- #71
PeterDonis
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timmdeeg said:it seems that the expansion scalar (being a single number) is defined by a "particular set of worldlines".
The expansion scalar is a property of a set of worldlines, yes. But every set of worldlines has one; it's not a property that only particular sets of worldlines (like the "comoving" worldlines in cosmology) have.
timmdeeg said:Lets consider a ball consisting of comoving particles. Are their worldlines such a particular set of worldlines?
Yes.
timmdeeg said:Assuming the cosmological principle the ball expands or shrinks spherically symmetric
If the ball is made up of "comoving" worldlines in our expanding universe, then it will be expanding (have a positive expansion scalar). If it is shrinking, it cannot be a ball of "comoving" worldlines in our actual universe; it must be a ball of "comoving" worldlines in some other spacetime.
timmdeeg said:I'm just guessing, yields energy density combined with pressure a scalar which decides if the ball and thus the universe expands or shrinks?
If we adopt standard cosmological coordinates, then in those coordinates the expansion scalar for the set of "comoving" worldlines appears as the quantity ##\dot{a} / a##, where ##a## is the scale factor--i.e., the Hubble parameter. The quantity you wrote down, ##- \left( \rho + 3 p \right)##, which is the RHS of the second Friedmann equation, is related to the rate of change of the expansion scalar. Ordinary matter and energy will always have ##\rho + 3p## positive, which means the rate of change of the expansion scalar will be negative--the expansion will get slower and slower, and might eventually reverse (depending on the initial conditions). Dark energy, however, has ##\rho + 3p## negative, which means it causes the expansion scalar to increase, not decrease. This is what is referred to as "accelerating expansion"; in this scenario, the expansion scalar will never become negative.