{"@context":{"@vocab":"https://cir.nii.ac.jp/schema/1.0/","rdfs":"http://www.w3.org/2000/01/rdf-schema#","dc":"http://purl.org/dc/elements/1.1/","dcterms":"http://purl.org/dc/terms/","foaf":"http://xmlns.com/foaf/0.1/","prism":"http://prismstandard.org/namespaces/basic/2.0/","cinii":"http://ci.nii.ac.jp/ns/1.0/","datacite":"https://schema.datacite.org/meta/kernel-4/","ndl":"http://ndl.go.jp/dcndl/terms/","jpcoar":"https://github.com/JPCOAR/schema/blob/master/2.0/"},"@id":"https://cir.nii.ac.jp/crid/1360004235009704064.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1103/physrevd.82.046007"}},{"identifier":{"@type":"URI","@value":"http://link.aps.org/article/10.1103/PhysRevD.82.046007"}},{"identifier":{"@type":"URI","@value":"http://harvest.aps.org/v2/journals/articles/10.1103/PhysRevD.82.046007/fulltext"}},{"identifier":{"@type":"DOI","@value":"10.48550/arxiv.1006.2306"}}],"resourceType":"学術雑誌論文(journal article)","dc:title":[{"@value":"Dynamical<mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:mi>p</mml:mi></mml:math>-branes with a cosmological constant"}],"description":[{"notation":[{"@value":"We present a class of dynamical solutions in a D-dimensional gravitational theory coupled to a dilaton, a form field strength, and a cosmological constant. We find that for any D due to the presence of a cosmological constant, the metric of solutions depends on a quadratic function of the brane world volume coordinates, and the transverse space cannot be Ricci flat except for the case of 1-branes. We then discuss the dynamics of 1-branes in a D-dimensional spacetime. For a positive cosmological constant, 1-brane solutions with D>4 approach the Milne universe in the far-brane region. On the other hand, for a negative cosmological constant, each 1-brane approaches the others as the time evolves from a positive value, but no brane collision occurs for D>4, since the spacetime close to the 1-branes eventually splits into the separate domains. In contrast, the D=3 case provides an example of colliding 1-branes. Finally, we discuss the dynamics of 0-branes and show that for D>2, they behave like the Milne universe after the infinite cosmic time has passed."}]},{"notation":[{"@value":"21 pages, 7 figures; v2: minor corrections"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380004235009703936","@type":"Researcher","foaf:name":[{"@value":"Kei-ichi Maeda"}]},{"@id":"https://cir.nii.ac.jp/crid/1380004235009704065","@type":"Researcher","foaf:name":[{"@value":"Masato 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