Modified Newtonian Dynamics of Large Scale Structure

Adi Nusser

doi:10.1046/j.1365-8711.2002.05235.x

paper

Modified Newtonian Dynamics of Large Scale Structure

arXiv:astro-ph/0109016 · doi:10.1046/j.1365-8711.2002.05235.x

Abstract

We examine the implications of Modified Newtonian Dynamics (MOND) on the large scale structure in a Friedmann-Robertson-Walker universe. We employ a ``Jeans swindle'' to write a MOND-type relationship between the fluctuations in the density and the gravitational force, $\vg$. In linear Newtonian theory, $|\vg|$ decreases with time and eventually becomes $< g_{0}$ , the threshold below which MOND is dominant. If the Newtonian initial density field has a power-law power-spectrum of index $n < - 1$ , then MOND domination proceeds from small to large scale. At early times MOND tends to drive the density power-spectrum towards $k^{- 1}$ , independent of its shape in the Newtonian regime. We use N-body simulations to solve the MOND equations of motion starting from initial conditions with a CDM power-spectrum. MOND with the standard value $g_{0} = 1 0^{- 8} c m s^{- 2}$ , yields a high clustering amplitude that can match the observed galaxy distribution only with strong (anti-) biasing. A value of $g_{0} \approx 1 0^{- 9} c m s^{- 2}$ , however, gives results similar to Newtonian dynamics and can be consistent with the observed large scale structure.

Version accepted for publication in the MNRAS. Results of more simulations are included

Modified Newtonian Dynamics of Large Scale Structure

Abstract

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