On Warped String Vacuum Profiles and Cosmologies, I. Supersymmetric Strngs. (arXiv:2109.06852v1 [hep-th])

<a href="http://arxiv.org/find/hep-th/1/au:+Mourad_J/0/1/0/all/0/1">J. Mourad</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Sagnotti_A/0/1/0/all/0/1">A. Sagnotti</a>

We investigate in detail solutions of supergravity that involve warped

products of flat geometries of the type M(p+1) x R x T(D-p-2) depending on a

single coordinate. In the absence of fluxes, the solutions include flat space

and Kasner-like vacua that break all supersymmetries. In the presence of a

symmetric flux, there are three families of solutions that are characterized by

a pair of boundaries and have a singularity at one of them, the origin. The

first family comprises supersymmetric vacua, which capture a universal limiting

behavior at the origin. The first and second families also contain

non–supersymmetric solutions whose behavior at the other boundary, which can

lie at a finite or infinite distance, is captured by the no–flux solutions.

The solutions of the third family have a second boundary at a finite distance

where they approach again the supersymmetric backgrounds. These vacua exhibit a

variety of interesting scenarios, which include compactifications on finite

intervals and (p+1)-dimensional effective theories where the string coupling

has an upper bound. We also build corresponding cosmologies, and in some of

them the string coupling can be finite throughout the evolution.

We investigate in detail solutions of supergravity that involve warped

products of flat geometries of the type M(p+1) x R x T(D-p-2) depending on a

single coordinate. In the absence of fluxes, the solutions include flat space

and Kasner-like vacua that break all supersymmetries. In the presence of a

symmetric flux, there are three families of solutions that are characterized by

a pair of boundaries and have a singularity at one of them, the origin. The

first family comprises supersymmetric vacua, which capture a universal limiting

behavior at the origin. The first and second families also contain

non–supersymmetric solutions whose behavior at the other boundary, which can

lie at a finite or infinite distance, is captured by the no–flux solutions.

The solutions of the third family have a second boundary at a finite distance

where they approach again the supersymmetric backgrounds. These vacua exhibit a

variety of interesting scenarios, which include compactifications on finite

intervals and (p+1)-dimensional effective theories where the string coupling

has an upper bound. We also build corresponding cosmologies, and in some of

them the string coupling can be finite throughout the evolution.

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