Motion Of Jupiter Research Articles

LONG-TERM spectral components of global, north and south hemisphere temperatures over the last millennium and solar-lunar forcing

Data of temperature anomalies from different sites worldwide for the last millennium are used to extract long-term components in global, northern and southern hemisphere temperatures for their quantitative contribution to climate change to evaluate and to search for possible causes. The Method of Global Minimum which is capable of making a self-consistent selection of trends from a data set and singling out harmonics with varying phase and amplitude is applied. Quantitative description of all components of the spectra including trends extracted for the first time by self-consistent method is given and discussed. Temperature trends have highest amplitude in north, south hemispheres and globally that leads to their largest contribution to climate change. Trend in north hemisphere temperature described by nonstationary sinusoid at period ∼1270 yr shows maximum near 1300 (medieval warming), deep minimum near 1700 (Maunder's minimum) and rise since 1700 to present. Trend in south hemisphere has smoothed maximum for medieval epoch, minimum near 1800 (Dalton's minimum) and rise since 1800. Both trends go up together since ∼1800, but north hemisphere temperature grows faster. Trend in global temperature described by nonstationary sinusoid at period ∼1000 yr demonstrates deep smoothed minimum near 1750 and subsequent rise with rate of increase ∼0.5 °C/100yr since 1800. Amplitude of the nonstationary cycle began rise since 1250 and continue to rise for present and close future. Temporal changes of amplitude and phase of nonstationary spectral components have typical features of nonlinear oscillations that points to a nonlinear mechanism supporting the periodical oscillations. It is shown that the 33-yr nonstationary component in global temperature has the highest rate of change ∼1.2 °C/100yr or 0.12 °C/10yr, which can explain rapid temperature changes (from warming to subsequent cooling and vice versa). It is also shown that periods of the temperature spectra include integers of periods of historically-known eclipse cycles and of periods related with motions of Jupiter, Saturn and Venus. Therefore Sun and Moon, Jupiter, Saturn and Venus influence on climate variability. The result also means existence of high-number commensurabilities between mean motions in the system Sun –Earth–Moon and these planets.

Masses of the Trojan Groups of Jupiter

The possibility of obtaining dynamical estimates of the total masses in the two Trojan asteroid groups of Jupiter is investigated. The compact Greek (L4) and Trojan (L5) groups contain several tens of thousands of asteroids near the stable Lagrange points moving in a 1: 1 resonance with the orbital motion of Jupiter. The dynamical mass estimates $$\begin{array}{*{20}{c}} {{M_{L4}} = (8.63 \pm 0.51) \times {{10}^{ - 6}}{M_ \oplus },} \\ {{M_{L5}} = (5.46 \pm 0.54) \times {{10}^{ - 6}}{M_ \oplus }} \end{array}$$ have been obtained by processing more than 800 thousand observations of planets and spacecraft using the new EPM2019 version of planetary ephemerides created at IAA RAS.

On Jupiter and his Galilean satellites: Librations of De Sitter’s periodic motions

The motion of Jupiter’s four Galilean satellites Io–Europa–Ganymedes–Callisto is subjected to an orbital 1:2:4–resonance of the former (and inner) three. Willem de Sitter in the early 20th century gave a mathematical explanation of this in a Newtonian framework. He found a family of stable periodic solutions by using the work of Poincaré. This paper briefly reviews De Sitter’s theory, and focuses on the underlying geometry of a suitable covering space, where we develop Kolmogorov–Arnold–Moser theory to find Lagrangean invariant tori excited by the normal modes of the De Sitter periodic orbits. In this way we find many librations near these periodic orbits that may well offer a more realistic explanation of the observations.

On Saturn’s rotation relative to a center of mass under the action of the gravitational moments of the Sun and Jupiter

Saturn’s rotation relative to a center of mass is considered within an elliptic restricted three-body problem. It is assumed that Saturn is a solid under the action of gravity of the Sun and Jupiter. The motions of Saturn and Jupiter are considered elliptic with small eccentricities eS and eJ, respectively; the mean motion of Jupiter nJ is also small. We obtain the averaged Hamiltonian function for a small parameter of e = nJ and integrals of evolution equations. The main effects of the influence of Jupiter on Saturn’s rotation are described: (α) the evolution of the constant parameters of regular precession for the angular momentum vector I2; (β) the occurrence of new libration zones of oscillations I2 near the plane of the celestial equator parallel to the plane of the Jupiter’s orbit; (γ) the occurrence of additional unstable equilibria of vector I2 at the points of the north and south poles of the celestial sphere and, as a result, the existence of homoclinic trajectories; and (δ) the existence of periodic trajectories with arbitrarily large periods near the homoclinic trajectory. It is shown that the effects of (β), (γ), and (δ) are caused by the eccentricity e of the Jupiter’s orbit and are practically independent of Jupiter’s mass (within satellite approximation).

