Confusion about entropy when applied to the whole universe. What are the macrostates? I'm really confused about the concept of entropy when applied to the whole universe. The often hear that the universe started with very low entropy and as the entropy increases the universe will slowly reach the heat death. The initial low entropy at the big bang is also used to explain the arrow of time.
I just do not understand these arguments. My main problem is with the concept of entropy. To me, the entropy make sense only and only if we define the macrostates we work with. If we want to talk about entropy of the whole universe we have to mention the macrostates we work with.
So when people talk about entropy of the universe, what macrostates do they have in mind?
Also, when we reach the supposed "heat death of the universe". I do not see any reason why we would not be able to use different macroscopic variable in which the universe would not look like as in its "heat death" state.
 A: It sounds like you're under the impression that people are claiming to have a general formulation of thermodynamics that gives a complete and rigorous description of cosmology, generalizing all of the 19th-century laws of thermodynamics in an appropriate way. As far as I know, nobody in the field really makes that claim.
One reason I'm pretty sure we don't have anything like this is that the first law of thermodynamics is conservation of energy, which is usually stated in terms of a global quantity that stays the same. But general relativity does not have a global, scalar, conserved measure of energy that applies to cosmological spacetimes. (It does have things like local conservation of energy-momentum, and conservation of energy in asymptotically flat spacetimes, but that's not the same thing.)
The laws of thermodynamics also refer to temperature, but there is no really satisfactory relativistic definition of temperature.
There are the laws of black hole thermodynamics, but those don't really connect to the ordinary laws of thermodynamics in a comprehensive way, and the way that time-reversal asymmetry comes in seems to me to be qualitatively different from the way it works in standard thermodynamics. Basically you get time-reversal asymmetry in the second law of black hole thermodynamics simply because you define a horizon as a surface from which you can't reach future null infinity.
So when people (including me) say that the arrow of time comes from the fact that we had a low-entropy big bang -- well, I can only speak for myself, but I say that in a loose way, not believing that there is any fully systematic underlying theory.

So when people talk about entropy of the universe, what macrostates do they have in mind? [...] Also, when we reach the supposed "heat death of the universe". I do not see any reason why we would not be able to use different macroscopic variable in which the universe would not look like as in its "heat death" state.

I don't quite understand what objections you have in mind here, though. These seem like questions that are not qualitatively different from the ones we would ask about a steam engine, and the answers would be pretty much the same, wouldn't they? Maybe you could edit your answer to spell out in more detail what you have in mind. E.g., are you worried about how to handle the time variable, so that we can say that the macrostate is the state at a certain time? (If so, then I think the answer would be that you can take any Cauchy surface that you like.)
A: There are different definitions for "makro-state" floating arround. In my opinion the most natural one is that a makro-state is identified with a probability distribution $\rho$ which is defined on the mikro states of the system. 
This definition works out for the universe as well: The mikrostates of the universe would be every possible little degree of freedom of every little particle that you can imagine. If the universe consists of n-particles (and we want to stay classical...) then the mikrostates would be points in the 6N-dimensional Phase space, containing 3 position and 3 momentum variables for each particle: $\vec{x}_1$, $\vec{x}_2$ .... and $\vec{p}_1$, $\vec{p}_2$ ... and so on.
The Makrostate the universe is in would then be a probabillity distribution $\rho(\vec{x}_1, \vec{x}_2 ....., \vec{p}_1,\vec{p}_2.....)$ that tells you what combination of momentums and positions is more or less probable. 
It makes sense to define entropy as a functional on this probability density as $S = \int \rho Ln (\rho)$: This way for the entire universe, because it is defined in the exact same way for all its subsystems (like for example a hot pot of tea). 
To adress you second question:
The assumption is now that entropy as a functional of $\rho$ will grow throughout the time evolution of $\rho$ (there are plausibility arguments why it as to grow, and that aside, this is has proven to be an excellent assumption when one tries to find the steady state of a system). If $\rho$ doesn't change anymore (it reached a steady state), the entropy should be at its maximum (the maximum in the space of all possible probability distributions). While this steady state appears rather quick in a teapot in which you pour in your milk, the universe is not (yet?) in it's steady state. 
When will this steady state (called heat death) happen - There are different assumptions on when it will happen, or if it will happen at all. The problem is that systems that reach their steady state are either supposed to be isolated, or in contact with a reservoir, that together with the system then forms a closed system. For the universe, whose components undergo an accelleration whe yet don't know where it comes from, one can't claim that the observable univsere is an isolated system. 
To adress your last question: Heat death is the steady state for the makrostate $\rho$ of the universe. If this makrostate $\rho$ doesn't change anymore, then any makroscopic variable $O = \int \rho O$ (integral over all mikrostates) doesn't change as well. Any makroscopic variable you can think of would be static as well. 
