{"created":"2023-07-27T06:25:44.324643+00:00","id":9160,"links":{},"metadata":{"_buckets":{"deposit":"f8ea192b-88a8-4c50-959f-b554f53d04b6"},"_deposit":{"created_by":3,"id":"9160","owners":[3],"pid":{"revision_id":0,"type":"depid","value":"9160"},"status":"published"},"_oai":{"id":"oai:kanazawa-u.repo.nii.ac.jp:00009160","sets":["934:935:936"]},"author_link":["10640","459"],"item_4_biblio_info_8":{"attribute_name":"書誌情報","attribute_value_mlt":[{"bibliographicIssueDates":{"bibliographicIssueDate":"2015-08-06","bibliographicIssueDateType":"Issued"},"bibliographicIssueNumber":"4","bibliographicPageStart":"043507","bibliographicVolumeNumber":"92","bibliographic_titles":[{"bibliographic_title":"Physical Review D - Particles, Fields, Gravitation and Cosmology"}]}]},"item_4_description_21":{"attribute_name":"抄録","attribute_value_mlt":[{"subitem_description":"The relationship between the cosmic microwave background radiation temperature and the redshift, i.e., the T-z relation, is examined in a phenomenological dissipative model. The model contains two constant terms, as if a nonzero cosmological constant Λ and a dissipative process are operative in a homogeneous, isotropic, and spatially flat universe. The T-z relation is derived from a general radiative temperature law, as appropriate for describing nonequilibrium states in a creation of cold dark matter model. Using this relation, the radiation temperature in the late Universe is calculated as a function of a dissipation rate ranging from μ=0, corresponding to a nondissipative lambda cold dark matter model, to μ=1, corresponding to a fully dissipative creation of cold dark matter model. The T-z relation for μ=0 is linear for standard cosmology and is consistent with observations. However, with increasing dissipation rate μ, the radiation temperature gradually deviates from a linear law because the effective equation-of-state parameter varies with time. When the background evolution of the Universe agrees with a fine-tuned pure lambda cold dark matter model, the T-z relation for low μ matches observations, whereas the T-z relation for high μ does not. Previous work also found that a weakly dissipative model accords with measurements of a growth rate for clustering related to structure formations. These results imply that low dissipation is likely for the Universe. The weakly dissipative model should be further constrained by recent observations. © 2015 American Physical Society.","subitem_description_type":"Abstract"}]},"item_4_publisher_17":{"attribute_name":"出版者","attribute_value_mlt":[{"subitem_publisher":"American Physical Society"}]},"item_4_relation_12":{"attribute_name":"DOI","attribute_value_mlt":[{"subitem_relation_type":"isIdenticalTo","subitem_relation_type_id":{"subitem_relation_type_id_text":"10.1103/PhysRevD.92.043507","subitem_relation_type_select":"DOI"}}]},"item_4_source_id_11":{"attribute_name":"NCID","attribute_value_mlt":[{"subitem_source_identifier":"AA00773624","subitem_source_identifier_type":"NCID"}]},"item_4_source_id_9":{"attribute_name":"ISSN","attribute_value_mlt":[{"subitem_source_identifier":"1550-7998","subitem_source_identifier_type":"ISSN"}]},"item_4_version_type_25":{"attribute_name":"著者版フラグ","attribute_value_mlt":[{"subitem_version_resource":"http://purl.org/coar/version/c_970fb48d4fbd8a85","subitem_version_type":"VoR"}]},"item_creator":{"attribute_name":"著者","attribute_type":"creator","attribute_value_mlt":[{"creatorNames":[{"creatorName":"Komatsu, Nobuyoshi"}],"nameIdentifiers":[{},{},{},{}]},{"creatorNames":[{"creatorName":"Kimura, Shigeo"}],"nameIdentifiers":[{},{},{}]}]},"item_files":{"attribute_name":"ファイル情報","attribute_type":"file","attribute_value_mlt":[{"accessrole":"open_date","date":[{"dateType":"Available","dateValue":"2017-10-03"}],"displaytype":"detail","filename":"TE-PR-KOMATSU-N-043507.pdf","filesize":[{"value":"614.3 kB"}],"format":"application/pdf","licensetype":"license_note","mimetype":"application/pdf","url":{"label":"TE-PR-KOMATSU-N-043507.pdf","url":"https://kanazawa-u.repo.nii.ac.jp/record/9160/files/TE-PR-KOMATSU-N-043507.pdf"},"version_id":"e36f0ac2-a3ec-4718-9a93-8fcd23577a14"}]},"item_language":{"attribute_name":"言語","attribute_value_mlt":[{"subitem_language":"eng"}]},"item_resource_type":{"attribute_name":"資源タイプ","attribute_value_mlt":[{"resourcetype":"journal article","resourceuri":"http://purl.org/coar/resource_type/c_6501"}]},"item_title":"Cosmic microwave background radiation temperature in a dissipative universe","item_titles":{"attribute_name":"タイトル","attribute_value_mlt":[{"subitem_title":"Cosmic microwave background radiation temperature in a dissipative universe"}]},"item_type_id":"4","owner":"3","path":["936"],"pubdate":{"attribute_name":"公開日","attribute_value":"2017-10-03"},"publish_date":"2017-10-03","publish_status":"0","recid":"9160","relation_version_is_last":true,"title":["Cosmic microwave background radiation temperature in a dissipative universe"],"weko_creator_id":"3","weko_shared_id":-1},"updated":"2023-07-28T01:58:07.528262+00:00"}