There's a related paper that came out this year. I started a thread about it:
https://www.physicsforums.com/showthread.php?t=680862
It's about the entropy of the gravitational field. People are still searching for a satisfactory definition of that, which will allow it to be measured and assigned a definite value.
When that goal is achieved, the gravitational entropy will be a really major factor in the overall entropy--a key player.
Here's a brief quote from the abstract of the Clifton Ellis Tavakol paper:
"For scalar perturbations of a Robertson-Walker geometry we find that the
entropy goes like the Hubble weighted anisotropy of the gravitational field, and therefore
increases as structure formation occurs."
This is the opposite from what we ordinarily expect from the matter sector. Just looking at matter in a fixed geometry we associate entropy with disorder, the absence of structure. I think having assimilated Layzer's ideas you may already be well aware of what I'm saying, namely that we usually associated ordered STRUCTURE with negative entropy. But under the influence of gravity ordered structure in the universe's matter sector has GROWN.
So this presents a seeming paradox, the structure formation paradox or puzzle. In order to resolve it we need a definition of
entropy in the geometry sector according to which the formation of structure has the opposite effect! Namely the formation of structure must cause the gravitational entropy to increase!
==quote Clifton Ellis Tavako
http://arxiv.org/abs/1303.5612 ==
A key question in cosmology is how to define the entropy in gravitational fields. A suitable definition already exists for the important case of stationary black holes [1], but in the cosmological setting a well-motivated and universally agreeable analogue has yet to be found. Addressing this deficit is an important problem, as in the presence of gravitational interactions the usual statements about matter becoming more and more uniform are incorrect. Instead, structure develops spontaneously when gravitational attraction dominates the dynamics [2, 3]. This behaviour is crucial to the existence of complex structures, and indeed life, in the Universe. The question then arises, how can evolution under the gravitational interaction be made compatible with the second law of thermodynamics? If the second law is valid in the presence of gravity, such that entropy increases monotonically into the future, then the current state of the universe must be considered more probable than the initial state, even though it is more structured. For this to be true, the gravitational field itself must be carrying entropy.
For a candidate definition of gravitational entropy to be compatible with cosmological processes, such as structure formation in the Universe, it needs to be valid in non-stationary and non-vacuum spacetimes. We will argue that an appropriate definition of gravitational entropy should only involve the free gravitational field, as specified by the Weyl part of the curvature tensor, C
abcd [4], and that a particular promising candidate...
==endquote==