Harvard University Department of Astronomy

The Cosmological Constant History of the Universe Basic Idea: The universe is expanding and cooling. Different physical processes and components dominate at different temperatures and densities. The growth of horizons means larger scale structures form later. Looking at large distances means looking back in time. General Features of Universe homogeneous and isotropic on large scales Olber's paradox: expanding universe, not at a special place Structure in the universe is evolving (was not always there, combined with finite speed of light gives another resolution) Going Forward in time: general evolutionary features cooling/diluting due to expansion structure growing due to gravitational attraction short history initial conditions (inflation) baryogenesis bbn (first 3 minutes) matter-radiation equality cmb (300,000 years) dark ages first structures their age, fraction of age of universe, in years peak of star formation and quasar activity today and recently Observations are stronger starting at the time of bbn and since. Systems which are simplest: the CMB (where calculations are under control) and those dominated by dark matter (which only use gravity). Both of these will be used later as indirect indications of the cosmological constant. Short statement of paradigm by M. Rees Some references. Home Syllabus References Lecture References Useful Links Contact Info Back to Harvard University Department of Astronomy Academics. Back to Harvard University Department of Astronomy Courses.