Abstract
After years of studying particle physics, it’s easy to conflate Gauge Theory with quantum field theories of vector fields. But classically a gauge symmetry refers to an infinte group of symmetry transformation where one must - or is at least entitled to - fix a gauge in order to work practically with the theory.
The equations of General Relativity are known to be invariant under suitable changes of coordinates, or diffeomorphisms of spacetime. This diffeomorphism invariance operates as a gauge symmetry.
With it’s assumptions of homogeneity and isotropy, the cosmological metric named for Friedmann, Lemaître, Robertson and Walker (FLRW) serves as an excellent toy model to study this gauge symmetry. This so-called "minisuperspace" also exposes us to the difference between assumed symmetries ( in this case, space ) and enforced symmetries (time). This lecture series will study this limited class of "time-diffeomorphisms" through the avatar of cosmic inflation: a single, neutral scalar moving in an FLRW background.
We begin our series with a full constraint analysis of this system. We find that the Friedmann equation is not an equation of motion at all but a Hamiltonian constraint, that the Lapse function (N) is pure gauge, and therefore that choosing a clock is a gauge choice. The dissipative "contact" descriptions the later posts compute in are then what you get by reducing this constrained symplectic system and their apparent pathologies are artifacts of the reduction, not the physics.
1 Time is not absolute
In ordinary mechanics the Hamiltonian generates time evolution and time is a parameter you are handed. In General Relativity neither is true: the theory is invariant under relabelling the time coordinate, and that invariance turns the Hamiltonian into a constraint. For the full theory this is the notorious “problem of time.” For a homogeneous universe it is not notorious at all - it is a short, completely explicit calculation, and doing it once fixes the vocabulary for everything that follows. So let us do it.
2 The minisuperspace Lagrangian
The standard ADM metric for the Hamiltonian description of General Relativity is
| (1) |
Here is called the Lapse function, and is the Shift vector. The spatial metric is determined by . This is essentially the four-dimensional metric broken down to a three-dimensional metric description. In principle all three of these objects are viable degrees of freedom.
The present "minisuperspace" set up fixes to zero by fiat, and enforces the FLRW metric by fixing
| (2) |
Hence the metric under consideration becomes
| (3) |
and the action in reduced Planck units (). Homogeneity collapses the field theory to a mechanics problem; per unit comoving volume, dropping a boundary term,
| (4) |
Two things are worth pausing on. First, the lapse appears without a time derivative. It is not a coordinate that evolves, but a multiplier we get to choose. Second, the scale-factor kinetic term carries a minus sign: the metric on configuration space (the DeWitt metric) is Lorentzian, with the timelike direction. That indefinite signature is the fingerprint of gravity hiding inside a mechanics problem, and it is why the quantum version is a wave equation, not a diffusion.
3 Momenta, and a constraint for free
The conjugate momenta follow from (4):
| (5) |
The last is not a definition of a velocity - it is a primary constraint11 1 Here and in what follows, we are using Dirac’s language of constrained Hamiltonian systems. So weakly equals represented by here, means equals up to a constraint. It’s a bookkeeping device., : the lapse has no dynamics. Legendre-transforming (and keeping around, as Dirac instructs),
| (6) |
The entire Hamiltonian is the lapse times . That is the first sign that something is unusual: in a normal theory is a fixed function on phase space; here it is proportional to a quantity we are free to scale.
4 Dirac consistency: the Friedmann equation is a constraint
A constraint is only consistent if it is preserved in time. Demanding and using gives
| (7) |
so the primary constraint drags a secondary constraint into existence: . No further constraints appear (the chain closes), and is first class - it Poisson-commutes with itself and with . Now substitute the momenta back into :
| (8) |
i.e.
| (9) |
That is to say, the Friedmann equation is the Hamiltonian constraint. It is not an equation of motion the system obeys as it evolves; it is a condition that carves out the physical surface in phase space, and the dynamics never leaves it22 2 For completeness, the genuine equations of motion generated by are and , which combine to - the scalar field equation we know from the study of inflation..
