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Nonlinear Evolution of Very Small Scale Cosmological Baryon Perturbations at Recombination.

https://hiroshima.repo.nii.ac.jp/records/2006327
https://hiroshima.repo.nii.ac.jp/records/2006327
d66fb660-2265-4ed1-b7e0-96e7fc8d26b1
名前 / ファイル ライセンス アクション
ArXiv1.pdf ArXiv1.pdf (322.8 KB)
Item type デフォルトアイテムタイプ_(フル)(1)
公開日 2023-03-18
タイトル
タイトル Nonlinear Evolution of Very Small Scale Cosmological Baryon Perturbations at Recombination.
言語 en
作成者 Liu, Guo-Chin

× Liu, Guo-Chin

en Liu, Guo-Chin

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Yamamoto, Kazuhiro

× Yamamoto, Kazuhiro

en Yamamoto, Kazuhiro

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Sugiyama, Naoshi

× Sugiyama, Naoshi

en Sugiyama, Naoshi

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Nishioka, Hiroaki

× Nishioka, Hiroaki

en Nishioka, Hiroaki

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アクセス権
アクセス権 open access
アクセス権URI http://purl.org/coar/access_right/c_abf2
権利情報
権利情報 Copyright (c) 2001 The American Astronomical Society.
主題
主題Scheme Other
主題 cosmology: theory
主題
主題Scheme Other
主題 Cosmic microwave background
主題
主題Scheme Other
主題 Large-scale structure of universe
主題
主題Scheme NDC
主題 440
内容記述
内容記述 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, originally proposed by Shaviv in 1998, is studied in detail. We find that inclusion of the diffusion term, which Shaviv neglected in his analysis, results in rather mild growth with growth factor ≪ 100, instead of the enormous amplification, ∼ 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. For these models, it has been found in previous works that the baryon density perturbations are not completely erased by diffusion damping if there are gravitational potential perturbations from the CDM component. Employing the perturbed rate equation derived in this paper, the nonlinear evolution of baryon density perturbations is investigated. We find that: (1) The nonlinear growth is larger for smaller scales. This mechanism only affects perturbations whose scales are smaller than ∼102 M⊙, comparable to stellar scales. (2) The maximum growth factors of baryon density fluctuations for various COBE-normalized CDM models are typically less than a factor of 10 for 3 σ large-scale velocity peaks. (3) The growth factor depends on Ωb.
言語 en
出版者
出版者 University of Chicago Press
言語
言語 eng
資源タイプ
資源タイプ識別子 http://purl.org/coar/resource_type/c_6501
資源タイプ journal article
出版タイプ
出版タイプ VoR
出版タイプResource http://purl.org/coar/version/c_970fb48d4fbd8a85
関連情報
関連タイプ isVersionOf
識別子タイプ DOI
関連識別子 http://dx.doi.org/10.1086/318352
収録物識別子
収録物識別子タイプ ISSN
収録物識別子 0004-637X
開始ページ
開始ページ 1
書誌情報 Astrophysical Journal
Astrophysical Journal

巻 547, p. 1-11, 発行日 2001
旧ID 46
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