Compactifications with S-duality twists

Hull, C.M.; Çatal-Özer, Aybike

doi:10.1088/1126-6708/2003/10/034

Cited by 47 publications

(78 citation statements)

References 37 publications

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“…With the available fluxes we can indeed have a term 20) where ωF 3 is a 4-form according to (2.15). We can also add D5 i -branes that wrap T 2 i .…”

Section: T-dual Superpotential and Tadpoles In Iib With O9-planesmentioning

confidence: 99%

More dual fluxes and moduli fixing

Aldazábal¹,

Cámara²,

Font³

et al. 2006

J. High Energy Phys.

180

508

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We generalize the recent proposal that invariance under T-duality leads to additional nongeometric fluxes required so that superpotentials in type IIA and type IIB orientifolds match.We show that invariance under type IIB S-duality requires the introduction of a new set of fluxes leading to further superpotential terms. We find new classes of N =1 supersymmetric Minkowski vacua based on type IIB toroidal orientifolds in which not only dilaton and complex moduli but also Kähler moduli are fixed. The chains of dualities relating type II orientifolds to heterotic and M-theory compactifications suggests the existence of yet further flux degrees of freedom. Restricting to a particular type IIA/IIB or heterotic compactification only some of these degrees of freedom have a simple perturbative and/or geometric interpretation.

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“…With the available fluxes we can indeed have a term 20) where ωF 3 is a 4-form according to (2.15). We can also add D5 i -branes that wrap T 2 i .…”

Section: T-dual Superpotential and Tadpoles In Iib With O9-planesmentioning

confidence: 99%

More dual fluxes and moduli fixing

Aldazábal¹,

Cámara²,

Font³

et al. 2006

J. High Energy Phys.

180

508

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“…Non-geometric backgrounds in string theory, meaning backgrounds that do not admit a metric geometry, for instance emerge in flux compactifications on which one acts with T-dualities or in mirror symmetry [13,14,15,16]. They also appear in compactifications with duality twists, which in some cases have been shown to be equivalent to asymmetric orbifolds [17,18,19]. Generalized geometries built to understand these situations have been originally proposed by Hitchin [20,21] and, the T-fold idea, by Hull [22,23].…”

Section: Invitationmentioning

confidence: 99%

Area metric gravity and accelerating cosmology

Punzi

Schüller

Wohlfarth³

2007

J. High Energy Phys.

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Area metric manifolds emerge as effective classical backgrounds in quantum string theory and quantum gauge theory, and present a true generalization of metric geometry. Here, we consider area metric manifolds in their own right, and develop in detail the foundations of area metric differential geometry. Based on the construction of an area metric curvature scalar, which reduces in the metric-induced case to the Ricci scalar, we re-interpret the Einstein-Hilbert action as dynamics for an area metric spacetime. In contrast to modifications of general relativity based on metric geometry, no continuous deformation scale needs to be introduced; the extension to area geometry is purely structural and thus rigid. We present an intriguing prediction of area metric gravity: without dark energy or fine-tuning, the late universe exhibits a small acceleration. INVITATIONA new theoretical concept which, once formulated, naturally emerges in many related contexts, deserves further study. Even more so, if it makes us view well-established theories in a novel way, and meaningfully points beyond standard theory.Area metrics, we argue in this paper, are such an emerging notion in fundamental physics.An area metric may be defined as a fourth rank tensor field which allows to assign a measure to two-dimensional tangent areas, in close analogy to the way a metric assigns a measure to tangent vectors. In more than three dimensions, area metric geometry is a true generalization of metric geometry; although every metric induces an area metric, not every area metric comes from an underlying metric. The mathematical constructions, and physical conclusions, of the present paper are then based on a single principle:Spacetime is an area metric manifold.We will be concerned with justifying this rather bold idea by a detailed construction of the geometry of area metric manifolds, followed by providing an appropriate theory of gravity, which finally culminates in an application of our ideas to cosmology. In the highly symmetric cosmological area metric spacetimes, we can compare our results easily to those of Einstein gravity. We obtain the interesting result that the simplest type of area metric cosmology, namely a universe filled with non-interacting string matter, may be solved exactly and is able to explain the observed [1,2] very small late-time acceleration of our Universe, see the figure on page 40, without introducing any notion of dark energy, nor by invoking fine-tuning arguments.It may come as a surprise, but standard physical theory itself predicts the departure from metric to true area metric manifolds. More precisely, the quantization of classical theories based on metric geometry generates, in a number of interesting cases, area metric geometries: back-reacting photons in quantum electrodynamics effectively propagate in an area metric background [3]; the massless states of quantum string theory give rise to the Neveu-Schwarz two-form potential and dilaton besides the graviton, producing a generalized geometry which may be neatly...

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“…The consistency can be checked as follows. The (3,19) signature of ρ αβ arises from the fact that 3 of the two-forms on K3 are selfdual, while the other 19 are anti-selfdual. The forms which are Poincaré dual to the P 1 base and the T 2 fibre can be neither selfnor anti-selfdual since both cycles have zero intersection with itself, while the product of a self-/anti-selfdual form with itself vanishes only if the form itself vanishes.…”

Section: Duality Of Heterotic and Type II Compactificationmentioning

confidence: 99%

“…The only thing we have to take care of at this point is that the fluxes can also contribute to the right hand side of the Bianchi identity (2.2). This contribution -when integrated over K3 -is given by [37] 6) where ρ αβ denotes the K3 intersection matrix, ρ αβ = ω α ∧ ω β , which has signature (3,19), while η IJ is the invariant tensor on the SO(2, n v − 1) factor of the moduli space defined in (2.4) which has signature (2, n v − 1). Within the set-up we have presented so far, δ has to vanish for consistency.…”

mentioning

confidence: 99%