1. Assume a flat Friedmann-Robertson-Walker universe dominated by a cosmological constant. Calculate the time evolution of the scale factor a. Choose as initial condition a(t0) = a0. 2. Using the energy conservation equation, derive the equation of state for a cosmological constant. 3. Assume an open Friedmann-Robertson-Walker universe dominated by its curvature. Calculate the time evolution of the scale factor a. Choose as initial condition a(t0) = a0.
1. Assume a flat Friedmann-Robertson-Walker universe dominated by a cosmological constant. Calculate the time evolution of the scale factor a. Choose as initial condition a(t0) = a0. 2. Using the energy conservation equation, derive the equation of state for a cosmological constant. 3. Assume an open Friedmann-Robertson-Walker universe dominated by its curvature. Calculate the time evolution of the scale factor a. Choose as initial condition a(t0) = a0.
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1. Assume a flat Friedmann-Robertson-Walker universe dominated by a cosmological constant. Calculate the time evolution of the scale factor a. Choose as initial
condition a(t0) = a0.
2. Using the energy conservation equation, derive the equation of state for a cosmological constant.
3. Assume an open Friedmann-Robertson-Walker universe dominated by its curvature.
Calculate the time evolution of the scale factor a. Choose as initial condition a(t0) =
a0.
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