Abstract

Collisionless media devoid of intrinsic stresses, for example, a dispersed phase in a multiphase medium, have a much wider variety of space-time structures and features formed in them than collisional media, for example, a carrier, gas, or liquid phase. This is a consequence of the fact that evolution in such media occurs in phase space, i.e., in a space of greater dimensions than the usual coordinate space. As a consequence, the process of the formation of features in collisionless media (clustering or vice versa, a loss of continuity) can occur primarily in the velocity space, which, in contrast to the features in the coordinate space (folds, caustics, or voids), is poorly observed directly. To identify such features, it is necessary to use visualization methods that allow us to consider, in detail, the evolution of the medium in the velocity space. This article is devoted to the development of techniques that allow visualizing the degree of anisotropy of the velocity fields of collisionless interpenetrating media. Simultaneously tracking the behavior of different fractions in such media is important, as their behavior can be significantly different. We propose three different techniques for visualizing the anisotropy of velocity fields using the example of two- and three-continuum dispersed media models. We proposed the construction of spatial distributions of eccentricity fields (scalar fields), or fields of principal directions of the velocity dispersion tensor (tensor fields). In the first case, we used some simple eccentricity functions for dispersion tensors for two fractions simultaneously, which we call surrogate entropy. In the second case, to visualize the anisotropy of the velocity fields of three fractions simultaneously, we used an ordered array (3-vector) of eccentricities for the color representation through decomposition in three basic colors. In the case of a multi-stream flow, we used cluster analysis methods to identify sections of a multi-stream flow (beams) and used glyphs to visualize the entire set of beams (vector-tensor fields).

Highlights

  • In astronomy, images are multidimensional data requiring visualization, three-dimensional (3D) [1], five-dimensional (5D) [2] or even six-dimensional (6D) [3], including, in one combination or another, spatial and velocity coordinates in phase space

  • We propose to use both simple and composite glyphs to simultaneously visualize multiple vector and tensor fields that specify the direction of propagation and average velocity of the beams, as well as the anisotropy of their velocity field

  • We considered the procedures for visualizing the flows of collisionless media in the form of impurities of particles immersed in the carrier gas phase

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Summary

Introduction

Images are multidimensional data requiring visualization, three-dimensional (3D) [1], five-dimensional (5D) [2] or even six-dimensional (6D) [3], including, in one combination or another, spatial and velocity coordinates in phase space. We developed visualization tools using the example of a two-dimensional dynamic model of a turbulent interstellar gas-dust matter passing through the spiral arm of a disk galaxy. (x) In a circular region with a radius of 10 computational cells centered at a point with a coordinate (x = −0.3 kpc, z = 0), there is a source of powerful radiation, which is understood as young stars born behind the front of a galactic shock wave in the area of sharp gas compression that promotes rapid star formation Such rows of young stars are clearly observed in the arms of spiral galaxies, as extended bright regions located behind dust lanes stretching along the inner edge of the arms [26,27,28].

Measures of Anisotropy of the Velocity Field
Geometrical Primitives for Visualizing Anisotropic Velocity Distribution
Cluster Analysis for Beam Identification
Conclusions
Patents
Full Text
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