No-scale Supergravity Models Research Articles

Finite temperature corrections in SU( N, 1) supergravity

We compute finite temperature corrections to the scalar potential in maximally symmetric SU( N, 1) supergravity. In the large N limit, the zero temperature potential is only scaled by the thermal corrections. As an example, we apply the general result to a class of phenomenologically interesting no-scale supergravity models.

Non-compact supergravity solves problems

Abstract We present a class of no-scale supergravity models based on maximally symmetric non-compact Kahler manifolds which (i) have m 3 2 ⪡O(m W ) ; (ii) respect all particle physics and cosmological constraints on gravitinos; (iii) allow the QCD θ parameter to relax harmlessly to zero; (iv) contain an axion-like particle compatible with particle physics and astrophysics constraints; (v) have a hidden sector that does not contain excessive axion vacuum energy.

A maximally symmetric no-scale inflationary universe

We present an inflationary model, based on maximally symmetric no-scale supergravity models, where the gravitino and inflation scale cosmological problems are solved simultaneously by means of a heavy — but weakly coupled to ordinary matter — gravitino. The gravitino mass is essentially given by the Hubble constant at the inflationary epoch, H≅10 12 GeV. The reheating temperature of the universe after inflation is T R≅(10 10−10 11) GeV and so gravitinos are no longer regenerated. The grand unified theory suffers a rapid phase transition into the SU(3)×SU(2)×U(1) phase, during — or at the end of — inflation with dilution of magnetic monopoles. The dynamical determination of the electroweak scale predicts top quark masses between 40 and 50 GeV.

No-scale supergravity models with a planck mass gravitino

We construct phenomenological N = 1 supergravity models in which the gravitino may be fixed to have a mass O(10 19 GeV), whilst the weak interaction mass scale is determined by radiative corrections to be hierarchically smaller. Weak gauge symmetry breaking is driven by dynamically determined gaugino masses, and all the SUSY partners of standard model particles have masses O(100) GeV.