WEKO3
アイテム
Entropic cosmology in a dissipative universe
http://hdl.handle.net/2297/40591
http://hdl.handle.net/2297/405912e4d03d8-c789-4fe1-8f0a-5eb820f67289
| 名前 / ファイル | ライセンス | アクション |
|---|---|---|
TE-PR-KOMATSU-N-123516.pdf (596.6 kB)
|
|
| Item type | 学術雑誌論文 / Journal Article(1) | |||||
|---|---|---|---|---|---|---|
| 公開日 | 2017-10-03 | |||||
| タイトル | ||||||
| タイトル | Entropic cosmology in a dissipative universe | |||||
| 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 | |||||
| 著者 |
Komatsu, Nobuyoshi
× Komatsu, Nobuyoshi× Kimura, Shigeo |
|||||
| 書誌情報 |
Physical Review D - Particles, Fields, Gravitation and Cosmology 巻 90, 号 12, p. 123516, 発行日 2014-12-12 |
|||||
| ISSN | ||||||
| 収録物識別子タイプ | ISSN | |||||
| 収録物識別子 | 1550-7998 | |||||
| NCID | ||||||
| 収録物識別子タイプ | NCID | |||||
| 収録物識別子 | AA00773624 | |||||
| DOI | ||||||
| 関連タイプ | isIdenticalTo | |||||
| 識別子タイプ | DOI | |||||
| 関連識別子 | 10.1103/PhysRevD.90.123516 | |||||
| 出版者 | ||||||
| 出版者 | American Physical Society | |||||
| 抄録 | ||||||
| 内容記述タイプ | Abstract | |||||
| 内容記述 | The bulk viscosity of cosmological fluid and the creation of cold dark matter both result in the generation of irreversible entropy (related to dissipative processes) in a homogeneous and isotropic universe. To consider such effects, the general cosmological equations are reformulated, focusing on a spatially flat matter-dominated universe. A phenomenological entropic-force model is examined that includes constant terms as a function of the dissipation rate ranging from μ=0, corresponding to a nondissipative ΛCDM (lambda cold dark matter) model, to μ=1, corresponding to a fully dissipative CCDM (creation of cold dark matter) model. A time-evolution equation is derived for the matter density contrast in order to characterize density perturbations in the present entropic-force model. It is found that the dissipation rate affects the density perturbations even if the background evolution of the late universe is equivalent to that of a fine-tuned pure ΛCDM model. With increasing dissipation rate μ, the calculated growth rate for the clustering gradually deviates from observations, especially at low redshifts. However, the growth rate for low μ(less than 0.1) is found to agree well with measurements. A low-dissipation model predicts a smaller growth rate than does the pure ΛCDM model (for which μ=0). More detailed data are needed to distinguish the low-dissipation model from the pure ΛCDM one. | |||||
| 著者版フラグ | ||||||
| 出版タイプ | VoR | |||||
| 出版タイプResource | http://purl.org/coar/version/c_970fb48d4fbd8a85 | |||||