3D Modeling of interactions between Jupiter’s ammonia clouds and large anticyclones

The motions of Jupiter’s tropospheric jets and vortices are made visible by its outermost clouds, which are expected to be largely composed of ammonia ice. Several groups have demonstrated that much of this dynamics can be reproduced in the vorticity fields of high-resolution models that, surprisingly, do not contain any clouds. While this reductionist approach is valuable, it has natural limitations. Here we report on numerical simulations that use the EPIC Jupiter model with a realistic ammonia-cloud microphysics module, focusing on how observable ammonia clouds interact with the Great Red Spot (GRS) and Oval BA. Maps of column-integrated ammonia-cloud density in the model resemble visible-band images of Jupiter and potential-vorticity maps. On the other hand, vertical cross sections through the model vortices reveal considerable heterogeneity in cloud density values between pressure levels in the vicinity of large anticyclones, and interestingly, ammonia snow appears occasionally. Away from the vortices, the ammonia clouds form at the levels expected from traditional one-dimensional models, and inside the vortices, the clouds are elevated and thick, in agreement with Galileo NIMS observations. However, rather than gathering slowly into place as a result of Jupiter’s weak secondary circulation, the ammonia clouds instead form high and thick inside the large anticyclones as soon as the cloud microphysics module is enabled. This suggests that any weak secondary circulation that might be present in Jupiter’s anticyclones, such as may arise because of radiative damping of their temperature anomalies, may have little or no direct effect on the altitude or thickness of the ammonia clouds. Instead, clouds form at those locations because the top halves of large anticyclones must be cool for the vortex to be able to fit under the tropopause, which is a primary-circulation, thermal-wind-shear effect of the stratification, not a secondary-circulation thermal feature. A planetary-scale void of ammonia clouds persists in the model southward of -38° planetographic latitude, but may partially reflect the fact that we have not yet included a full complement of vortices, all condensable species or the underlying dry-convective forcing from Jupiter’s interior.

Location, structure, and motion of Jupiter's dusk magnetospheric boundary from ∼1625 to 2550 RJ

We report on plasma observations along Jupiter's dusk magnetospheric flank from ∼1625 to 2550 RJ using measurements from the Solar Wind Around Pluto instrument onboard New Horizons (NH). NH observed 16 magnetopause crossings between 1654 and 2429 RJ that were identified by transitions between magnetotail/boundary layer and magnetosheath plasma. These transitions were either sharp, with the magnetopause clearly separating two distinct plasma regimes, or comparatively gradual, where it was difficult to distinguish between different plasma populations. The magnetosheath distributions had high counts, were relatively wide in energy/charge (E/Q), and steadily decreased in speed. Flow speeds in the sheath were always higher (lower) when NH entered (exited) this region. A boundary layer was observed inside of the magnetopause at several crossings. The boundary layer plasma was composed of light ions, and the counts and mean E/Q of these distributions were generally lower than magnetosheath values indicating a lower density and speed. Some of the NH magnetopause crossing locations fell within tail cross‐section estimates from model results/observations closer to the planet, though more than half were outside of the largest tail radius estimate. Estimates of angular displacement of the tail boundary compared favorably with a statistical study of near‐Jupiter solar wind flow cone angle distributions. We propose that the outward crossings resulted from dawnward deflection and contraction of the tail from forward shocks and compression regions in the near‐Jupiter solar wind, and the inward crossings resulted from duskward deflection and tail expansion from the passage of reverse shocks and rarefaction regions.

Numerical theory of the motion of Jupiter’s Galilean satellites

A numerical theory of the motion of Jupiter’s Galilean satellites was constructed using 3767 absolute observations of the satellites. The theory was based on the numerical integration of the equations of motion of the satellites. The integration was carried out by Everhart’s method using the ERA software package developed at the Institute of Applied Astronomy (IAA). Perturbations due to the oblateness of the central planet, perturbations from Saturn and the Sun, and the mutual attraction of the satellites were taken into account in the integration. As a result, the coefficients of the Chebyshev series expansion for coordinates and velocities were found for the period from 1962 to 2010. The initial coordinates and velocities of the satellites, as well as their masses, the mass of Jupiter, and the harmonic coefficient J2 of the potential of Jupiter, were adjusted. The resulting ephemerides were compared to those of Lieske and Lainey.

