scholarly journals Carlsberg optical astrometry of the outer solar system

1996 ◽  
Vol 172 ◽  
pp. 399-406
Author(s):  
L.V. Morrison ◽  
M.E. Buontempo
Keyword(s):  
Solar System ◽  
Optical Observations ◽  
Outer Solar System ◽  
Outer Planets ◽  
Run Off ◽  
Solar System Objects

The Carlsberg astrometric telescope has made about 17000 observations of outer Solar System objects since it began operation in 1984. The observed positions of the major planets are compared with JPL DE200 and DE403. The agreement with DE403 is good in general, but unresolved discrepancies of the order 0″.1 are found in Jupiter and Saturn. The run-off between the observations and DE200 which was fitted to observations before 1980 emphasize the need to continue optical observations of the outer planets.

scholarly journals Evaluating the Dynamical Stability of Outer Solar System Objects in the Presence of Planet Nine

2017 ◽  
Vol 154 (2) ◽  
pp. 61 ◽  
Author(s):  
Juliette C. Becker ◽  
Fred C. Adams ◽  
Tali Khain ◽  
Stephanie J. Hamilton ◽  
David Gerdes
Keyword(s):  
Solar System ◽  
Dynamical Stability ◽  
Outer Solar System ◽  
Solar System Objects

scholarly journals DYNAMICALLY EXCITED OUTER SOLAR SYSTEM OBJECTS IN THEHUBBLE SPACE TELESCOPEARCHIVE

2011 ◽  
Vol 742 (2) ◽  
pp. 118 ◽  
Author(s):  
Cesar I. Fuentes ◽  
David E. Trilling ◽  
Matthew J. Holman
Keyword(s):  
Solar System ◽  
Outer Solar System ◽  
Solar System Objects

scholarly journals Near-infrared Methanol Bands Probe Energetic Processing of Icy Outer Solar System Objects

2020 ◽  
Vol 894 (1) ◽  
pp. L3 ◽  
Author(s):  
Riccardo Giovanni Urso ◽  
Donia Baklouti ◽  
Zahia Djouadi ◽  
Noemí Pinilla-Alonso ◽  
Rosario Brunetto
Keyword(s):  
Solar System ◽  
Near Infrared ◽  
Outer Solar System ◽  
Solar System Objects

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.

Numerical simulations of the accretion of Uranus and Neptune. II. Effect of low velocity encounters

1999 ◽  
Vol 173 ◽  
pp. 31-36 ◽  
Author(s):  
A. Brunini ◽  
J.A. Fernández
Keyword(s):  
Solar System ◽  
Numerical Simulations ◽  
Numerical Experiments ◽  
Relative Velocity ◽  
Solid Material ◽  
Outer Solar System ◽  
Low Velocity ◽  
Mean Motion Resonances ◽  
Outer Planets ◽  
Accretion Process

AbstractNew numerical simulations of the accretion of the outer solar system were carried out by means of a symplectic integration code developed by the authors. By contrast with our previous numerical experiments, we now pay special attention to the treatment of low relative velocity encounters between planetesimals. Our new results corroborate, in general, a marked radial drift of the accreting outer planets, and that less than 50% of the solid material originally present in the system contributes to the accretion process. The results confirm that mean motion resonances play a major role during the accretion of the outer solar system.

scholarly journals Carlsberg Positions of Planets Compared with JPL DE403

1997 ◽  
Vol 165 ◽  
pp. 541-546
Author(s):  
L.V. Morrison ◽  
M.E. Buontempo
Keyword(s):  
Solar System ◽  
Reference Frame ◽  
Systematic Difference ◽  
Outer Solar System ◽  
Vlbi Observations ◽  
Solar System Objects ◽  
Hipparcos Catalogue ◽  
Preliminary Version ◽  
Celestial Reference Frame

AbstractThe Carlsberg meridian telescope has made nearly 20 000 observations of outer Solar System objects since it began operation in 1984. A preliminary version of the Hipparcos catalogue has been used to refer the positions to the International Celestial Reference Frame (ICRF). The observed positions of the major planets are compared with JPL DE403 which is also referred to the ICRF. The agreement with DE403 is good, except for the declination of Jupiter where there is a systematic difference reaching 015 in 1995. The cause of this discrepancy is being investigated at JPL with recent VLBI observations of Galileo.

