Consistent de Sitter string vacua from Kähler stabilization and D‐term uplifting

Parameswaran, Susha L.; Westphal, Alexander

doi:10.1002/prop.200610374

Cited by 19 publications

(11 citation statements)

References 58 publications

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“…This means that these vacua are on specific positions in moduli space for which one can argue that all other, ignored, corrections are subleading. See [81][82][83][84][85][86][87][88][89] for an incomplete list. General conditions on the perturbative stability for such solutions, implied by the sgoldstino, were analysed in [90,91] and provide interesting constraints on model building.…”

Section: Iib String Theorymentioning

confidence: 99%

What if string theory has no de Sitter vacua?

Danielsson

Riet

2018

Int. J. Mod. Phys. D

389

526

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We present a brief overview of attempts to construct de Sitter vacua in string theory and explain how the results of this 20-year endeavor could point to the fact that string theory harbours no de Sitter vacua at all. Making such a statement is often considered controversial and "bad news for string theory". We discuss how perhaps the opposite can be true.2 An interesting light-version of a review on dark energy in string theory can be found in [27] 3 See also [34].

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Section: Iib String Theorymentioning

confidence: 99%

What if string theory has no de Sitter vacua?

Danielsson

Riet

2018

Int. J. Mod. Phys. D

389

526

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“…There are many other possible ways to achieve uplifting of Minkowski and AdS vacua in supergravity, see for instance [36][37][38][39][40]. The main new ingredient that we add to these procedures is finding and uplifting a broad landscape of stable supersymmetric Minkowski vacua.…”

Section: Stu Model and A Polonyi Fieldmentioning

confidence: 99%

Analytic classes of metastable de Sitter vacua

Каллош¹,

Linde²,

Vercnocke³

et al. 2014

J. High Energ. Phys.

113

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In this paper, we give a systematic procedure for building locally stable dS vacua in N = 1 supergravity models motivated by string theory. We assume that one of the superfields has a Kähler potential of no-scale type and impose a hierarchy of supersymmetry breaking conditions. In the no-scale modulus direction the supersymmetry breaking is not small, in all other directions it is of order ǫ. We establish the existence of an abundance of vacua for large regions in the parameter space spanned by ǫ and the cosmological constant. These regions exist regardless of the details of the other moduli, provided the superpotential can be tuned such that the off-diagonal blocks of the mass matrix are parametrically small. We test and support this general dS landscape construction by explicit analytic solutions for the STU model. The Minkowski limits of these dS vacua either break supersymmetry or have flat directions in agreement with a no-go theorem that we prove, stating that a supersymmetric Minkowski vacuum without flat directions cannot be continuously deformed into a non-supersymmetric vacuum. We also describe a method for finding a broad class of stable supersymmetric Minkowski vacua that can be F-term uplifted to dS vacua and which have an easily controllable SUSY breaking scale.

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“…There are several alternatives in the literature, that can be divided into two groups: D-term [81,[109][110][111][112][113][114][115][116] or F-term upliftings [82,83,[117][118][119][120][121][122][123][124][125][126]. To keep our analysis general, following our discussion in Sect.…”

Section: A Simple Casementioning

confidence: 99%

“…Then, from the above equations, it is clear that some subtleties arise in the case b = 3 because then the factor (bβ−3) introduces an additional suppression that is not taken into account by the ε/μ and large volume expansion. On the other hand, b = 3 is quite interesting because explicit uplifting mechanisms exist with this scaling [81][82][83][109][110][111][112][113][114][115][116][117][118][119][120][121][122][123][124][125][126]. A part from the anti D3-brane at the tip of a warped throat that scales with b = 2, we are not aware of any other explicit model with b = 3; such scaling could be interpreted 37 as if the physics responsible for the susy-breaking were localized on a Dp-brane with p = 3.…”

Section: Wwwfp-journalorgmentioning

confidence: 99%

Phenomenological aspects of type IIB flux compactifications

Pajer

2009

Fortschritte der Physik

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The purpose of this work is to investigate how phenomenologically successful constructions in the field of high energy physics can be embedded into a fundamental theory, and what we can learn from this procedure. In fact, the synergy of an effective and a fundamental approach might be very fruitful. On the one hand, it poses several theoretical challenges to potential candidates for a fundamental theory, which might be ruled out or restricted in their generality. On the other hand, this mutual interplay can inspire new experiments and observations or suggest correlations which are invisible from an effective point of view. Our starting point is that string theory is entitled to be a valid candidate for a fundamental theory by a series of properties such as the fact that it is a consistent, UV‐finite, anomaly‐free quantum theory and it describes, in appropriate limits, quantum field theory and general relativity, hence providing a unified description of the four known forces. Within string theory, we choose to work in the framework of type IIB flux compactifications where the issue of moduli stabilization can be successfully addressed. On the phenomenological side, we focus on particle physics and cosmology, and in particular on the MSSM and the mechanism of inflation, respectively. We construct and study two different models of inflation in string theory. These are models of brane inflation, i.e. models where the primordial exponential expansion of the universe is driven by a scalar field representing the position of a D3‐brane (a 3+1‐dimensional dynamical object) in a compact space. We show explicitly that, allowing for fine tuning, a prolonged stage of slow‐roll inflation can be achieved during which perturbations are generated in good agreement with the CMB data. In addition, we give an example of the fruitful synergy we mentioned above. One of our two models, namely inflation at the tip, might induce also DBI inflation which produces peculiar features in the spectrum of density perturbations that might be looked for using CMB data. On the particle physics side, we consider a model, the large volume scenario (LVS), which, among other things, provides a rationale for a low scale susy‐breaking. We perform some checks on the consistency of LVS as a string theory model. To this end, we formulate an educated guess for the form of string loop corrections. We then show that physical predictions such as the soft susy‐breaking terms are actually surprisingly robust against the inclusion of these corrections.

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Consistent de Sitter string vacua from Kähler stabilization and D‐term uplifting

Cited by 19 publications

References 58 publications

What if string theory has no de Sitter vacua?

What if string theory has no de Sitter vacua?

Analytic classes of metastable de Sitter vacua

Phenomenological aspects of type IIB flux compactifications

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