On the Effects of Coupled Scalar Fields on Structure Formation

Abstract

A coupling between a scalar field (representing the dark energy) and dark matter could produce rich phenomena in cosmology. It affects cosmic structure formation mainly through the fifth force, a velocity-dependent force that acts parallel to particle's direction of motion and proportional to its speed, an effective rescaling of the particle masses, and a modified background expansion rate. In many cases these effects entangle and it is difficult to see which is the dominant one. Here we perform N-body simulations to study their qualitative behaviour and relative importance in affecting the key structure formation observables, for a model with exponential scalar field coupling. We find that the fifth force, a prominent example of the scalar-coupling effects, is far less important than the rescaling of particle mass or the modified expansion rate. In particular, the rescaling of particle masses is shown to be the key factor leading to less concentration of particles in halos than in LCDM, a pattern which is also observed in previous independent coupled scalar field simulations.

9 pages, 8 figures

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• Structure Formation in the Symmetron Model
• Testing models of vacuum energy interacting with cold dark matter
• Constraints on interacting dark energy models through cosmic chronometers and Gaussian process
• Testing the quasi-static approximation in $f(R)$ gravity simulations
• Probing the imprint of interacting dark energy on very large scales
• Distinguishing interacting dark energy from wCDM with CMB, lensing, and baryon acoustic oscillation data
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• Coupled Quintessence and the Halo Mass Function
• Speeding up N-body simulations of modified gravity: Vainshtein screening models
• Quantifying the impacts of future gravitational-wave data on constraining interacting dark energy
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• Models of vacuum energy interacting with cold dark matter: Constraints and comparison
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• Weak lensing predictions for coupled dark energy cosmologies at non-linear scales
• DM haloes in the fifth-force cosmology
• The signature of the scattering between dark sectors in large scale cosmic microwave background anisotropies
• Raytracing simulations of coupled dark energy models
• Wormhole solutions supported by interacting dark matter and dark energy
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• New observational constraints on interacting dark energy using galaxy clusters virial equilibrium states
• The CIDER simulations: Nonlinear structure formation in the Constrained Interacting Dark Energy Scenario
• Chameleon dark matter stars
• The modified Newtonian dynamics with an extra anti-dissipation term can yield the MOND model