Universal dS vacua in STU-models

Abstract

Stable de Sitter solutions in minimal F-term supergravity are known to lie close to Minkowski critical points. We consider a class of STU-models arising from type IIB compactifications with generalised fluxes. There, we apply an analytical method for solving the equations of motion for the moduli fields based on the idea of treating derivatives of the superpotential of different orders up to third as independent objects. In particular, supersymmetric and no-scale Minkowski solutions are singled out by physical reasons. Focusing on the study of dS vacua close to supersymmetric Minkowski points, we are able to elaborate a complete analytical treatment of the mass matrix based on the sGoldstino bound. This leads to a class of interesting universal dS vacua. We finally explore a similar possibility around no-scale Minkowski points and discuss some examples.

What if string theory has no de Sitter vacua?

“…It is interesting to note that many dS-vacua obtained using non-perturbative additions, such as P (S, U )e αiT , with P (S, U ) a polynomial, can be captured using non-geometric fluxes [118]. The non-perturbative features will be different, but local properties such as the existence of a critical point, as well as moduli masses, can be fitted, since these depend only on the first couple of orders in an expansion.…”

Scaling limits of dS vacua and the swampland

“…8 There are several other ingredients that have appeared in the literature. In particular, it has long been known that the inclusion of so called non-geometric Q-and R-fluxes can lead to stable dS vacua [91][92][93][94][95][96]. These fluxes scale like…”

String theory realizations of the nilpotent goldstino

“…When the universal goldstino contribution to energy M 2 is slightly larger than the one from gravitino −3m 2 3/2 , the models describe the dark energy with a cosmological constant Λ in the spirit of the string landscape. 1 For other approaches towards de Sitter space in string compactifications see [17][18][19][20][21][22][23][24][25][26][27][28][29][30][31][32][33][34][35][36]. 2 We write the scalar potential and then the cosmological constant in units of M planck so there is an implicit M 2 planck factor on the right hand side of the equation.…”