Inflation in supersymmetric unified theories

We construct supersymmetric unified models which automatically lead to a period of inflation. The models all involve a U(1) symmetry which does not belong to the MSSM. We consider three different types of models depending on whether this extra U(1) is the subgroup of a non-Abelian gauge group, is a U(1) factor belonging to the visible sector or is a U(1) factor belonging to the hidden sector. Depending on the structure of the unified theory, on the spontaneous symmetry-breaking pattern and on whether we have global or local supersymmetry, inflation may be driven by the nonvanishing vacuum expectation value of an $F$ term or by that of a $D$ term. In both scenarios cosmic strings form at the end of inflation, and they have different properties in each model. Both inflation and cosmic strings contribute to the CMBR temperature anisotropies. We show that the strings contribute to the $C_l$’s up to the level of 75%. Hence the contribution from strings to the CMBR and to the density perturbations in the early Universe which lead to structure formation cannot be neglected. We also discuss a very interesting class of models which involve a $\mathrm{U}{\mathrm{}\left(1\right)\mathrm{}}_{B-L}$ gauge symmetry.