The Influence of Giant Planets Near a Mean Motion Resonance on Earth‐like Planets in the Habitable Zone of Sun‐like Stars

We present a numerical study of several two-planet systems based on the motions of Jupiter and Saturn, in which the two giant planets move in low eccentric orbits close to a mean motion resonance. It is more likely to find two planets with similar characteristics in a system than a clone of the Jupiter-Saturn pair of our solar system. Therefore, we vary the distance between the two planets and their mass ratio by changing Saturn's semimajor axis from 8 to 11 AU and increasing its mass by factors of 2-40. The different two-planets were analyzed for the interacting perturbations due to the mean motion resonances of the giant planets. We select several mass ratios for the gas giants, for which we study their influence on test bodies (with negligible mass) moving in the habitable zone (HZ) of a Sun-like star. The orbits are calculated for 2 × 107 yr. In all cases the HZ is dominated by a significant curved band, indicating higher eccentricity, which corresponds to a secular resonance with Jupiter. Interesting results of this study are finding (1) an increase of Venus's eccentricity for the real Jupiter and Saturn masses and the actual semimajor axis of Saturn; (2) an increase of the eccentricity of a test planet at Earth's position when Saturn's mass was increased by a factor of 3 or more; and (3) if the two giant planets are in 2:1 resonance, we observe a strong influence on the outer region of the HZ.

Dynamics of Jovian atmospheres with applications of nonlinear singular vector method

AbstractNonlinear singular vectors (NSVs) of a Jovian atmosphere model are obtained numerically in this paper. NSVs are the initial perturbation, whose nonlinear evolution attains the maximal value of the cost function, which is constructed according to the physical problem of interest. The results demonstrate that the motions of Jupiter's atmosphere is relatively stable under some assumptions. Copyright © 2007 John Wiley & Sons, Ltd.

Applications of conditional nonlinear optimal perturbation to the study of the stability and sensitivity of the Jovian atmosphere

A two-layer quasi-geostrophic model is used to study the stability and sensitivity of motions on small-scale vortices in Jupiter’s atmosphere. Conditional nonlinear optimal perturbations (CNOPs) and linear singular vectors (LSVs) are both obtained numerically and compared in this paper. The results show that CNOPs can capture the nonlinear characteristics of motions in small-scale vortices in Jupiter’s atmosphere and show great difference from LSVs under the condition that the initial constraint condition is large or the optimization time is not very short or both. Besides, in some basic states, local CNOPs are found. The pattern of LSV is more similar to local CNOP than global CNOP in some cases. The elementary application of the method of CNOP to the Jovian atmosphere helps us to explore the stability of various-scale motions of Jupiter’s atmosphere and to compare the stability of motions in Jupiter’s atmosphere and Earth’s atmosphere further.

A New System of Initial Parameters for Numerical Simulation of the Motion of Jupiter's Galilean Satellites

A differential correction using Lieske's analytical theory was applied for a 100-year time interval, and a new system of initial parameters was obtained for numerical simulation of the motion of Jupiter's Galilean satellites.

Orbital and solar resonance in the Jovian Moon system

The periodic orbit representing the motion of the inner three Galilean satellites of Jupiter is constructed in a rotating frame. Stability analysis indicates linear instability; but the repeated Poincare exponents are associated with time and rotational symmetries, and it is concluded that the system is orbitally stable. Analysis of system frequencies reveals two resonances with the Sun. The rotation rate of the reference frame is close to 89∶10 the mean motion of Jupiter, and the period of the reference orbit is nearly 17∶10446 the period of Jupiter. The 89∶10 resonance is investigated via the method of averaging. The Jovian system currently circulates just outside the capture boundary with a period of about 117000 year, but with rotation rate of the reference frame varying by over an order of magnitude. Including tidal interaction, the system is evolving towards temporary capture in this resonance.

The structure, composition and motions of Jupiter's atmosphere

Beyond the asteroid belt lies Jupiter, the largest planet in the solar system, surrounded by an extensive system of satellites. It differs greatly from the terrestrial planets. Jupiter is a huge, rapidly rotating body with an apparently permanently banded appearance of changing colours. Its atmosphere is mainly composed of hydrogen and helium in amounts similar to those found in the sun. The composition and structure of the clouds which obscure the lower levels of atmosphere are presently not known. Present theories are unable to account completely for the banded structure, colours, and the Great Red Spot in Jupiter's atmosphere.

