Using an analogy with an Ising-like spin model, we define microcanonical measures for the dynamics of three dimensional (3D) axisymmetric turbulent flow in a Taylor-Couette geometry. We compute the relevant physical quantities and argue that axisymmetry induces a large scale organization in turbulent flows. We show that there exists a low energy, low temperature regime, for which the orthoradia...

A ®nite element model for investigating damage evolution in brittle matrix composites was developed. This modeling is based on an axisymmetric unit cell composed of a ®ber and its surrounding matrix. The unit cell was discretized into linearly elastic elements for the ®ber and the matrix and cohesive elements which allow cracking in the matrix, ®ber-matrix interface, and ®ber. The cohesive elem...

Aims. Some basic structures in planetary nebulae are modeled as self-organized magnetohydrodynamic (MHD) plasma configurations with radial flow. Methods. These configurations are described by time self-similar dynamics, where space and time dependences of each physical variable are in separable form. Axisymmetric toroidal MHD plasma configuration is solved under the gravitational field of a cen...

An axisymmetric model of a cool, dynamo-active accretion disc is applied to protostellar discs. Thermally and magnetically driven outflows develop that are not collimated within 0.1AU. In the presence of a central magnetic field from the protostar, accretion onto the protostar is highly episodic, which is in agreement with earlier work.

The Kramer–Neugebauer–like transformation is constructed for the stationary axisymmetric D=4 Einstein–Maxwell–dilaton–axion system. This transformation directly maps the dualized sigma–model equations of the theory into the nondualized ones. Also the new chiral 4× 4 matrix representation of the problem is presented. PACS numbers: 04.20.Jb, 03.65.Ca Typeset using REVTEX 1

Equilibrium models of differentially rotating nascent neutron stars are constructed, which represent the result of the accretion induced collapse of rapidly rotating white dwarfs. The models are built in a two-step procedure: (1) a rapidly rotating precollapse white dwarf model is constructed; (2) a stationary axisymmetric neutron star having the same total mass and angular momentum distributio...

We model a massless viscous disk using Smoothed Particle Hydro-dynamics (SPH) and note that it evolves according to the Lynden-Bell & Pringle theory (1974) until a non-axisymmetric instability develops at the inner edge of the disk. This instability may have the same origin as the instability of initially axisymmetric viscous disks discussed by Lyubarskij et al. (1994). To clarify the evolution...

Spherical and axisymmetric accretion onto black holes is discussed. Physical processes in various families of solutions are explained and their characteristics are summarized. Recently discovered solutions of axisymmetric flow provide us with various radiation efficiency and spectrum, which may successfully model diverse accretion systems. Possible role of preheating is also speculated. The var...

Stationary, axisymmetric, and slowly rotating vacuum spacetimes in the Hořava-Lifshitz (HL) gravity are studied, and it is shown that, for any given spherical static vacuum solution of the HL theory (of any model, including the ones with an additional U(1) symmetry), there always exists a corresponding slowly rotating, stationary, and axisymmetric vacuum solution, which reduces to the former, w...

The inelastic response of Tennessee marble is modelled by an elastic plastic constitutive relation that includes pressure dependence of yield, strain-softening and inelastic volume strain (dilatancy). Data from 12 axisymmetric compression tests at con"ning pressures from 0 to 100 MPa are used to determine the dependence of the yield function and plastic potential, which are di!erent, on the "rs...