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Dynamics of a gravitationally loaded chain of elastic beads.

Elastic beads repel in a highly nonlinear fashion, as described by Hertz law, when they are compressed against one another. Vertical stacking results in significant compressions of beads at finite distances from the surface of the stack due to gravity. Analytic studies that have been reported in the literature assume acoustic excitations upon weak perturbation [J. Hong et al., Phys. Rev. Lett. 82, 3058 (1999)] and soliton-like excitations upon strong perturbation [V. Nesterenko, J. Appl. Mech. Tech. Phys. 5, 733 (1983); S. Sen and M. Manciu, Physica A 268, 644 (1999)]. The present study probes the position, velocity and acceleration and selected two-point temporal correlations and their power spectra for individual beads for cases in which the system has been (i) weakly, (ii) strongly, and (iii) moderately perturbed at the surface in the sense specified in the text. Our studies reveal the existence of distinctly different dynamical behavior of the tagged beads, in contrast to conventional acoustic response, as the strength of the perturbation is varied at fixed gravitational loading. We also comment on the effects of polydispersity on system dynamics and probe the relaxation of isolated light and heavy beads in the chain. (c) 2000 American Institute of Physics.

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Chaos in the one-dimensional gravitational three-body problem.

We have investigated the appearance of chaos in the one-dimensional Newtonian gravitational three-body system (three masses on a line with -1/r pairwise potential). In the center of mass coordinates this system has two degrees of freedom and can be conveniently studied using Poincare sections. We have concentrated in particular on how the behavior changes when the relative masses of the three bodies change. We consider only the physically more interesting case of negative total energy. For two mass choices we have calculated 18 000 full orbits (with initial states on a 100x180 lattice on the Poincare section) and obtained dwell time distributions. For 105 mass choices we have calculated Poincare maps for 10x18 starting points. Our results show that the Poincare section (and hence the phase space) divides into three well defined regions with orbits of different characteristics: (1) There is a region of fast scattering, with a minimum of pairwise collisions. This region consists of 'scallops' bordering the E=0 line, within a scallop the orbits vary smoothly. The number of the scallops increases as the mass of the central particle decreases. (2) In the chaotic scattering region the interaction times are longer, and both the interaction time and the final state depend sensitively on the starting point on the Poincare section. For both (1) and (2) the initial and final states consist of a binary + single particle. (3) The third region consists of quasiperiodic orbits where the three masses are bound together forever. At the center of the quasiperiodic region there is a periodic orbit discovered (numerically) by Schubart in 1956. The stability of the Schubart orbit turns out to correlate strongly with the global behavior.

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Gravitational interaction of hadrons: Band-spinor representations of GL(n,R).

We demonstrate the existence of double-valued linear (infinite) spinorial representations of the group of general coordinate transformations. We discuss the topology of the group of general coordinate transformations and its subgroups GA(nR), GL(n,R), SL(nr) for n = 2,3,4, and the existence of a double covering. We present the construction of band-spinor representations of GL(n,R) in terms of Harish-Chandra modules.It is suggested that hadrons interact with gravitation as band-spinors of that type. In the metric-affine extension of general relativity, the hadron intrinsic hypermomentum is minimally coupled to the connection, in addition to the coupling of the energy momentum tensor to the vierbeins. The relativistic conservation of intrinsic hypermomentum fits the observed regularities of hadrons: SU(6) ( approximately spin independence), scaling, and complex-J trajectories. The latter correspond to volume-preserving deformations (confinement?) exciting rotational bands.

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Electromagnetism and gravitation.

Generation of electric fields in rapidly rotating insulators is discussed and calculated. An interesting effect is expected in TlCl. A possible appearance of magnetic fields near rapidly rotating gravitating bodies is proposed. The simple suggestion made here would lead to magnetic fields of negligible magnitude.

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Gravitational symmetry breaking in microtubular dissipative structures.