5 Why the clock is a gauge choice
Now, on the constraint surface, the total Hamiltonian vanishes,
| (10) |
and , the thing that remains, does not evolve the system forward in time. Being first class, it generates gauge transformations. What looks like “evolution” is the flow of the constraint, and the arbitrary function multiplying it is the lapse . Different choices of are different gauge fixings of one and the same physical history. In other words:
there is no preferred time; picking a clock means fixing the Lapse function.
This is the concrete, minisuperspace face of the problem of time, and is the raison d’être for these notes. is cosmic time; is conformal time; is the e-fold clock in which the inflaton dynamics becomes autonomous and its velocity is bounded, .
Each is a legitimate section of the same gauge orbit, and this is the whole moral of our series, each makes some features manifest and hides others. Just like choosing a gauge in electromagnetism. In part 2, we work through a menu of such choices.
6 From symplectic to contact: where the later posts live
The unreduced phase space carries the canonical symplectic form . Restricted to , this is the Gibbons–Hawking–Stewart structure, and serves as a natural measure on classical universes [3, 4]. The system also has a dynamical similarity: rescaling the spatial volume (and the momenta to match) maps solutions to solutions and leaves the field dynamics untouched. This is equivalent to the statement, in canonical dress, that the overall scale of is classically invisible. Sloan observed that quotienting the symplectic system by this similarity yields a contact system [5, 6]: odd-dimensional, with a genuine dissipative flow whose friction is precisely the non-conservation of the reduced Liouville measure.
Which variable you eliminate in the quotient is itself a choice. Sloan removes the volume and keeps a Hubble-like coordinate , evolving in cosmic time, with contact form and contact Hamiltonian . The presentation this series uses instead eliminates through the Friedmann constraint and keeps as the time. In this context we have the “time-derivative”
Hence this gauge choice lands on the reduced flow for with the state-dependent friction . These are two sections of the same reduction - plausibly related by a contactomorphism and a reparametrization, a point worth settling but not needed here. The contact reduction itself is Sloan’s; what is new downstream is the e-fold presentation and the use it is put to (the Itzhaki–Kovetz fixed point and its Arnold-singularity structure).
7 What this buys the rest of the series
The lesson to carry forward is a hierarchy. Underneath everything sits a constrained symplectic system with no preferred time. Choosing a clock (Part 2) gauge-fixes the lapse. Eliminating then reduces that system to a lower-dimensional contact description (Part 3), where a surprising amount of rigid geometry becomes visible. And when that reduced description appears to break at a zero-energy vacuum, where the field kinates and the contact picture degenerates. We discuss this in detail (Part 4), where we find that nothing has actually gone wrong with the physics: we have merely run a gauge-and-reduction choice past its domain of validity. The cure is to un-reduce, to give back and return to the constrained symplectic system we started from here. The series is, in the end, a round trip through this diagram, and this post is the fixed point it departs from and returns to.
References
- [1] R. Arnowitt, S. Deser, C. W. Misner, The Dynamics of General Relativity, in Gravitation: an Introduction to Current Research, L. Witten ed. (Wiley, 1962), ch. 7; reprinted arXiv:gr-qc/0405109.
- [2] P. A. M. Dirac, Lectures on Quantum Mechanics (Belfer Graduate School of Science, Yeshiva University, 1964).
- [3] G. W. Gibbons, S. W. Hawking, J. M. Stewart, A natural measure on the set of all universes, Nucl. Phys. B 281 (1987) 736.
- [4] G. W. Gibbons, N. Turok, The Measure Problem in Cosmology, Phys. Rev. D 77 (2008) 063516, arXiv:hep-th/0609095.
- [5] D. Sloan, Dynamical Similarity, Phys. Rev. D 97 (2018) 123541, arXiv:1803.04472.
- [6] D. Sloan, Scalar Fields and the FLRW Singularity, Class. Quantum Grav. 36 (2019) 235004, arXiv:1907.08287.