On the Theory of the Galilean Satellites of Jupiter

In this communication the main equations for the variables: radius vector, longitude, P and Q (variables built from Laplace's perihelium first integral) are given in closed form. These equations are used for deriving the equations of a second-order theory. At this order, the equations for P and Q, are separated and they are integrodifferential linear equations. The equations for the radius vector and for the longitudes, give, after integration, perturbations which are purely trigonometric. The solution shows the features observed in the motion of Jupiter's Galilean satellites. The results are discussed, and extended to include the space variables.

The effects of resonance with Jupiter in the system of short-period comets

AbstractStructural effects of the resonance with the mean motion of Jupiter on the system of short-period comets are discussed. The distribution of mean motions, determined from sets of consecutive perihelion passages of all known periodic comets, reveals a number of gaps associated with low-order resonance; most pronounced are those corresponding to the simplest commensurabilities of 5/2, 2/1, 5/3, 3/2, 1/1 and 1/2. The formation of the gaps is explained by a compound effect of five possible types of behaviour of the comets set into an approximate resonance, ranging from quick passages through the gap to temporary librations avoiding closer approaches to Jupiter. In addition to the comets of almost asteroidal appearance, librating with small amplitudes around the lower resonance ratios (Marsden, 1970b), there is an interesting group of faint diffuse comets librating in characteristic periods of about 200 years, with large amplitudes of about±8% in μ and almost±180° in σ, around the 2/1 resonance gap. This transient type of motion appears to be nearly as frequent as a circulating motion with period of revolution of less than one half that of Jupiter. The temporary members of this group are characteristic not only by their appearance but also by rather peculiar discovery conditions.

On the structure and motions of Jupiter's red spot

Abstract A new hypothesis-called the Cartesian diver hypothesis-is proposed to explain the physical nature and observed variations in longitude, size and intensity of Jupiter's Great Red Spot. In the light of recent laboratory studies of phase behavior in light gas mixtures, it is suggested that the Red Spot is a region of contrast in the cloud structure of Jupiter's outer layers, caused by the presence of a mass of hydrogen-rich solid floating within a fluid layer of hydrogen and helium at some depth below the visible surface. It is shown that this floating solid would exhibit many of the characteristics of a Cartesian diver. Equations of motion for a Cartesian diver in a rotating system are derived, which suggest that the longitudinal motion of the Red Spot consists of several oscillatory components of different amplitudes and frequencies. These predictions are in agreement with motions determined from recent precise measurements of Red Spot longitude. Mechanisms for the source of the observed oscillations are discussed, and estimates are made of the extent of the underlying vertical motions. Effects of the rapid rotation of the planet upon the dynamic behavior of the fluid in the vicinity of the Cartesian diver are qualitatively included, and the resulting physical model is used to explain not only the observed variations of size and intensity of the Red Spot, but also the manner in which these variations correlate with changes in longitude. Laboratory studies and further observations designed to assist in verifying the Cartesian diver hypothesis are suggested.

The motion of Jupiter's fifth satellite

A method is described for obtaining and reducing a series of photographic observations of the fifth satellite and the disk of Jupiter against a background of stars. A discussion of these and earlier observations leads to revised values for the mean motion and the regression of the nodes.

Sudden Changes in the Motion of Jupiter's Great Red Spot During 1962

Fifty-seven visual determinations of the System II longitude of Jupiter's Great Red Spot, made during the last four months of 1962, have been plotted and analysed. The totally independent testimony of a number of observers provides what appears to be overwhelming evidence that during about three weeks, centred near October 20, the longitude of the Red Spot, which previously and subsequently was sensibly stationary in System II, increased by approximately 4°. On the evidence available it seems impossible to extend the duration of the transition beyond a maximum of five weeks. These conclusions augment rather than conflict with those recently published by B. A. Smith and C. W. Tombaugh, which were derived from the measurement of a number of photographs of Jupiter, obtained by them during the same period.

Motion of Jupiter and mass of Saturn

view Abstract Citations (5) References (3) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Motion of Jupiter and mass of Saturn Clemence, G. M. Abstract The discrepancy between theory and observation in the longitude of Jupiter found by Krotkov and Dicke, which has coefficient of 0,'25 and a period of 4520 days, is removed by attributing mass 1/3499.7 to Saturn and adding two known corrections to the motion of the perihelion. Publication: The Astronomical Journal Pub Date: February 1960 DOI: 10.1086/108172 Bibcode: 1960AJ.....65...21C full text sources ADS |

The motion of Jupiter's Eighth Satellite from 1910 to 1916: (Plate 3.)

The motion of Jupiter's Eighth Satellite from 1910 to 1916: (Plate 3.)