Reduction-diffusion theories can account for both morphogenesis and the sensitivity of biological systems to weak fields. They predict that gravity can cause the symmetry breaking that is necessary for pattern formation. Microtubules play an important role in organizing the cell, and recent studies hae shown that they can form in vitro dissipative structures. We have found that these structures show patterns of microtubular orientation that are gravity dependent and that the gravitational field causes symmetry breaking. This behavior, which cannot be explained by convection, is in accordance with the theory of dissipative structures. These results suggest that microtubular dissipative structures may play an important role both in morphogenesis and in accounting for the sensitivity of biological systems to weak fields. They aso provide another explanation for biological gravitropism.

Animals↗

A Model for Structure Formation Seeded by Gravitationally Produced Matter.

This model assumes the baryons, radiation, three families of massless neutrinos, and cold dark matter were mutually thermalized before the baryon number was fixed, primeval curvature fluctuations were subdominant, and homogeneity was broken by scale-invariant fluctuations in a new dark matter component that behaves like a relativistic ideal fluid. The fluid behavior could follow if this new component were a single scalar field that interacts only with gravity and with itself by a pure quartic potential. The initial energy distribution could follow if this component were gravitationally produced by inflation. The power spectra of the present distributions of mass and radiation in this model are not inconsistent with the measurements but are sufficiently different from the adiabatic cold dark matter model to allow a sharp test in the near future.

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Optical Gravitational Lensing Experiment Cepheids Have Lower Amplitudes in the Small Magellanic Cloud than in the Large Magellanic Cloud.

We selected Cepheids from the Optical Gravitational Lensing Experiment database for the Magellanic Clouds in the period range of 101.1</=P</=101.4 days. There were 33 objects in the LMC and 35 in the SMC. We find that the median amplitude of Cepheids in the LMC is 18% larger than in the SMC, a 4 sigma effect. For a sample of 42 galactic Cepheids in the same period range, the median amplitude is 7% larger than in the LMC, suggesting that the higher the metal content the larger the amplitude. This implies that the period-flux amplitude relation is not universal and cannot be used to measure distances accurately, unless properly calibrated.

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Gravitational Lensing Effect on the Two-Point Correlation of Hot Spots in the Cosmic Microwave Background.

We investigate the weak gravitational lensing effect that is due to the large-scale structure of the universe on two-point correlations of local maxima (hot spots) in the two-dimensional sky map of the cosmic microwave background (CMB) anisotropy. According to the Gaussian random statistics, as most inflationary scenarios predict, the hot spots are discretely distributed, with some characteristic angular separations on the last scattering surface that are due to oscillations of the CMB angular power spectrum. The weak lensing then causes pairs of hot spots, which are separated with the characteristic scale, to be observed with various separations. We found that the lensing fairly smooths out the oscillatory features of the two-point correlation function of hot spots. This indicates that the hot spot correlations can be a new statistical tool for measuring the shape and normalization of the power spectrum of matter fluctuations from the lensing signatures.

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Adaptive Optics Imaging of the CLASS Gravitational Lens System B1359+154 with the Canada-France-Hawaii Telescope.

We present adaptive optics imaging of the CLASS gravitational lens system B1359+154 obtained with the Canada-France-Hawaii Telescope (CFHT) in the infrared K band. The observations show at least three brightness peaks within the ring of lensed images, which we identify as emission from multiple lensing galaxies. The results confirm the suspected compound nature of the lens, as deduced from preliminary mass modeling. The detection of several additional nearby galaxies suggests that B1359+154 is lensed by the compact core of a small galaxy group. We attempted to produce an updated lens model based on the CFHT observations and new 5 GHz radio data obtained with the MERLIN array, but there are too few constraints to construct a realistic model at this time. The uncertainties inherent with modeling compound lenses make B1359+154 a challenging target for Hubble constant determination through the measurement of differential time delays. However, time delays will offer additional constraints to help pin down the mass model. This lens system therefore presents a unique opportunity to directly measure the mass distribution of a galaxy group at intermediate redshift.

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Application of gravitational clustering analysis to liquid gastric emptying.

