This discussion starts with new stellar evolution calculations that follow the development of the low mass (M type) stars that dominate the stellar IMF.  We then determine the final mass distribution of stellar remnants – the neutron stars, white dwarfs, and brown dwarfs remaining at the end of stellar evolution. After several trillion years, the supply of interstellar gas grows depleted, yet star formation continues at a highly attenuated rate through brown dwarf collisions.  This process tails off as the galaxy gradually loses its stars by ejecting the majority, and driving a minority toward accretion onto massive black holes. As the galaxy disperses, weakly interacting dark matter particles are accreted by white dwarfs, where they subsequently annihilate and keep the old stellar remnants relatively ``warm''.  After accounting for the destruction of the galaxy, we consider the fate of expelled degenerate objects (planets, white dwarfs, and neutron stars) within the assumption that proton decay is a viable process.  The evolution and eventual sublimation of these objects is dictated by the decay of their constituent nucleons; this scenario is developed in some detail. After white dwarfs and neutron stars have disappeared, the black holes slowly lose their mass as they emit Hawking radiation.  After the largest black holes have evaporated, the universe slowly slides into darkness. 

Location and Time: 339 Strong Hall, at noon.