English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We show that the nonlinear evolution of the cosmic gravitational clusteringis approximately spatial local in the $x$-$k$ (position-scale) phase space ifthe initial perturbations are Gaussian. That is, if viewing the mass field withmodes in the phase space, the nonlinear evolution will cause strong couplingamong modes with different scale $k$, but at the same spatial area $x$, whilethe modes at different area $x$ remain uncorrelated, or very weakly correlated.We first study the quasi-local clustering behavior with the halo model, anddemonstrate that the quasi-local evolution in the phase space is essentiallydue to the self-similar and hierarchical features of the cosmic gravitationalclustering. The scaling of mass density profile of halos insures that thecoupling between $(x-k)$ modes at different physical positions is substantiallysuppressed. Using high resolution N-body simulation samples in the LCDM model,we justify the quasi-locality with the correlation function between the DWT(discrete wavelet transform) variables of the cosmic mass field. Although themass field underwent a highly non-linear evolution, and the DWT variablesdisplay significantly non-Gaussian features, there are almost no correlationsamong the DWT variables at different spatial positions. Possible applicationsof the quasi-locality have been discussed.Comment: AAS Latex file, 33 pages, 7 figures included, accepted for  publication in Ap

Quasi‐Local Evolution of the Cosmic Gravitational Clustering in the Halo Model