scholarly journals Construction et Precision de Nouvelles Theories Planetaires

1979 ◽  
Vol 81 ◽  
pp. 61-67 ◽  
Author(s):  
P. Bretagnon ◽  
J. Chapront
Keyword(s):  
Solar System ◽  
General Theory ◽  
Numerical Integration ◽  
Classical Type ◽  
Minor Planets ◽  
Secular Variations ◽  
Planetary Theories

At the Bureau of Longitudes the construction of planetary theories have been developed in three directions: A general theory of the motion of the four largest planets in the solar system is in the course of development at the Faculty of Sciences at Lille by L. Duriez (1977) following the methods of V. A. Brumberg and J. Chapront (1973). Theories of the classical type with secular variations of the motions of all of the planets from Mercury to Neptune are being completed at the Bureau of Longitudes. They are constructed by P. Bretagnon and J. L. Simon (1975, 1978). The numerical complement to all of these studies, numerical integration, a representation of the solution by Tchebychev series, are being carried out by P. Rocher as concerns the motions of minor planets, and by J. Piranx for the action of Pluto on Uranus and Neptune in the framework of theories with secular variations.

scholarly journals Construction of a planetary solution with the help of an n-body program and analytical complements

1986 ◽  
Vol 114 ◽  
pp. 69-69
Author(s):  
P. Bretagnon
Keyword(s):  
Numerical Integration ◽  
Relativistic Effects ◽  
Analytical Form ◽  
Minor Planets ◽  
The Sun ◽  
The Moon ◽  
The Earth ◽  
Planetary Theories

Up to now we have been dealing with the construction of entirely analytical planetary theories such as VS0P82 (Bretagnon, 1982) and T0P82 (Simon, 1983). These theories take into account the whole of the newtonian perturbations of nine point masses: the Sun, the Earth-Moon barycenter, the planets Mercury, Venus, Mars, Jupiter, Saturn, Uranus and Neptune. They also take into account perturbations due to some minor planets, to the action of the Moon and the relativistic effects. The perturbations of these last three types are in a very simple way under analytical form but they considerably increase the computations when introduced in the numerical integration programs.

scholarly journals On the relationship between long-period comets and large trans-Neptunian planetary bodies

2016 ◽  
Vol 12 (S325) ◽  
pp. 263-265
Author(s):  
Rustam Guliyev ◽  
Ayyub Guliyev
Keyword(s):  
Solar System ◽  
Numerical Integration ◽  
Dynamical Evolution ◽  
Integration Methods ◽  
Long Period ◽  
Planetary Bodies ◽  
Numerical Integration Methods ◽  
Relationship Of ◽  
The Relationship

AbstractIn the present work we investigate the possible relationship of long-period comets with five large and distant trans-Neptunian bodies (Sedna, Eris, 2007 OR10, 2012 VP113and 2008 ST291) in order to determine the probability of the transfer of a part of these kind of comets to the inner of the Solar System. To identify such relationships, we studied the relative positions of the comet orbits and listed TNOs. Using numerical integration methods, we examined dynamical evolution of the comets and have found one encounter of comet C/1861J1 and Eris.

scholarly journals Calibration of the angular momenta of the minor planets in the solar system

2019 ◽  
Vol 630 ◽  
pp. A68 ◽  
Author(s):  
Jian Li ◽  
Zhihong Jeff Xia ◽  
Liyong Zhou
Keyword(s):  
Angular Momentum ◽  
Solar System ◽  
Total Angular Momentum ◽  
Physical Parameters ◽  
Minor Planets ◽  
The Sun ◽  
Relative Angle ◽  
Angular Momenta ◽  
Dwarf Planets ◽  
Invariable Plane

Aims. We aim to determine the relative angle between the total angular momentum of the minor planets and that of the Sun-planets system, and to improve the orientation of the invariable plane of the solar system. Methods. By utilizing physical parameters available in public domain archives, we assigned reasonable masses to 718 041 minor planets throughout the solar system, including near-Earth objects, main belt asteroids, Jupiter trojans, trans-Neptunian objects, scattered-disk objects, and centaurs. Then we combined the orbital data to calibrate the angular momenta of these small bodies, and evaluated the specific contribution of the massive dwarf planets. The effects of uncertainties on the mass determination and the observational incompleteness were also estimated. Results. We determine the total angular momentum of the known minor planets to be 1.7817 × 1046 g cm2 s−1. The relative angle α between this vector and the total angular momentum of the Sun-planets system is calculated to be about 14.74°. By excluding the dwarf planets Eris, Pluto, and Haumea, which have peculiar angular momentum directions, the angle α drops sharply to 1.76°; a similar result applies to each individual minor planet group (e.g., trans-Neptunian objects). This suggests that, without these three most massive bodies, the plane perpendicular to the total angular momentum of the minor planets would be close to the invariable plane of the solar system. On the other hand, the inclusion of Eris, Haumea, and Makemake can produce a difference of 1254 mas in the inclination of the invariable plane, which is much larger than the difference of 9 mas induced by Ceres, Vesta, and Pallas as found previously. By taking into account the angular momentum contributions from all minor planets, including the unseen ones, the orientation improvement of the invariable plane is larger than 1000 mas in inclination with a 1σ error of ∼50−140 mas.

