A family of solutions to this equation scale with time to the two-thirds times one over the quantity "one plus w" power where w is equal to one-third for models involving optically thick conditions. One can derive an equation of state for a fluid pressure which can then be plugged into the first derivative of this equation to obtain a namesake acceleration equation. This equation typically includes four terms proportional to powers of redshift which represent matter, radiation, curvature and the cosmological constant and those terms are set equal to the square of the Hubble parameter. For 10 points, name this important equation in cosmology w
A family of solutions to this equation scale with time to the two-thirds times one over the quantity "one plus w" power where w is equal to one-third for models involving optically thick conditions. One can derive an equation of state for a fluid pressure which can then be plugged into the first derivative of this equation to obtain a namesake acceleration equation. This equation typically includes four terms proportional to powers of redshift which represent matter, radiation, curvature and the cosmological constant and those terms are set equal to the square of the Hubble parameter. For 10 points, name this important equation in cosmology which describes the homogenous and isotropic expansion of space and can be derived using a quadruply-eponymous metric that takes its name from Lemaitre, Robertson, Walker and this equation's namesake.
A family of solutions to this equation scale with time to the two-thirds times one over the quantity "one plus w" power where w is equal to one-third for models involving optically thick conditions.
Friedmann Equation