Dynamical modelling of the Galilean moons for the JUICE mission
TL;DR: In this article, a sensitivity analysis of the influence on the dynamics of the system for a wide array of gravitational, tidal and rotational characteristics of the Jovian system is presented.
About: This article is published in Planetary and Space Science.The article was published on 2016-12-01. It has received 19 citations till now. The article focuses on the topics: Galilean moons & Ephemeris.
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01 Jan 2003
TL;DR: In this article, the authors present a survey of expected libration amplitudes for a subset of solar system bodies, identifying those bodies with amplitudes likely to be detectable, and commenting on spin state, and radial structure implications.
Abstract: Physical librations in longitude are forced periodic variations of a body's rotation rate. If the torque producing the librations can be calculated, then observations of the phase and amplitude of librations can provide information on mass distribution, and effective strength of the body. In the near future prospects for observing physical librations look quite promising. Radio interferometric observations of Venus and Mercury may yield sufficiently accurate rotational observations that librations there may be visible. Range measurements from Earth to networks of landed instrument packages on Mars are likely to yield librational data there as well. We compute expected libration amplitudes from physical and orbital parameters of a set of planets and satellites partially motivated by a desire to identify candidates for future observations. Solar system bodies occupy one of three general rotation states: non-resonant states, resonant states, and the synchronous resonant state. Analytical treatments of forced librations were initially motivated by the Moon. Lunar librations were predicted by Newton, first detected telescopically by Bessel, and definitively resolved through lunar laser ranging which has led to quite thorough analysis of of librations for the synchronous case. The synchronous resonant state is commonly observed among satellites. The only known body to exist in a non-synchronous resonance is Mercury which exists in a 3:2 resonance, completing three rotations for every two revolutions about the sun. The analysis of Goldreich and Peale has lead to improved understanding of the general case of half integer resonance states. The dynamics of forced librations in non-resonant rotators has received less attention. While there are few cases in which non-resonant forced librations have been observed, Earth is an important exception, and current observing techniques may have the capacity to detect them on Venus. A comprehensive observing program spanning a range of solar system bodies can address an array of geophysical issues involving interior mass distribution of planets, satellites, and asteroids. Calculations of expected librations can supply amplitude estimates helpful in identifying the likelihood of detecting librations observationally. We present a survey of expected libration amplitudes for a subset of solar system bodies, identifying those bodies with amplitudes likely to be detectable, and commenting on spin state, and radial structure implications.
50 citations
TL;DR: In this article, the influence of the JUICE-PRIDE observables to the determination of the ephemerides of the Io system and the associated physical parameters is analyzed.
32 citations
Institut Polytechnique des Sciences Avancées1, Sternberg Astronomical Institute2, Institut de mécanique céleste et de calcul des éphémérides3, PSL Research University4, Voronezh State University5, Armagh Observatory6, Eclipse Internet7, American Association of Variable Star Observers8, Sao Paulo State University9, Ural Federal University10, Search for extraterrestrial intelligence11, Royal Astronomical Society12, Russian Academy of Sciences13, Met Office14, Sofradir15, Romanian Academy16, Indian Institute of Astrophysics17, University of Siena18, National Aviation University19
TL;DR: In this paper, the authors focused on processing the complete photometric observations data base to compute new accurate astrometric positions from the light curves of the mutual occultations and eclipses.
Abstract: During the 2014-2015 mutual events season, the Institut de Mecanique Celeste et de Calcul desEphemerides (IMCCE), Paris, France, and the Sternberg Astronomical Institute (SAI), Moscow, Russia, led an international observation campaign to record ground-based photomet-ric observations of Galilean moon mutual occultations and eclipses. We focused on processing the complete photometric observations data base to compute new accurate astrometric positions. We used our method to derive astrometric positions from the light curves of the events.
19 citations
Cites background from "Dynamical modelling of the Galilean..."
...Thus, our work is crucial for current and future spacecraft navigation (Dirkx et al. 2016), and for dynamical purposes, since the ephemerides are improved by adjusting the new astrometric positions to the theories....
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TL;DR: In this paper, the authors present the results of simulations using JUICE data from two different experiments (3GM and PRIDE) and perform a simultaneous estimation of the spacecraft and Galilean satellites' orbits, along with some dynamical parameters of interest.
12 citations
TL;DR: In this article, the resonant and secular motion of the Galilean satellites through a Hamiltonian, depending on the slow angles only, obtained with an analytical expansion of the perturbing functions and an averaging operation.
Abstract: The Galilean satellites’ dynamics has been studied extensively during the last century. In the past it was common to use analytical expansions in order to get simple models to integrate, but with the new generation of computers it became prevalent the numerical integration of very sophisticated and almost complete equations of motion. In this article we aim to describe the resonant and secular motion of the Galilean satellites through a Hamiltonian, depending on the slow angles only, obtained with an analytical expansion of the perturbing functions and an averaging operation. In order to have a model as near as possible to the actual dynamics, we added perturbations and we considered terms that in similar studies of the past were neglected, such as the terms involving the inclinations and the Sun’s perturbation. Moreover, we added the tidal dissipation into the equations, in order to investigate how well the model captures the evolution of the system.
