The Jovian ring

1984 ◽  
Vol 75 ◽  
pp. 203-209
Author(s):  
Joseph A. Burns
Keyword(s):  
Equatorial Plane ◽  
Charged Particles ◽  
Dynamical Evolution ◽  
Main Band ◽  
Small Grains ◽  
Three Components

ABSTRACTLying in Jupiter's equatorial plane is a diaphanous ring having little substructure within its three components (main band, faint disk, and halo). Micron-sized grains account for much of the visible ring, but particles of centimeter sizes and larger must also be present to absorb charged particles. Since dynamical evolution times and survival life times are quite short (≲102-3yr) for small grains, the Jovian ring is being continually replenished; probably most of the visible ring is generated by micrometeoroids colliding into unseen parent bodies that reside in the main band.

Stability of trajectories in Ernst space–time

1986 ◽  
Vol 64 (11) ◽  
pp. 1455-1457 ◽  
Author(s):  
K. D. Krori ◽  
Ranjana Choudhury ◽  
J. C. Sarmah
Keyword(s):  
Equatorial Plane ◽  
Charged Particles ◽  
Space Time ◽  
Neutral Particles

In this paper we show that stable trajectories of charged particles, neutral particles, photons, and tachyons occur in the equatorial plane of the Ernst space–time. We also present typical bound trajectories of these particles in the equatorial plane (θ = π/2) as well as on an r = constant surface.

MOTION OF CHARGED PARTICLES AROUND A FIVE-DIMENSIONAL ROTATING MAGNETIZED BLACK HOLE

2007 ◽  
Vol 16 (08) ◽  
pp. 1369-1379
Author(s):  
R. KAYA
Keyword(s):  
Magnetic Field ◽  
Black Hole ◽  
External Magnetic Field ◽  
Effective Potential ◽  
Equatorial Plane ◽  
Charged Particles ◽  
Circular Motion ◽  
Test Particles ◽  
Jacobi Formalism ◽  
The Stability

We study the effect of an external magnetic field on the stability of circular motion of charged particles in the equatorial plane of a five-dimensional rotating black hole. Using the Hamilton–Jacobi formalism, we derive the effective potential for the radial motion of test particles around a five-dimensional magnetized Myers–Perry black hole. We show that there exist stable circular orbits in equatorial planes in the background of this metric.

Saturn’s E ring

1984 ◽  
Vol 75 ◽  
pp. 103-109 ◽  
Author(s):  
W.A. Baum ◽  
T.J. Kreidl ◽  
L.H. Wasserman
Keyword(s):  
Spatial Distribution ◽  
Equatorial Plane ◽  
Total Mass ◽  
Attenuation Factor ◽  
Charged Particles ◽  
Ccd Observations ◽  
Ring Material ◽  
Physical Thickness

ABSTRACTThe spatial distribution of material in Saturn’s E ring has been derived from ground-based CCD observations obtained at the time of the 1980 edge-on presentation. The ring commences abruptly near 3 RS, peaks at the orbit of Enceladus (3.94 RS), and has tenuous outskirts to more than 8 Rs. On reasonable assumptions, we calculate the attenuation factor to be 5xl0-11km-1in the equatorial plane near Enceladus, and the physical thickness of the ring there to be 7500 km (FWHM). The attenuation factor in the equatorial plane is lower by a factor of 8 at Tethys, 76 at Dione, and roughly 1000 at Rhea, while the physical thickness increases by factors of 1.7, 2.9, and 5.5, respectively. This distribution of ring material appears to call for interactions with charged particles and fields. If the E-ring particles are predominantly icy and small, the total mass of the ring is probably less than 106tons.

Bifurcation Analysis of Charged Particles Moving on a Rough Surface Under Different Damping Effects

2017 ◽  
Vol 27 (05) ◽  
pp. 1750069
Author(s):  
Hao Zhang ◽  
Pengcheng Luo ◽  
Huifang Ding
Keyword(s):  
Rough Surface ◽  
Jacobian Matrix ◽  
Particle System ◽  
Charged Particles ◽  
Period Doubling ◽  
Dynamical Evolution ◽  
Underlying Mechanism ◽  
Damping Force ◽  
Damping Effects ◽  
The Stability

This paper deals with two types of bifurcation behaviors of charged particles moving on rough surface under different damping effects. Based on the derived models, the stability of the particle system is judged by eigenvalue analysis and then the eigenvalue movement of the Jacobian matrix is analyzed to reveal the underlying mechanism of the dynamical evolution. It is shown that in the particle system with constant damping force, the system loses stability via Neimark–Sacker bifurcation, whereas in the system with time-dependent damping force, the stability is lost by way of period-doubling bifurcation. In addition, a powerful tool called manifold is employed to meticulously characterize the phase space so as to clearly describe the process of energy evolution, which leads to the inherent understanding of the complex behaviors and particularly the global dynamical properties in the particle system. Finally, some bifurcation diagrams are obtained to give a more evident explanation of complex behaviors. These results are very useful for the entire transport knowledge of charged particle system.

scholarly journals On the effect of the magneton in the scattering of α -rays

1914 ◽  
Vol 90 (619) ◽  
pp. 356-364 ◽  
Keyword(s):  
Magnetic Fields ◽  
Equatorial Plane ◽  
Nuclear Charge ◽  
Charged Particles ◽  
North Pole ◽  
Simple Problem ◽  
Present Communication ◽  
Made In

