Bubble Wall Dynamics at Finite Temperature

INTRODUCTION In this work, we consider bubble dynamics in the context of cosmological phase transitions. It is believed that higher degrees of symmetries were realized in nature at higher temperatures of the early universe compared to the symmetries of the present epoch. As the temperature came down along with the expansion of space, there may have ocurred successive symmetry breakings and corresponding phase transitions. These phase transitions can produce many interesting remnants that can significantly affect the subsequent evolution of the universe. Topological defects such as magnetic monopoles, domail walls, cosmic strings and textures can be produced in the process of phase transitions. Inflation is considered in connection with the phase transition at the GUT scale(10 14 GeV ). Baryogenesis may be connected with the elecroweak phase transition at about 10 2 GeV . Quark-hadron phase transition at about 100 MeV<