scholarly journals A Dynamical Survey of Inner Solar System Asteroids

1999 ◽  
Vol 172 ◽  
pp. 371-372
Author(s):  
Marc A. Murison
Keyword(s):  
Solar System ◽  
Numerical Integration ◽  
High Order ◽  
Mean Motion Resonances ◽  
Mean Motion

AbstractResults from a numerical integration survey of all 179 currently-known inner solar system asteroids with a ≤ aMars, q ≥ aMercury are presented. A surprising number of asteroids are currently in, or very near, mean-motion resonances with Mercury, Venus, Earth, or Mars. Some of the resonance associations are of high order. Most of the resonance associations are relatively short-lived, with the asteroids wandering in and out of resonance on timescales of hundreds to several thousand years.

scholarly journals Gaia Data Release 2

2018 ◽  
Vol 616 ◽  
pp. A1 ◽  
Author(s):  
◽  
A. G. A. Brown ◽  
A. Vallenari ◽  
T. Prusti ◽  
J. H. J. de Bruijne ◽  
...  
Keyword(s):  
Solar System ◽  
Reference Frame ◽  
Broad Band ◽  
Radial Velocities ◽  
Minor Planets ◽  
Major Advance ◽  
Photometric System ◽  
Proper Motions ◽  
Apparent Brightness ◽  
Data Release

Context. We present the second Gaia data release, Gaia DR2, consisting of astrometry, photometry, radial velocities, and information on astrophysical parameters and variability, for sources brighter than magnitude 21. In addition epoch astrometry and photometry are provided for a modest sample of minor planets in the solar system. Aims. A summary of the contents of Gaia DR2 is presented, accompanied by a discussion on the differences with respect to Gaia DR1 and an overview of the main limitations which are still present in the survey. Recommendations are made on the responsible use of Gaia DR2 results. Methods. The raw data collected with the Gaia instruments during the first 22 months of the mission have been processed by the Gaia Data Processing and Analysis Consortium (DPAC) and turned into this second data release, which represents a major advance with respect to Gaia DR1 in terms of completeness, performance, and richness of the data products. Results. Gaia DR2 contains celestial positions and the apparent brightness in G for approximately 1.7 billion sources. For 1.3 billion of those sources, parallaxes and proper motions are in addition available. The sample of sources for which variability information is provided is expanded to 0.5 million stars. This data release contains four new elements: broad-band colour information in the form of the apparent brightness in the GBP (330–680 nm) and GRP (630–1050 nm) bands is available for 1.4 billion sources; median radial velocities for some 7 million sources are presented; for between 77 and 161 million sources estimates are provided of the stellar effective temperature, extinction, reddening, and radius and luminosity; and for a pre-selected list of 14 000 minor planets in the solar system epoch astrometry and photometry are presented. Finally, Gaia DR2 also represents a new materialisation of the celestial reference frame in the optical, the Gaia-CRF2, which is the first optical reference frame based solely on extragalactic sources. There are notable changes in the photometric system and the catalogue source list with respect to Gaia DR1, and we stress the need to consider the two data releases as independent. Conclusions. Gaia DR2 represents a major achievement for the Gaia mission, delivering on the long standing promise to provide parallaxes and proper motions for over 1 billion stars, and representing a first step in the availability of complementary radial velocity and source astrophysical information for a sample of stars in the Gaia survey which covers a very substantial fraction of the volume of our galaxy.

scholarly journals Commission 20: Positions and Motions of Minor Planets, Comets and Satellites

2005 ◽  
Vol 1 (T26A) ◽  
pp. 153-160
Author(s):  
Giovanni B. Valsecchi ◽  
Julio A. Fernández ◽  
J.-E. Arlot ◽  
E.L.G. Bowell ◽  
Y. Chernetenko ◽  
...  
Keyword(s):  
Solar System ◽  
Minor Planets ◽  
Orbital Elements ◽  
The Past ◽  
Earth Object ◽  
Solar System Bodies

The past triennium has continued to see a huge influx of astrometric positions of small solar system bodies provided by near-Earth object (NEO) surveys. As a result, the size of the orbital databases of all populations of small solar system bodies continues to increase dramatically, and this in turn allows finer and finer analyses of the types of motion in various regions of the orbital elements space.

scholarly journals I. Inferences and suggestions in cosmical and geological philosophy

1865 ◽  
Vol 14 ◽  
pp. 119-129 ◽  
Keyword(s):  
Solar System ◽  
Minor Planets ◽  
Philosophical Investigation ◽  
The Sun ◽  
Zodiacal Light ◽  
Primary Induction

