In the early Universe, a dual component made of coupled CDM and a scalar field Φ, if their coupling β > (3)1/2/2, owns an attractor solution, making them a stationary fraction of cosmic energy during the radiation dominated era. Along the attractor, both such components expand a-4 and have early density parameters Ωd = 1/(4β 2) and Ωc = 2 Ωd (field and CDM, respectively). In a previous paper it was shown that, if a further component, expanding a -3, breaks such stationary expansion at z ∼ 3-5 × 10 3, cosmic components gradually acquire densities consistent with observations. This paper, first of all, considers the case that this component is warm. However, its main topic is the analysis of fluctuation evolution: out of horizon modes are then determined; their entry into horizon is numerically evaluated as well as the dependence of Meszaros effect on the coupling β; finally, we compute: (i) transfer function and linear spectral function; (ii) CMB Cl spectra. Both are close to standard ΛCDM models; in particular, the former one can be so down to a scale smaller than Milky Way, in spite of its main DM component being made of particles of mass < 1 keV. The previously coupled CDM component, whose present density parameter is (10-3), exhibits wider fluctuations δρ/ρ, but approximately β-independent δρ values. We discuss how lower scale features of these cosmologies might ease quite a few problems that ΛCDM does not easily solve. © 2014 IOP Publishing Ltd and Sissa Medialab srl

Bonometto, S., & Mainini, R. (2014). Fluctuations in strongly coupled cosmologies. JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS, 2014(3) [10.1088/1475-7516/2014/03/038].

Fluctuations in strongly coupled cosmologies

MAININI, ROBERTO
Ultimo
2014

Abstract

In the early Universe, a dual component made of coupled CDM and a scalar field Φ, if their coupling β > (3)1/2/2, owns an attractor solution, making them a stationary fraction of cosmic energy during the radiation dominated era. Along the attractor, both such components expand a-4 and have early density parameters Ωd = 1/(4β 2) and Ωc = 2 Ωd (field and CDM, respectively). In a previous paper it was shown that, if a further component, expanding a -3, breaks such stationary expansion at z ∼ 3-5 × 10 3, cosmic components gradually acquire densities consistent with observations. This paper, first of all, considers the case that this component is warm. However, its main topic is the analysis of fluctuation evolution: out of horizon modes are then determined; their entry into horizon is numerically evaluated as well as the dependence of Meszaros effect on the coupling β; finally, we compute: (i) transfer function and linear spectral function; (ii) CMB Cl spectra. Both are close to standard ΛCDM models; in particular, the former one can be so down to a scale smaller than Milky Way, in spite of its main DM component being made of particles of mass < 1 keV. The previously coupled CDM component, whose present density parameter is (10-3), exhibits wider fluctuations δρ/ρ, but approximately β-independent δρ values. We discuss how lower scale features of these cosmologies might ease quite a few problems that ΛCDM does not easily solve. © 2014 IOP Publishing Ltd and Sissa Medialab srl
Articolo in rivista - Articolo scientifico
cosmological parameters from CMBR; dark energy theory; dark matter theory; Astronomy and Astrophysics
English
Bonometto, S., & Mainini, R. (2014). Fluctuations in strongly coupled cosmologies. JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS, 2014(3) [10.1088/1475-7516/2014/03/038].
Bonometto, S; Mainini, R
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/10281/106205
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