Journal
JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
Volume -, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/1475-7516/2015/02/034
Keywords
modified gravity; cosmological simulations; dark matter simulations
Funding
- STFC [ST/K501979/1, ST/L00075X/1]
- Royal Astronomical Society
- Durham University
- ERC Advanced Investigator grant COSMIWAY [GA 267291]
- Polish National Science Center [DEC-2011/01/D/ST9/01960]
- BIS National E-infrastructure capital grant [ST/K00042X/1]
- STFC capital grant [ST/H008519/1]
- STFC DiRAC Operations grant [ST/K003267/1]
- Science and Technology Facilities Council [ST/K501979/1, ST/H008519/1, ST/I00162X/1, ST/M007006/1, ST/K00042X/1, ST/L00075X/1] Funding Source: researchfish
- STFC [ST/I00162X/1, ST/H008519/1, ST/L00075X/1, ST/K00042X/1, ST/K501979/1, ST/M007006/1] Funding Source: UKRI
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Numerical simulations in modified gravity have commonly been performed under the quasi-static approximation - that is, by neglecting the effect of time derivatives in the equation of motion of the scalar field that governs the fifth force in a given modified gravity theory. To test the validity of this approximation, we analyse the case of f(R) gravity beyond this quasi-static limit, by considering effects, if any, these terms have in the matter and velocity divergence cosmic fields. To this end, we use the adaptive mesh refinement code ECOSMOG to study three variants (vertical bar f(R)vertical bar = 10(-4)[F4]; 10(-5)[F5] and 10(-6)[F6]) of the Hu-Sawicki f(R) gravity model, each of which refers to a different magnitude for the scalar field that generates the fifth force. We find that for F4 and F5, which show stronger deviations from standard gravity, a low-resolution simulation is enough to conclude that time derivatives make a negligible contribution to the matter distribution. The F6 model shows a larger deviation from the quasi-static approximation, but one that diminishes when re-simulated at higher-resolution. We therefore come to the conclusion that the quasi-static approximation is valid for the most practical applications in f(R) cosmologies.
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