A computer program [1] which solves the partial differential equations for sound propagat ion numerically is applied to the study of problems in acoustic emission. The program uses finite difference techniques to calculate sound fields due to distributions of sources in complex

The vast use of computers on scientific numerical computation makes the awareness of the limited precision that these machines are able to provide us an essential matter. A limited and insufficient precision allied to the truncation and rounding errors may induce the user to incorrect

impedance contributions is needed. In the present case, the relevant part of the electromagnetic spectrum lies beneath the cutoff frequency of the component, thus no wave propagation or resonance has to be expected. getting familiar with the existing software modules, trial calculations for simple beam pipe

of a cuplike vesicle is lower than that of the original spherical one. A more precise numerical evaluation of the shape of the open vesicles is also made. In this, we use the line tension and the equivalent spontaneous curvature of the membrane as theoretical parameters. The analysis reproduces

Abstract not found

Abstract. Selfconsistent magnetospheres of rotating cosmic magnets (neutron stars/pulsars) with arbitrary inclination of the magnetic against the rotation axis are considered. Present studies concentrate on the regime dominated by the force–free surface (FFS). A macroscopic fluid description is applied and radiation reaction is taken into account. As in earlier work of our group, a ’standard set of parameters ’ is used. Under these conditions, the following features are found among other results: global charge separation exists for all degrees of inclination of the magnetic against the rotation axis; clouds of different charge are seperated by regions of vanishing particle number density; as expected, test particles inserted into the latter regions propagate into one of the adjacent clouds; strong polodial currents exist; locally averaged particle energies for protons typically range up to 10 16 − 10 17 eV, depending on the angle of inclination.

Abstract. After describing in short some problems and methods regarding the smoothness of null infinity for isolated systems, I present numerical calculations in which both spatial and null infinity can be studied. The reduced conformal field equations based on the conformal Gauss gauge allow us

In this paper the densities D(i) of prime numbers p having the least primitive root g(p) =i, where i is equal to one of the initial positive integers less than 32, have been numerically calculated. The computations were carried out under the assumption of the Generalised Riemann Hypothesis

Data augmentation and Gibbs sampling are two closely related, sampling-based approaches to the calculation of posterior moments. The fact that each produces a sample whose constituents are neither independent nor identically distributed complicates the assessment of convergence and numerical

and numerical calculations