A gravitational clustering analysis was applied to principal component weighting factors and t1/2 values from 100 liquid gastric emptying studies. Using principal components, groups of patients with clinical features in common were identified, whereas the analysis of the t1/2 values failed to differentiate them.

Duodenal Ulcer↗

Thermodynamics of a two-dimensional unbounded self-gravitating system.

The thermodynamics of a two-dimensional self-gravitating system occupying the whole plane is considered in the mean-field approximation. First, it is proven that, if the number N of particles and the total energy E are imposed as the only external constraints, then the entropy admits the least upper bound S+(N,E)=2E/N+N ln(epi(2)) (in appropriate units). Moreover, there does exist a unique state of maximum entropy, which is characterized by a Maxwellian distribution function with a temperature T=N/2 independent of E. Next, it is shown that, if the total angular momentum J is imposed as a further constraint, the largest possible value of the entropy does not change, and there is no admissible state of maximum entropy, but in the case J=0. Finally, some inequalities satisfied by a class of so-called H functions and related generalized entropies are given.

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Relaxation and lyapunov time scales in a one-dimensional gravitating sheet system

The relation between relaxation, the time scale of Lyapunov instabilities, and the Kolmogorov-Sinai time in a one-dimensional gravitating sheet system is studied. Both the maximum Lyapunov exponent and the Kolmogorov-Sinai entropy decrease as proportional to N(-1/5). The time scales determined by these quantities evidently differ from any type of relaxation time found in the previous investigations. The relaxation time to quasiequilibria (microscopic relaxation) is found to have the same N dependence as the inverse of the minimum positive Lyapunov exponent. The relaxation time to the final thermal equilibrium differs from the inverse of the Lyapunov exponents and the Kolmogorov-Sinai time.

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Parametric excitation of Alfven waves by gravitational radiation

We consider the parametric excitation of Alfven waves by gravitational radiation propagating on a Minkowski background, parallel to an external magnetic field. As a starting point, standard ideal magnetohydrodynamics equations incorporating the curvature of space-time has been derived. The growth rate of the Alfven waves has been calculated, using the normal-mode approach. Various astrophysical applications of our investigations are discussed, and finally we demonstrate that the coupling coefficients of the interacting modes fulfill the Manley-Rowe relations.

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Stability of a viscous fluid in an oscillating gravitational field.

The stability of the interface of a viscous incompressible fluid superimposed on a massless fluid is studied for the case of an oscillating gravitational field. For the viscous case, the dispersion relation is shown to represent an infinite determinant of the Hill type, which is investigated analytically. The method presented allows one to find the whole dispersion curve of the instability and its asymptotics in an explicit form. The stabilizing effect of the externally imposed oscillations leads to the appearance of stability windows on the growth rate spectrum. Illustrations are given for the influence of all the parameters of the problem on this effect.

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Kinetic approach to low-frequency waves in dusty self-gravitating plasmas.

A kinetic model is derived for the propagation of low-frequency waves in a dusty plasma containing very heavy dust particles, when the self-gravitational interaction due to these grains is included in the analysis. Analytical expressions for the dispersion function are used to examine the instability and damping of the modes. The stability regions of low-frequency waves are compared in the kinetic and the analogous hydrodynamic models, showing that there are only slight differences. However, the kinetic analysis modifies the growth rates of the Jeans instability and can considerably alter the conditions for the propagation of stable dust modes.

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Origin of scaling structure and non-Gaussian velocity distribution in a self-gravitating ring model.

Fractal structures and non-Gaussian velocity distributions are characteristic properties commonly observed in virialized self-gravitating systems, such as galaxies and interstellar molecular clouds. We study the origin of these properties using a one-dimensional ring model that we propose in this paper. In this simple model, N particles are moving, on a circular ring fixed in three-dimensional space, with mutual interaction of gravity. This model is suitable for the accurate symplectic integration method by which we argue the phase transition in this system. Especially, in between the extended phase and the collapsed phase, we find an interesting phase (halo phase) that has negative specific heat at the intermediate energy scale. Moreover, in this phase, there appear scaling properties and nonthermal and non-Gaussian velocity distributions. In contrast, these peculiar properties are never observed in other gas and core phases. Particles in each phase have a typical time scale of motions determined by the cutoff length xi, the ring radius R, and the total energy E. Thus all relaxation patterns of the system are determined by these three time scales.

