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A Further Analysis of a Cosmological Model of Quintessence and Scalar Dark Matter | | T. Matos
; L. A. Urena-Lopez
; | | Date: |
1 Jun 2000 | | Journal: | Phys.Rev. D63 (2001) 063506 | | Subject: | astro-ph | | Affiliation: | CINVESTAV | | Abstract: | We present the complete solution to a 95% scalar field cosmological model in which the dark matter is modeled by a scalar field $Phi$ with the scalar potential $V(Phi)=V_{o}[ cosh {(lambda sqrt{kappa_{o}}Phi)}-1]$ and the dark energy is modeled by a scalar field $Psi$, endowed with the scalar potential $ ilde{V}(Psi)= ilde{V_{o}}[ sinh {(alpha sqrt{kappa_{o}}Psi)}] ^{eta}$. This model has only two free parameters, $lambda$ and the equation of state $omega_{Psi}$. With these potentials, the fine tuning and the cosmic coincidence problems are ameliorated for both dark matter and dark energy and the models agrees with astronomical observations. For the scalar dark matter, we clarify the meaning of a scalar Jeans lenght and then the model predicts a suppression of the Mass Power Spectrum for small scales having a wave number $k > k_{min,Phi}$, where $k_{min,Phi} simeq 4.5 h {
m Mpc}^{-1}$ for $lambda simeq 20.28$. This last fact could help to explain the dearth of dwarf galaxies and the smoothness of galaxy core halos. From this, all parameters of the scalar dark matter potential are completely determined. The dark matter consists of an ultra-light particle, whose mass is $m_{Phi} simeq 1.1 imes 10^{-23} {
m eV}$ and all the success of the standard cold dark matter model is recovered. This implies that a scalar field could also be a good candidate as the dark matter of the Universe. | | Source: | arXiv, astro-ph/0006024 | | Services: | Forum | Review | PDF | Favorites | |
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