English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We present a detailed study of the finite-temperature behaviour of the LARGEVolume type IIB flux compactifications. We show that certain moduli canthermalise at high temperatures. Despite that, their contribution to thefinite-temperature effective potential is always negligible and the latter hasa runaway behaviour. We compute the maximal temperature $T_{max}$, above whichthe internal space decompactifies, as well as the temperature $T_*$, that isreached after the decay of the heaviest moduli. The natural constraint$T_*<T_{max}$ implies a lower bound on the allowed values of the internalvolume $\mathcal{V}$. We find that this restriction rules out a significantrange of values corresponding to smaller volumes of the order $\mathcal{V}\sim10^{4}l_s^6$, which lead to standard GUT theories. Instead, the bound favoursvalues of the order $\mathcal{V}\sim 10^{15}l_s^6$, which lead to TeV scaleSUSY desirable for solving the hierarchy problem. Moreover, our result favourslow-energy inflationary scenarios with density perturbations generated by afield, which is not the inflaton. In such a scenario, one could achieve bothinflation and TeV-scale SUSY, although gravity waves would not be observable.Finally, we pose a two-fold challenge for the solution of the cosmologicalmoduli problem. First, we show that the heavy moduli decay before they canbegin to dominate the energy density of the Universe. Hence they are not ableto dilute any unwanted relics. And second, we argue that, in order to obtainthermal inflation in the closed string moduli sector, one needs to go beyondthe present EFT description.

LARGE Volume String Compactifications at Finite Temperature