The contribution of Centaur-emitted dust to the interplanetary dust distribution

2019 ◽  
Vol 490 (2) ◽  
pp. 2421-2429 ◽  
Author(s):  
A R Poppe
Keyword(s):  
Solar System ◽  
Mass Loss ◽  
Kuiper Belt ◽  
Interplanetary Dust ◽  
Outer Solar System ◽  
Dust Grains ◽  
Kuiper Belt Objects ◽  
Dust Density ◽  
Outer Planets ◽  
Current Mass

ABSTRACT Interplanetary dust grains originate from a variety of source bodies, including comets, asteroids, and Edgeworth–Kuiper belt objects. Centaurs, generally defined as those objects with orbits that cross the outer planets, have occasionally been observed to exhibit cometary-like outgassing at distances beyond Jupiter, implying that they may be an important source of dust grains in the outer Solar system. Here, we use an interplanetary dust grain dynamics model to study the behaviour and equilibrium distribution of Centaur-emitted interplanetary dust grains. We focus on the five Centaurs with the highest current mass-loss rates: 29P/Schwassmann-Wachmann 1, 166P/2001 T4, 174P/Echeclus, C/2001 M10, and P/2004 A1, which together comprise 98 per cent of the current mass loss from all Centaurs. Our simulations show that Centaur-emitted dust grains with radii s < 2 μm have median lifetimes consistent with Poynting–Robertson (P–R) drag lifetimes, while grains with radii s > 2 μm have median lifetimes much shorter than their P–R drag lifetimes, suggesting that dynamical interactions with the outer planets are effective in scattering larger grains, in analogy to the relatively short lifetimes of Centaurs themselves. Equilibrium density distributions of grains emitted from specific Centaurs show a variety of structure including local maxima in the outer Solar system and azimuthal asymmetries, depending on the orbital elements of the parent Centaur. Finally, we compare the total Centaur interplanetary dust density to dust produced from Edgeworth–Kuiper belt objects, Jupiter-family comets, and Oort cloud comets, and conclude that Centaur-emitted dust may be an important component between 5 and 15 au, contributing approximately 25 per cent of the local interplanetary dust density at Saturn.

scholarly journals Long Term Evolution of the Solar System

1992 ◽  
Vol 152 ◽  
pp. 17-24 ◽  
Author(s):  
Jack Wisdom
Keyword(s):  
Solar System ◽  
Test Particle ◽  
Long Term Evolution ◽  
Mapping Method ◽  
Outer Solar System ◽  
Central Mass ◽  
Outer Planets ◽  
Term Evolution ◽  
Particle Stability

The mapping method of Wisdom (1982) has been generalized to encompass all n-body problems with a dominant central mass (Wisdom and Holman, 1991). The new mapping method is presented as well as a number of initial applications. These include billion year integrations of the outer planets, a number of 100 million year integrations of the whole solar system, and a systematic survey of test particle stability in the outer solar system.

Surveying the Trans-Neptunian Solar System with TESS

2020 ◽  
Author(s):  
Malena Rice ◽  
Greg Laughlin
Keyword(s):  
Solar System ◽  
Light Curve ◽  
Parameter Space ◽  
Outer Solar System ◽  
Orbital Geometry ◽  
Solar System Objects ◽  
First Results ◽  
Rule Out

&lt;p&gt;In recent years, the observed orbital geometry of extreme trans-Neptunian objects (TNOs) has provided tantalizing evidence predicting the existence of an as-yet undiscovered &amp;#8220;Planet Nine.&amp;#8221; Combined with orbit stability models, these observations permit a detailed prediction of Planet Nine's properties, with a shrinking parameter space as more of these rare objects are discovered. I will present the first results from a new survey utilizing light curve data from the Transiting Exoplanet Survey Satellite (TESS) to search for TNOs at distances 70-800 au, with a magnitude limit V~22. This survey leverages an innovative new pipeline designed to extract the locations, magnitudes, and 27-day orbital arcs of undiscovered outer solar system objects, including both Planet Nine and the population of extreme trans-Neptunian objects pertinent to the Planet Nine theory, using a blind shift-stacking search along all plausible outer solar system orbits. Together with the extensive sky coverage of the TESS survey, this search will place stringent constraints upon the as-yet undiscovered TNO population, with great potential to either discover Planet Nine or almost entirely rule out its existence.&lt;/p&gt;

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