of each new centaur to confirm that none would actually be predicted to be active, and we provide size estimates for the objects. Conclusions. The addition of 20 OSSOS objects to the population of ~250 known centaurs is consistent with the currently understood scenario, in which drastic drops in perihelion distance induce changes in the thermal balance prone to trigger cometary activity in the giant planet region.

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

scholarly journals Dust Measurements in the Outer Solar System

1994 ◽  
Vol 160 ◽  
pp. 367-380
Author(s):  
Eberhard Grün
Keyword(s):  
Solar System ◽  
Interstellar Dust ◽  
Thermal Emission ◽  
Scattered Light ◽  
Interplanetary Dust ◽  
Dust Particles ◽  
Spatial Density ◽  
Outer Solar System ◽  
The Sun

In-situ measurements of micrometeoroids provide information on the spatial distribution of interplanetary dust and its dynamical properties. Pioneers 10 and 11, Galileo and Ulysses spaceprobes took measurements of interplanetary dust from 0.7 to 18 AU distance from the sun. Distinctly different populations of dust particles exist in the inner and outer solar system. In the inner solar system, out to about 3 AU, zodiacal dust particles are recognized by their scattered light, their thermal emission and by in-situ detection from spaceprobes. These particles orbit the sun on low inclination (i ≤ 30°) and moderate eccentricity (e ≤ 0.6) orbits. Their spatial density falls off with approximately the inverse of the solar distance. Dust particles on high inclination or even retrograde trajectories dominate the dust population outside about 3 AU. The dust detector on board the Ulysses spaceprobe identified interstellar dust sweeping through the outer solar system on hyperbolic trajectories. Within about 2 AU from Jupiter Ulysses discovered periodic streams of dust particles originating from within the jovian system.

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.

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

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.

Conclusion

2013 ◽  
Author(s):  
Andrew P. Ingersoll
Keyword(s):  
Solar System ◽  
Giant Planets ◽  
Outer Solar System ◽  
The Sun ◽  
Extraterrestrial Life ◽  
Better Than

This concluding chapter discusses some of the lessons that can be learned from studying the planets and planetary climates. It first considers the general principles that turned out to be right; for example, size and distance from the Sun matter. The larger objects are able to hold on to their atmospheres better than the small objects. The outer solar system is hydrogen rich and the inner solar system is oxygen rich; as one moves away from the Sun different substances take on different roles. There are also assumptions that proved inaccurate; such was the case for Venus, Mars, and the moons of the giant planets. The chapter also asks whether the study of planetary climates provides lessons for Earth, whether the study of planets has informed us about the likelihood of extraterrestrial life, and whether it has made the development of extraterrestrial life seem more likely.

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.

scholarly journals Low Velocity Encounters of Minor Bodies With the Outer Planets

1983 ◽  
Vol 74 ◽  
pp. 377-395
Author(s):  
A. Carusi ◽  
E. Perozzi ◽  
G.B. Valsecchi
Keyword(s):  
Solar System ◽  
Orbital Evolution ◽  
Outer Solar System ◽  
Low Velocity ◽  
Minor Body ◽  
Outer Planets ◽  
Close Encounters ◽  
Satellite Capture

Previous studies of close encounters of minor bodies with Jupiter have shown that the perturbations are stronger either if the encounter is very deep or if the velocity of the minor body relative to the planet is low. In the present research we investigate the effects of low velocity encounters between fictitious minor bodies and the four outer planets. Two possible outcomes of this type of encounter are the temporary satellite capture of the minor body by the planet, and the exchange of perihelion with aphelion of the minor body orbit. Different occurrence rates of these processes are found for different planets, and the implications for the orbital evolution of minor bodies in the outer Solar System are discussed.

Ultraviolet photolysis of amino acids in a 100 K water ice matrix: Application to the outer Solar System bodies

Icarus ◽  
2007 ◽  
Vol 187 (2) ◽  
pp. 584-591 ◽  
Author(s):  
Grazyna E. Orzechowska ◽  
Jay D. Goguen ◽  
Paul V. Johnson ◽  
Alexandre Tsapin ◽  
Isik Kanik
Keyword(s):  
Amino Acids ◽  
Solar System ◽  
Outer Solar System ◽  
Water Ice ◽  
Matrix Application ◽  
Solar System Bodies ◽  
Ultraviolet Photolysis
Sign in / Sign up

Export Citation Format

Share Document