Tensor- and spinor-valued random fields with applications to continuum physics and cosmology

TL;DR

This paper reviews the spectral theory of tensor- and spinor-valued random fields, highlighting their applications in continuum physics and cosmology, including the modeling of physical properties and cosmic backgrounds.

Contribution

It provides a comprehensive overview of the mathematical framework and physical applications of isotropic random fields valued in linear spaces and bundles, with new insights into their symmetry properties.

Findings

Spectral theory of tensor-valued random fields in physics and cosmology

Application of symmetry groups to characterize isotropic fields

Modeling cosmic background as isotropic random cross-sections

Abstract

In this paper, we review the history, current state-of-art, and physical applications of the spectral theory of two classes of random functions. One class consists of homogeneous and isotropic random fields defined on a Euclidean space and taking values in a real finite-dimensional linear space. In applications to continuum physics, such a field describes physical properties of a homogeneous and isotropic continuous medium in the situation, when a microstructure is attached to all medium points. The range of the field is the fixed point set of a symmetry class, where two compact Lie groups act by orthogonal representations. The material symmetry group of a homogeneous medium is the same at each point and acts trivially, while the group of physical symmetries may act nontrivially. In an isotropic random medium, the rank 1 (resp. rank 2) correlation tensors of the field transform under the action of the group of physical symmetries according to the above representation (resp. its tensor square), making the field isotropic. Another class consists of isotropic random cross-sections of homogeneous vector bundles over a coset space of a compact Lie group. In applications to cosmology, the coset space models the sky sphere, while the random cross-section models a cosmic background. The Cosmological Principle ensures that the cross-section is isotropic. For convenience of the reader, a necessary material from multilinear algebra, representation theory, and differential geometry is reviewed in Appendix.