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Figure 1:
Layout of the main relations covered in this review. |
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Figure 2:
Different superstring formulations require curved backgrounds to be on-shell. |
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Figure 3:
Set of half-BPS branes discussed in this review, their tensions and some of their connections under T-duality and the strongly-coupled limit of type IIA. |
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Figure 4:
Schematic diagram describing the derivation of Buscher’s T-duality rules using type IIA/IIB supergravities. |
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Figure 5:
Kappa symmetry and world volume diffeomorphisms allow one to couple the brane degrees of freedom to the superfield components of supergravity in a manifestly covariant and supersymmetric way. Invariance under kappa symmetry forces the background to be on-shell. The gauge fixing of these symmetries connects the GS formulation with world volume supersymmetry, whose on-shell degrees of freedom match the Goldstone modes of the brane supergravity configurations. |
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Figure 6:
Set of relations involving kappa symmetry, spacetime supersymmetry algebras, their bounds and their realisation as field theory BPS bounds in terms of brane solitons using the Hamiltonian formulation of brane effective actions. |
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Figure 7:
Relation between the quantisation of the classical moduli space of certain supersymmetric probe configurations, their supergravity realisations and their possible interpretation as black hole constituents. |
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Figure 8:
General framework in which probe calculations in appropriate backgrounds with suitable boundary conditions can be reinterpreted as strongly coupled observables and spectrum in non-abelian gauge theories using the AdS/CFT correspondence. |
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Figure 9:
Conceptual framework in which the probe approximation captures the dynamics of small subsystems interacting with larger ones that have reliable gravity duals. |
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Figure 10:
Open strings stretched between multiple branes and their matrix representation. |
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Figure 11:
Integrating out the degrees of freedom at one loop corresponding to ![]() |
http://www.livingreviews.org/lrr-2012-3 |
Living Rev. Relativity 15, (2012), 3
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