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26 April 2024 |
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Nonlinear Evolution of Very Small Scale Cosmological Baryon Perturbations at Recombination | | Guo-Chin Liu
; Kazuhiro Yamamoto
; Naoshi Sugiyama
; Hiroaki Nishioka
; | | Date: |
16 Jun 2000 | | Journal: | Astrophys.J. 547 (2001) 1-11 | | Subject: | astro-ph | | Affiliation: | 1 and 2), Kazuhiro Yamamoto , Naoshi Sugiyama , Hiroaki Nishioka (NAO Japan,Kyoto Univ.,Hiroshima Univ. | | Abstract: | The evolution of baryon density perturbations on very small scales is investigated. In particular, the nonlinear growth induced by the radiation drag force from the shear velocity field on larger scales during the recombination epoch, which is originally proposed by Shaviv in 1998, is studied in detail. It is found that inclusion of the diffusion term which Shaviv neglected in his analysis results in rather mild growth whose growth rate is $ll 100$ instead of enormous amplification $sim 10^4$ of Shaviv’s original claim since the diffusion suppresses the growth. The growth factor strongly depends on the amplitude of the large scale velocity field. The nonlinear growth mechanism is applied to density perturbations of general adiabatic cold dark matter (CDM) models. In these models, it has been found in the previous works that the baryon density perturbations are not completely erased by diffusion damping if there exists gravitational potential of CDM. With employing the perturbed rate equation which is derived in this paper, the nonlinear evolution of baryon density perturbations is investigated. It is found that: (1) The nonlinear growth is larger for smaller scales. This mechanism only affects the perturbations whose scales are smaller than $sim 10^2M_odot$, which are coincident with the stellar scales. (2) The maximum growth factors of baryon density fluctuations for various COBE normalized CDM models are typically less than factor 10 for $3-sigma$ large scale velocity peaks. (3) The growth factor depends on $Omega_{
m b}$. | | Source: | arXiv, astro-ph/0006223 | | Services: | Forum | Review | PDF | Favorites | |
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