The present communication is intended to illustrate a remark made in the discussion on the constitution of the atom at the meeting of the Society on March 19. Its object is no more than to show that the molecular magnetic fields discovered by Weiss are very efficient agents in the scattering of α - and β -particles. For this purpose the simple case of charged particles moving in the equatorial plane of a fixed magnetic doublet is considered without taking account of a central nuclear charge. The solution of this simple problem will be sufficient to enable a rough estimate of the magnitude of the effect to be formed. Suppose the plane of the paper to be the equatorial plane of the doublet situated at O (figs. 1, 2) with its north pole above the paper so that the field is down through the paper and is equal to M/ r 3 .

Radial motion of charged particles along axis of the Kerr–Newman– (anti-)de sitter space-time

2018 ◽  
Vol 6 (2) ◽  
pp. 19
Author(s):  
Kameshwar Nath Mishra ◽  
Varull Mishra
Keyword(s):  
Charged Particle ◽  
Effective Potential ◽  
Equatorial Plane ◽  
Jacobi Equation ◽  
Charged Particles ◽  
De Sitter Space ◽  
Space Time ◽  
Radial Motion ◽  
De Sitter ◽  
Hamilton Jacobi Equation

The motion of uncharged particles in the Kerr–Newman–(anti-)de Sitter space-time has been studied by using the Hamilton –Jacobi equation. We have considered both charged particle Q and non-vanishing cosmological constant Λ , focusing on the equatorial plane and space time of the axis. For the study of radial of radial motion on the axis of space time an effective potential have been developto describe the turning points  

Statistical results on discovered near-Earth asteroids

1999 ◽  
Vol 173 ◽  
pp. 81-86
Author(s):  
S. Berinde
Keyword(s):  
Dynamical Evolution ◽  
Minor Planet ◽  
Orbital Elements ◽  
The Earth ◽  
Near Earth Asteroids ◽  
Statistical Results

AbstractThe first part of this paper gives a recent overview (until July 1st, 1998) of the Near-Earth Asteroids (NEAs) database stored at Minor Planet Center. Some statistical interpretations point out strong observational biases in the population of discovered NEAs, due to the preferential discoveries, depending on the objects’ distances and sizes. It is known that many newly discovered NEAs have no accurately determinated orbits because of the lack of observations. Consequently, it is hard to speak about future encounters and collisions with the Earth in terms of mutual distances between bodies. Because the dynamical evolution of asteroids’ orbits is less sensitive to the improvement of their orbital elements, we introduced a new subclass of NEAs named Earth-encounter asteroids in order to describe more reliably the potentially dangerous bodies as impactors with the Earth. So, we pay attention at those asteroids having an encounter between their orbits and that of the Earth within 100 years, trying to classify these encounters.

From the Oort cloud to Halley-type comets

1999 ◽  
Vol 173 ◽  
pp. 327-338 ◽  
Author(s):  
J.A. Fernández ◽  
T. Gallardo
Keyword(s):  
Total Population ◽  
Complex Function ◽  
Dynamical Evolution ◽  
Oort Cloud ◽  
Capture Process ◽  
Influx Rate ◽  
Short Period ◽  
Dynamical Properties ◽  
Orbital Periods ◽  
Probability Of Capture

AbstractThe Oort cloud probably is the source of Halley-type (HT) comets and perhaps of some Jupiter-family (JF) comets. The process of capture of Oort cloud comets into HT comets by planetary perturbations and its efficiency are very important problems in comet ary dynamics. A small fraction of comets coming from the Oort cloud − of about 10−2− are found to become HT comets (orbital periods < 200 yr). The steady-state population of HT comets is a complex function of the influx rate of new comets, the probability of capture and their physical lifetimes. From the discovery rate of active HT comets, their total population can be estimated to be of a few hundreds for perihelion distancesq <2 AU. Randomly-oriented LP comets captured into short-period orbits (orbital periods < 20 yr) show dynamical properties that do not match the observed properties of JF comets, in particular the distribution of their orbital inclinations, so Oort cloud comets can be ruled out as a suitable source for most JF comets. The scope of this presentation is to review the capture process of new comets into HT and short-period orbits, including the possibility that some of them may become sungrazers during their dynamical evolution.

Exploring Coronal Structures with SOHO

2000 ◽  
Vol 179 ◽  
pp. 403-406
Author(s):  
M. Karovska ◽  
B. Wood ◽  
J. Chen ◽  
J. Cook ◽  
R. Howard
Keyword(s):  
Solar Corona ◽  
Image Enhancement ◽  
Coronal Mass Ejections ◽  
Dynamical Evolution ◽  
Small Scale ◽  
Low Contrast ◽  
Contrast Structures ◽  
Scale Structures ◽  
Small Scale Structures ◽  
Coronal Structures

AbstractWe applied advanced image enhancement techniques to explore in detail the characteristics of the small-scale structures and/or the low contrast structures in several Coronal Mass Ejections (CMEs) observed by SOHO. We highlight here the results from our studies of the morphology and dynamical evolution of CME structures in the solar corona using two instruments on board SOHO: LASCO and EIT.

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