Andrei Linde proposes a hybrid inflation model where inflation ends via a rapid 'waterfall' of a scalar field σ, triggered by another scalar field φ. This model combines elements of chaotic inflation and spontaneous symmetry breaking. Inflation ends not through the inflaton potential but via the non-inflationary potential of σ. Another hybrid model combines Brans-Dicke theory, new inflation, and chaotic inflation, avoiding the big-bubble problem through a second-order phase transition. A third model combines Brans-Dicke theory with chaotic inflation, resulting in exponentially large domains with different Planck masses and density perturbations. The hybrid inflation model ends rapidly after φ reaches its critical value, leading to a small Hubble constant at the end of inflation. The model produces density perturbations consistent with COBE data. The model's parameters allow for a wide range of values, making it versatile. The model also exhibits a power-law spectrum of perturbations, which is unusual. The model avoids the problem of initial conditions and allows for different domains with varying Planck masses and density perturbations. The model is compared to other inflationary scenarios and shows that it can produce realistic results without requiring extreme parameters. The author acknowledges contributions from various colleagues and notes that the model is part of a broader effort to understand inflationary cosmology.Andrei Linde proposes a hybrid inflation model where inflation ends via a rapid 'waterfall' of a scalar field σ, triggered by another scalar field φ. This model combines elements of chaotic inflation and spontaneous symmetry breaking. Inflation ends not through the inflaton potential but via the non-inflationary potential of σ. Another hybrid model combines Brans-Dicke theory, new inflation, and chaotic inflation, avoiding the big-bubble problem through a second-order phase transition. A third model combines Brans-Dicke theory with chaotic inflation, resulting in exponentially large domains with different Planck masses and density perturbations. The hybrid inflation model ends rapidly after φ reaches its critical value, leading to a small Hubble constant at the end of inflation. The model produces density perturbations consistent with COBE data. The model's parameters allow for a wide range of values, making it versatile. The model also exhibits a power-law spectrum of perturbations, which is unusual. The model avoids the problem of initial conditions and allows for different domains with varying Planck masses and density perturbations. The model is compared to other inflationary scenarios and shows that it can produce realistic results without requiring extreme parameters. The author acknowledges contributions from various colleagues and notes that the model is part of a broader effort to understand inflationary cosmology.