12 citations
References
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Book•
01 Jan 2000TL;DR: This is a modern textbook that guides the reader trough the theory and practice of satellite orbit prediction and determination from basic principles of orbital mechanics, and covers elaborate force models as well as precise methods of satellite tracking.
Abstract: This is a modern textbook that guides the reader trough the theory and practice of satellite orbit prediction and determination. Starting from basic principles of orbital mechanics, it covers elaborate force models as well as precise methods of satellite tracking. Emphasis is on numerical treatment and a multitude of algorithms adopted in modern satellite trajectory computation are described in detail. Numerous exercises and applications are provided and supplemented by a unique collection of computer programs with associated C++ source codes included on the accompanying CD-ROM. These programs are built around a powerful spaceflight dynamics library well suited to the development of inividual applications. An extensive collection of Internet resources is provided through WWW hyperlinks to detailed and frequently updated online information on spaceflight dynamics. The book addresses students and scientists working in the field of navigation, geodesy and spaceflight technology, as well as satellite engineers and operators focusing on spaceflight dynamics.
1,147 citations
TL;DR: The SPICE system is described, current and future SPICE applications are identified, and customer support offered by NAIF is summarized.
917 citations
University of Nantes1, Imperial College London2, Paris Diderot University3, University of Leicester4, European Space Research and Technology Centre5, University College London6, University of Oxford7, Max Planck Society8, Centre national de la recherche scientifique9, Spanish National Research Council10
TL;DR: The JUpiter ICy moons Explorer (JUICE) mission as mentioned in this paper was selected by ESA in May 2012 to perform detailed investigations of Jupiter and its system in all their interrelations and complexity with particular emphasis on Ganymede as a planetary body and potential habitat.
493 citations
United States Geological Survey1, University of Maryland, College Park2, Lowell Observatory3, W.M. Keck Observatory4, Centre national de la recherche scientifique5, Goddard Space Flight Center6, University of Virginia7, University of Western Ontario8, University of Hawaii9, Cornell University10, Queen Mary University of London11
TL;DR: The IAU Working Group on Cartographic Coordinates and Rotational Elements (WGPSN) as mentioned in this paper takes into account the IAU working group for planetary system Nomenclature and the International Astronomical Union (IAUWCN) definition of dwarf planets, and introduces improved values for the pole and rotation rate of Mercury, returns the rotation rates of Jupiter to a previous value, and adds the equatorial radius of the Sun for comparison.
Abstract: Every three years the IAU Working Group on Cartographic Coordinates and Rotational Elements revises tables giving the directions of the poles of rotation and the prime meridians of the planets, satellites, minor planets, and comets. This report takes into account the IAU Working Group for Planetary System Nomenclature (WGPSN) and the IAU Committee on Small Body Nomenclature (CSBN) definition of dwarf planets, introduces improved values for the pole and rotation rate of Mercury, returns the rotation rate of Jupiter to a previous value, introduces improved values for the rotation of five satellites of Saturn, and adds the equatorial radius of the Sun for comparison. It also adds or updates size and shape information for the Earth, Mars’ satellites Deimos and Phobos, the four Galilean satellites of Jupiter, and 22 satellites of Saturn. Pole, rotation, and size information has been added for the asteroids (21) Lutetia, (511) Davida, and (2867) Steins. Pole and rotation information has been added for (2) Pallas and (21) Lutetia. Pole and rotation and mean radius information has been added for (1) Ceres. Pole information has been updated for (4) Vesta. The high precision realization for the pole and rotation rate of the Moon is updated. Alternative orientation models for Mars, Jupiter, and Saturn are noted. The Working Group also reaffirms that once an observable feature at a defined longitude is chosen, a longitude definition origin should not change except under unusual circumstances. It is also noted that alternative coordinate systems may exist for various (e.g. dynamical) purposes, but specific cartographic coordinate system information continues to be recommended for each body. The Working Group elaborates on its purpose, and also announces its plans to occasionally provide limited updates to its recommendations via its website, in order to address community needs for some updates more often than every 3 years. Brief recommendations are also made to the general planetary community regarding the need for controlled products, and improved or consensus rotation models for Mars, Jupiter, and Saturn.
484 citations
TL;DR: In this paper, a theory of orbital evolution is developed in which the disturbing function is expressed in a Fourier series with respect to time, so that the effects of variation of dissipation factor 1/Q, or lag angle ϵ, with amplitude and frequency can be examined.
Abstract: Dissipation of tidal energy in the earth's mantle and the moon was calculated assuming a dissipation factor 1/Q constant throughout both bodies. In the mantle the dissipation varies from about 2 × 10−6/Q erg cm−3 sec−1 near the pole at the bottom of the mantle to about 0.02 × 10−6/Q erg cm−3 sec−1 near the surface. The effects of compressibility and inhomogeneity are less than 3%. In a homogeneous moon the dissipation varies from a maximum of about 0.03 × 10−6/Q erg cm−3 sec−1 near the center to a minimum of about 0.4 × 10−9/Q erg cm−3 sec−1 at the surface. A theory of orbital evolution is developed in which the disturbing function is expressed in a Fourier series with respect to time, so that the effects of variation of dissipation factor 1/Q, or lag angle ϵ, with amplitude and frequency can be examined. Comparisons with results of other authors are made.
454 citations