Excepting a Big Rip scenario, there is no eventual 'clash'.
Consider a Friedmann–Lemaître–Robertson–Walker universe:
$$mathrm{d}s^2 = -mathrm{d}t^2 + a^2(t)left[frac{mathrm{d}r^2}{1-kr^2} + r^2left(mathrm{d}theta^2 + sin^2theta,mathrm{d}phi^2right)right]text{,}$$
where $a(t)$ is the scale factor and $kin{-1,0,+1}$ corresponds to a spatially open, flat, or closed cases, respectively. In a local orthonormal frame, the nonzero Riemann curvature components are, up to symmetries:
$$begin{eqnarray*}
R_{hat{t}hat{r}hat{t}hat{r}} = R_{hat{t}hat{theta}hat{t}hat{theta}} = R_{hat{t}hat{phi}hat{t}hat{phi}} =& -frac{ddot{a}}{a} &= frac{4pi G}{3}left(rho + 3pright)text{,} \
R_{hat{r}hat{theta}hat{r}hat{theta}} = R_{hat{r}hat{phi}hat{r}hat{phi}} = R_{hat{theta}hat{phi}hat{theta}hat{phi}} =& frac{k+dot{a}^2}{a^2} &= frac{8pi G}{3}rhotext{,}
end{eqnarray*}$$
where overdot denotes differentiation with respect to coordinate time $t$ and the Friedmann equations were used to rewrite them in terms of density $rho$ and pressure $p$. From the link, note in particular that $dot{rho} = -3frac{dot{a}}{a}left(rho+pright)$.
If dark energy is described by a cosmological constant $Lambda$, as it is in the standard ΛCDM model, then it contributes a constant density and pressure $rho = -p = Lambda/8pi G$, and so no amount of cosmic expansion would change things. Locally, things look just the same as they ever did: for a universe dominated by dark energy, the curvature stays the same, so the gravitational tidal forces do too. Through those tiny tidal forces, the dark energy provides some immeasurably tiny perturbation on the behavior of objects, including atomic nuclei, forcing a slightly different equilibrium size than would be otherwise. But it is so small that that it has no relevance to anything on that scale, nor do those equilibrium sizes change in time. The cosmological constant holds true to its name.
On the other hand, if dark energy has an equation of state $p = wrho$, then a flat expanding universe dominated by dark energy has
$$dot{rho} = -3frac{dot{a}}{a}left(rho+pright) = -3sqrt{frac{8pi G}{3}}left(1+wright)rho^{3/2}text{,}$$
and immediately one can see that there is something special about $w<-1$, leading to an accumulation of dark energy, while the cosmological constant's $w = -1$ leads to no change. This leads to a Big Rip more generally, as zibadawa timmy's answer explains.
? If the metric expands surely objects get further away from one another and that would include the stars inside galaxaies as well as the galaxies themselves?
Not at all. It wouldn't even make any sense: if you have an object like an atom or a star in gravitational freefall, by the equivalence principle only tidal forces across it are relevant. The tidal forces stretch the object until the internal forces balance them. But for a Λ-driven accelerated expansion, dark energy contribution to tidal forces is constant. Hence, an object already in equilibrium has no reason to further change its size, no matter how long the cosmic acceleration occurs. This also applies to galaxies, only that the internal forces are also gravitational and balance the dark energy contribution.
Looking at this in more detail, imagine a test particle with four-velocity $u$, and a nearby one with the same four-velocity, separated by some vector $n$ connecting their worldlines. If they're both in gravitational freefall, then their relative acceleration is given by the geodesic deviation equation, $frac{D^2n^a}{dtau^2} = -R^alpha{}_{mubetanu}u^mu u^nu n^beta$. The gravitoelectric part of the Riemann tensor, $mathbb{E}^alpha{}_beta = R^alpha{}_{mubetanu}u^mu u^nu$, represents the static tidal forces in a local inertial frame comoving with $u$, which will drive those particles apart (or together, depending). Hence, keeping those particles at the same distance would require a force between them, but it's not necessary for this force to change unless the tidal forces also change.
Galaxies don't change size through cosmological expansion. Stars don't either, nor do atoms. Not for Λ-driven expansion, at least. It would take an increase in tidal forces, such as those provided by a Big Rip, for them to do so.
A related way of looking at the issue is this: according to the Einstein field equation, the initial acceleration of a small ball of initially comoving test particles with some four-velocity $u$ (in the comoving inertial frame), which is given by the Ricci tensor, turns out to be:
$$lim_{Vto 0}left.frac{ddot{V}}{V}right|_{t=0}!!!!= -underbrace{R_{munu}u^mu u^nu}_{mathbb{E}^alpha{}_alpha} = -4pi G(rho + 3p)text{,}$$
where $rho$ is density and $p$ is the average of the principal stresses in the local inertial frame. For a positive cosmological constant, $rho = -p>0$, and correspondingly a ball of test particles will expand. That's cosmic expansion on a local scale; because of uniformity of the FLRW universe, the same proportionality works on the large scale as well, as we can think of distant galaxies as themselves test particles if their interactions are too minute to make a difference.
Again, we are led to the same conclusion: if the ball has internal forces that prevent expansion, then those forces don't need to change in time unless the dark energy density also changes, which doesn't happen for cosmological constant. If they're not 'clashing' now, then they won't need to in the future either.
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