Cosmology of Antisymmetric Tensor Field in D-brane Universe

Abstract

We analyze homogeneous, anisotropic cosmology driven by a self-interacting ``massive'' antisymmetric tensor field $B_{\mu \nu }$ which is present in string theories with D-branes. Time-dependent magnetic $B$ field existing in the early universe can lead to the Bianchi type I universe. Evolutions of such a tensor field are solved exactly or numerically in the universe dominated by vacuum energy, radiation, and $B$ field itself. The matter-like behavior of the $B$ field (dubbed as ``$B$-matter'') ensures that the anisotropy disappears at late time and thus becomes unobservable in a reasonable cosmological scenario. Such a feature should be contrasted to the cosmology of the conventional massless antisymmetric tensor field.

arXiv comment13 pages

References in corpus (9)

• Low energy effective string cosmology
• String--Kaluza--Klein Cosmology
• String Cosmology with a Time-Dependent Antisymmetric Tensor Potential
• Kaluza-Klein anisotropy in the CMB
• Magneto-dilatonic Bianchi-I cosmology: isotropization and singularity problems
• Anisotropy in Bianchi-type brane cosmologies
• String-Dominated Cosmology
• Chaos-order transition in Bianchi I non-Abelian Born-Infeld cosmology
• Isotropisation of Bianchi class A models with a minimally coupled scalar field and a perfect fluid

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• Cosmological implication of antisymmetric tensor field on D-brane
• Inflation on a Pair of D3-brane and D3bar-brane in Klebanov-Strassler Background