Theory of the Sun—Synthesis of Ponderable Matter in the Sun—Cause of the Solar Spots—Production of the Zodiacal Light—Origin of Meteorites—Original Formation of the Planets—Discrimination of the Views in Cosmical Philosophy advanced from those of Mayer and his School—Theory of the Minor Planets—Projectile Power of the Sun. This paper commences with the “ Theory of the Sun ,” embracing the subjects of the source of its energies, and the synthesis of ponderable matter. The position, powers, and functions of the Sun, as the physical centre of the solar system, are peculiar, and in fact unique. The “Primary Induction” from them, indicating, in the author’s opinion, “the principle of philosophical investigation.” which should be applied to the Sun, is conceived to be “That they imply a corresponding uniqueness and peculiarity in its constitution, characterizing also the nature as well as the disposition of the substances of which it essentially consists. But the particular density of the Sun indicates that it actually consists both of ponderable and imponderable matter.

scholarly journals The Hill stability of triple minor planets in the Solar system

2012 ◽  
Vol 427 (2) ◽  
pp. 1034-1042 ◽  
Author(s):  
Xiaodong Liu ◽  
Hexi Baoyin ◽  
Nikolaos Georgakarakos ◽  
John Richard Donnison ◽  
Xingrui Ma
Keyword(s):  
Solar System ◽  
Minor Planets ◽  
Hill Stability ◽  
The Hill

scholarly journals Spectroscopic Observations of Solar System Objects: Pushing the Limits

1995 ◽  
Vol 167 ◽  
pp. 251-261
Author(s):  
Anita L. Cochran
Keyword(s):  
Solar System ◽  
Minor Planets ◽  
Spectroscopic Observations ◽  
Planetary Satellites ◽  
Solar System Objects ◽  
Spatially Extended

Targets within the solar system generally fall into one of two types: a) major planets (except Pluto) and our Moon; b) minor planets, comets, Pluto and planetary satellites. The first group is noteworthy for being reasonably bright. Most are also spatially extended. The inner planets never achieve large solar elongation. The second group comprises bodies which are generally faint. Comets are spatially extended. The minor planets and comets may be in orbits which are highly inclined or viewed at small solar elongations. Comets may even be in retrograde orbits. Planetary satellites may be bright or faint but suffer from being in the glare of the parent planet.

scholarly journals Commission 15: Physical Study of Comets, Minor Planets, and Meteorites

1985 ◽  
Vol 19 (1) ◽  
pp. 167-187
Author(s):  
C. R. Chapman ◽  
L. Kresak ◽  
B. D. Donn ◽  
F. Dossin ◽  
H. Fechtig ◽  
...  
Keyword(s):  
Soviet Union ◽  
Solar System ◽  
Hubble Space Telescope ◽  
The United States ◽  
Minor Planets ◽  
Small Bodies ◽  
New Era ◽  
Asteroid Exploration ◽  
The Soviet Union ◽  
Physical Study

The last three years have witnessed a growing interest in the physical properties of the small bodies in the solar system. Perhaps the most significant impetus to research on small bodies has been the imminent arrival of Comet Halley in the inner solar system. This famous comet, which was recovered in autumn 1982, has been the object of intense study during the past year as it has approached the sun and developed a tail. Much of the international, ground-based astronomical research on Halley has been coordinated through the International Halley Watch program. Spacecraft from several nations have been successfully launched (or soon will be, we hope) and are on their way to intercept the comet and make close-up observations and in situ measurements. The commencement of spacecraft study of small bodies marks a new era in comet/asteroid science and, in coordination with ground-based and Earth-orbital observations, will result in unprecedented new knowledge about the origin of the solar system and about solar system processes. Although Halley is receiving the most attention, interest is also high in Comet Giacobini-Zinner, the vicinity of which will be probed by a diverted American spacecraft in September 1985. Upcoming spacecraft studies of comets through 1986 are described at the end of the comet section of this report. Asteroid exploration by spacecraft is also anticipated to begin in the near future. The trajectory of the NASA Gailieo Mission to Jupiter has been changed to permit close-encounter observations of the large main-belt asteroid 29 Amphitrite in December 1986; these observations will be conducted on a “best effort” basis only a few months after launch of Galileo. Interest is also high in Europe, the Soviet Union, and the United States in possible spacecraft missions to additional comets and asteroids during the 1990’s. If these efforts are pursued, there will be a concomitant ground-based effort. The last three years have also witnessed extremely productive efforts to observe small bodies from Earth orbit. For example, the Infrared Astronomical Satellite discovered a comet in 1983, which made the closest approach to the Earth of any comet in centuries. IRAS made important discoveries and measurements of other comets and also assembled an immense database on infrared brightnesses of thousands of numbered and unnumbered asteroids. The planned launch of the Hubble Space Telescope next year highlights the continuing potential for applying extremely powerful instrumental techniques to the study of comets and asteroids from above the Earth’s atmosphere.

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