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 $\phi$ related to the gaugino condensate via $\lambda^T\lambda=\phi^3.$ 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 $$\drr=A\cdot \ 10^3\cdot\ \left(\frac{m_{SUSY}}{m_{Pl}}\right)^{\half}\ \left(\frac{\lambda}{100\ \mbox{Mpc}}\right)^{0.03}\ \ ,$$ 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 $T\sim 1\tev.$ This {\em necessitates} that the presently observed baryon asymmetry be generated at a cosmic temperature below 1 TeV.