Gaugino Condensation as the Origin of Primordial Fluctuations

I present a model for inflation based on the gaugino-dilaton dynamics of supersymmetry breaking. The inflaton is the dimension–1 scalar field $\varphi$ related to the gaugino condensate via ${\lambda }^T\lambda ={\varphi }^3\mathrm{.}$ Recent work in this area is used to obtain two significant results: (1) Scalar density fluctuations at second horizon crossing are generated on scale $\lambda$ with amplitude $$\text{drr}=A\cdot {10}^3\cdot {\left(\frac{m_{SUSY}}{m_{Pl}}\right)}^{\text{half}}{\left(\frac{\lambda }{100Mpc}\right)}^{0.03},$$ where $A$ is a constant which depends on (unknown) details of gaugino-dilaton dynamics in the strong-coupling phase. Agreement with COBE results is obtained if $A\simeq 2.$ \ (2) Due to mixing with hidden sector glueballs, the dilaton mass is large $(\sim \left(\mp
\ms^2\right)^ {\frac{1}{3}}\sim 10^8\ \mbox{GeV}),$ and reheating takes place at $T\sim 1\text{tev}\mathrm{.}$ This {\em necessitates} that the presently observed baryon asymmetry be generated at a cosmic temperature below 1 TeV.