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Chaos and the continuum limit in the gravitational N-body problem: integrable potentials.

This paper summarizes a numerical investigation of the statistical properties of orbits evolved in "frozen," time-independent N-body realizations of smooth, time-independent density distributions corresponding to integrable potentials, allowing for 10(2.5) < or = N < or = 10(5.5). Two principal conclusions were reached: (1) In agreement with recent work by Valluri and Merritt, one finds that, in the limit of a nearly "unsoftened" two-body kernel, i.e., V(r) approximately equals (r(2) + epsilon(2))(-1/2) for epsilon --> 0, the value of the largest Lyapunov exponent chi does not decrease systematically with increasing N, so that, viewed in terms of the sensitivity of individual orbits to small changes in initial conditions, there is no sense in which chaos "turns off" for large N. However, it is clear that, for any finite epsilon, chi will tend to zero for sufficiently large N. (2) Even though chi does not decrease for an unsoftened kernel, there is a clear, quantifiable sense in which, as N increases, chaotic orbits in the frozen-N systems remain "close to" integrable characteristics in the smooth potential for progressively longer times. When viewed in configuration or velocity space, or as probed by collisionless invariants like angular momentum, frozen-N orbits typically diverge from smooth potential characteristics as a power law in time, rather than exponentially, on a time scale approximately equals N(p)t(D), with p approximately 1/2 and t(D) a characteristic dynamical, or crossing, time. For the case of angular momentum, the divergence is well approximated by a t(1/2) dependence, so that, when viewed in terms of collisionless invariants, discreteness effects act as a diffusion process that, presumably, can be modeled by nearly white Gaussian noise in the context of a Langevin or Fokker-Planck description. For position and velocity, the divergence is more rapid, characterized by a nearly linear power-law growth, t(q) with q approximately 1, a result that likely reflects the effects of linear phase mixing. The inference that, pointwise, individual N-body orbits can be reasonably approximated by orbits in a smooth potential only for times < N(1/2)t(D) has potential implications for various resonance phenomena that can act in real self-gravitating systems.

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Effect of angular momentum on equilibrium properties of a self-gravitating system.

The microcanonical properties of a two-dimensional system of N classical particles interacting via a smoothed Newtonian potential, as a function of the total energy E and the total angular momentum L, are discussed. The two first moments of the distribution of the linear momentum of a given particle at a fixed position show that (a) on average the system rotates like a solid body and (b) the velocity dispersion is a function of the distance from the center. In order to estimate suitable observables, a numerical method based on an importance sampling algorithm is presented. The entropy surface S shows a negative specific heat capacity region at fixed L for all L. Observables probing the average mass distribution are used to understand the link between thermostatistical properties and the spatial distribution of particles. In order to define a phase in a nonextensive system, we introduce a more general observable than that proposed by Gross and Votyakov [Eur. Phys. J. B 15, 115 (2000)]. This observable is the sign of the largest eigenvalue of the Hessian matrix of the entropy surface. If it is negative then the system is in a pure (single) phase; if it is positive then the system undergoes a first order phase transition. At large E the gravitational system is in a homogeneous gas phase. At low E there are several collapse phases. At L=0 there is a single-cluster phase and for L not equal 0 there are several phases with two clusters. The relative size of the clusters depends on L. All these pure phases are separated by a first order phase transition region. Signals of critical behavior emerge at several points of the parameter space (E,L). We also show that a huge loss of information appears if we treat the system as a function of the intensive parameters. Besides the known nonequivalence at first order phase transitions, the pure phases with two clusters of different sizes are not accessible to the canonical ensemble. Moreover, for a particular choice of intensive parameters introduced in this paper, there exist in the microcanonical ensemble some values of those intensive parameters for which the corresponding canonical ensemble does not exist, i.e., the partition sum diverges.

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