Let R be a Noetherian ring, F := Rr and M ⊆ F a submodule of rank r. Let A∗(M) denote the stable value of Ass(Fn/Mn), for n large, where Fn is the nth symmetric power of Fn and Mn is the image of the nth symmetric power of M in Fn. We provide a number of characterizations for a prime ideal to belong to A∗(M). We also show that A∗(M) ⊆ A∗(M), where A∗(M) denotes the stable value of Ass(Fn/Mn).

In this paper, random walks with independent steps distributed according to a Q-power-law probability distribution function with Q=1/(1-q) are studied. In the case q>1, we show that (i) a stochastic representation of the location of the walk after n steps can be explicitly given (for both finite and infinite variance) and (ii) a clear connection with the superstatistics framework can be establi...

Algorithms based on spectral graph cut objectives such as normalized cuts, ratio cuts and ratio association have become popular in recent years because they are widely applicable and simple to implement via standard eigenvector computations. Despite strong performance for a number of clustering tasks, spectral graph cut algorithms still suffer from several limitations: first, they require the n...

Key words radiative transfer – stars: emission line, Be – stars: winds, outflows – stars: Wolf-Rayet – circumstellar matter In dense hot star winds, the infrared and radio continua are dominated by free-free opacity and recombination emission line spectra. In the case of a spherically symmetric outflow that is isothermal and expanding at constant radial speed, the radiative transfer for the con...

In dense hot star winds, the infrared and radio continua are dominated by free-free opacity and recombination emission line spectra. In the case of a spherically symmetric outflow that is isothermal and expanding at constant radial speed, the radiative transfer for the continuum emission from a dense wind is analytic. Even the emission profile shape for a recombination line can be derived. Key ...

We consider the kinematic stage of evolution magnetic field advected by turbulent hydrodynamic flow. use a generalization Kazantsev-Kraichnan model to investigate time irreversible flows. In viscous range scales, infinite-time limit spectrum is power law but its slope more flat than that predicted Kazantsev model. This result agrees with numerical simulations. The rate energy growth slower in t...

Shannon[1] and Yavuz[2] estimated the entropy of real documents. This note drives an upper bound of entropy from the power law. Let D be a set of documents and f r(w) be the number of occurrences of a word w in the document. Given an interger k, we denote by F (k) the number of words whose frequency is k, i.e., F (k) = ♯{w ∈ D | f r(w) = k}. The entropy of the document set D is defined by E(D) ...

The struggle for power has been a persistent phenomenon throughout history, involving the rulers, general public, and various other interest groups. As one of these groups, the legal community has been in a unique position to regulate the relationship between the ruler and the public because of its dual responsibilities to provide services to the public and to impose constraints on the rulers. ...

Power-law distributions describe many phenomena related to rock fracture. Data collected to measure the parameters of such distributions only represent samples from some underlying population. Without proper consideration of the scale and size limitations of such data, estimates of the population parameters, particularly the exponent D, are likely to be biased. A Monte Carlo simulation of the s...