Self‐Similar Evolution of Gravitational Clustering. II.N‐Body Simulations of then= −2 Spectrum | Zendy

Bhuvnesh Jain | Zendy; Edmund Bertschinger | Zendy

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Self‐Similar Evolution of Gravitational Clustering. II.N‐Body Simulations of then= −2 Spectrum

Author(s) -

Bhuvnesh Jain,

Edmund Bertschinger

Publication year - 1998

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/306538

Subject(s) - scaling , physics , cluster analysis , gravitation , spectral density , spectrum (functional analysis) , statistical physics , nonlinear system , spectral line , similarity (geometry) , computational physics , mathematical analysis , classical mechanics , geometry , quantum mechanics , mathematics , statistics , artificial intelligence , computer science , image (mathematics)

The power spectrum P(k)\propto k^n with n=-2 is close to the shape of themeasured galaxy spectrum on small scales. Unfortunately this spectrum hasproven rather difficult to simulate. Further, 2-dimensional simulations havesuggested a breakdown of self-similar scaling for spectra with n<-1 due todivergent contributions from the coupling of long wave modes. This paper is thesecond (numerical) part of our investigation into the nonlinear gravitationalclustering of scale-free spectra. Using high-resolution N-body simulations wefind that the n=-2 power spectrum, as well as trajectories of the amplitude andphase of Fourier modes, display self-similar scaling. The evolution of thephase shift does show a different scaling at late times, but this was shownanalytically to arise from the purely kinematical effect of bulk flows. Thusour analytical and N-body results verify that self-similarity in gravitationalclustering holds for -3

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