Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://temporology.bio.msu.ru/EREPORTS/rovelli_time.pdf Äàòà èçìåíåíèÿ: Fri Feb 28 02:00:23 2014 Äàòà èíäåêñèðîâàíèÿ: Fri Feb 28 02:01:55 2014 Êîäèðîâêà:

"Forget time"
Essay written for the FQXi contest on the Nature of Time Carlo Rovelli
(Dated: August 24, 2008) Following a line of research that I have developed for several years, I argue that the best strategy for understanding quantum gravity is to build a picture of the physical world where the notion of time plays no role at all. I summarize here this point of view, explaining why I think that in a fundamental description of nature we must "forget time", and how this can be done in the classical and in the quantum theory. The idea is to develop a formalism that treats dependent and independent variables on the same footing. In short, I propose to interpret mechanics as a theory of relations between variables, rather than the theory of the evolution of variables in time.

I.

THE NEED TO FORGET TIME

General relativity has changed our understanding of space and time. The efforts to find a theory capable of describing the expected quantum properties of gravity forces us to fully confront this change, and perhaps even push it further. The spacetime of general relativity, indeed, (a 4d pseudo-riemannian space) is likely to be just a classical approximation that loses its meaning in the quantum theory, for the same reason the trajectory of a particle does (see for instance [1]). How should we then think about time in the future quantum theory of gravity? Here I argue for a possible answer to this question. The answer I defend is that we must forget the notion of time altogether, and build a quantum theory of gravity where this notion does not appear at all. The notion of time familiar to us may then be reconstructed in special physical situations, or within an approximation, as is the case for a number of familiar physical quantities that disappear when moving to a deeper level of description (for instance: the "surface of a liquid" disappears when going to the atomic level, or "temperature" is a notion that makes sense only in certain physical situations and when there are enough degrees of freedom.) I have argued for this point of view in the past in a number of papers [2-13], and in the book [14]. However, I have never tried to articulate this point of view in a compact, direct, and self-contained way. I take therefore the opportunity of the FQXi contest for doing so. In the following I explain in detail what I mean by "forgetting time", why I think it is necessary to do so in order to construct a quantum theory of gravity, and how I think it is possible. The discussion here is general, and focused on the notion of time: I will not enter at all in the technical complications associated with the definition of a quantum theory of gravity (on this, see [14] for one possible approach), but only discuss the change in the notion of time that I believe is required for a deeper understanding of the world, in the light of what we have learned about Nature with general relativity and quantum theory. I am aware that the answer I outline here is only one among many possibilities. Other authors have argued that the notion of time is irreducible, and cannot be left out of a fundamental description of Nature in the way I propose. Until our theoretical and experimental investigations tell us otherwise, I think that what is important is to put the alternatives clearly on the table, and extensively discuss their rationale and consistency. It is in this spirit that I present here the timeless point of view.

I I.

TIME AS THE INDEPENDENT PARAMETER FOR THE EVOLUTION

Until the Relativity revolution, the notion of time played a clear and uncontroversial role in physics. In prerelativistic physics, time is one of the fundamental notions in terms of which physics is built. Time is assumed to "flow", and mechanics is understood as the science describing the laws of the change of the physical systems in time. Time is described by a real variable t. If the state of a physical system can be described by a set of physical variables an , then the evolution of the system is described by the functions an (t). The laws of motion are differential equations for these quantities.1 A comprehensive theoretical framework for mechanics is provided by the Hamiltonian theory. In this, the state of a system with n degrees of freedom is described by 2n variables (qi , pi ), the coordinates of the phase space; the dynamics

1

The idea that physical laws must express the necessary change of the systems in time is very old. It can be traced to the most ancient record we have of the idea of natural law: a fragment from the VI century BC's Greek philosopher Anaximander, that says: Al l things transform into one another, [...] fol lowing the necessity [...] and accor ding to the order of time.


2 is governed by the Hamiltonian H (qi , pi ), which is a function on the phase space; and the equations of motion are given by the Hamilton equations dqi /dt = H/ pi , dpi /dt = - H/ qi . It is clear that the physical variable t is an essential ingredient of the picture and plays a very special role in this framework. This role can be summarized as follows: in pre-relativistic mechanics, time is a special physical quantity, whose value is measured by physical clocks, that plays the role of the independent variable of physical evolution.

I I I.

MECHANICS IS ABOUT RELATIONS BETWEEN VARIABLES

The Relativity revolution has modified the notion of time in a number of ways. I skip here the changes introduced by Special Relativity (in particular, the relativity of simultaneity), which are much discussed and well understood, and concentrate on those introduced by general relativity. In the formalism of general relativity, we can distinguish different notions of time. In particular, we must distinguish the coordinate time t that appears as the argument of the field variable, for instance in gµ (x, t), from the proper time s measured along a given world line = ( µ ( )), defined by s = d gµ ( ( ))d µ /d d /d . The coordinate time t plays the same role as evolution parameter of the equations of motion as ordinary nonrelativistic time. The equations of motion of the theory are indeed the Einstein equations, which can be seen as second order evolution equations in t. However, the physical interpretation of t is very different from the interpretation of the variable with the same name in the non-relativistic theory. While non-relativistic time is the observable quantity measured (or approximated) by physical clocks, in general relativity clocks measure s along their worldline, not t. The relativistic coordinate t is a freely chosen label with no direct physical interpretation. This is a well known consequence of the invariance of the Einstein equations under general changes of coordinates. The physical content of a solution of Einstein's equations is not in its dependence on t, but rather in what remains once the dependence on t (and x) has been factored away. What is then the physical content of a solution of Einstein's equations, and how is evolution described in this context? To answer, consider what is actually measured in general relativistic experiments. Here are some typical examples: Two clo cks. Consider a clock at rest on the surface of the Earth and a clock on a satellite in orbit around the Earth. Call T1 and T2 the readings of the two clocks. Each measures the proper time along its own worldline, in the Earth gravitational field. The two readings can be taken repeatedly (say at each passage of the satellite over n n the location of the Earth clock.) Let (T1 , T2 ), (T1 , T2 ), ..., (T1 , T2 ), ... be the sequence of readings. This can be compared with the theory. More precisely, given a solution of the Einstein eqs (for gravitational field, Earth and satellite), the theory predicts the value of T2 that will be associated to each value of T1 . Or vice versa. Solar system. The distances between the Earth and the other planets of the solar system can be measured with great accuracy today (for instance by the proper time on Earth between the emission of a laser pulse and the reception of its echo from the planet.) Call dp the distance from the planet p, measure these distances repeatedly, and write a table of quantities dp , dp , dp , ...dn , .... Then we can ask if these fit a sequence predicted by the theory. p Again, given a solution of Einstein's equations, the theory predicts which n-tuplets (dp ) are possible. Binary pulsar. A binary pulsar is a system of two stars rotating around each other, where one of the two is a pulsar, namely a star that sends a regular pulsating beep. The frequency at which we receive the beeps is modulated by the Doppler effect: it is higher when the pulsar is in the phase of the revolution where it moves towards us. Therefore we receive a pulsating signal with frequency increasing and decreasing periodically. Let n be the number of pulses we receive and N the number of periods. We can plot the two against each other and describe the increase of N as a function of n (or vice versa).2 The moral of these examples is that in general What we measure are a number of variables, particularly enlightening: notice that it can b variable T2 , or viceversa. Which of the two is relativistic observations there is no preferred independent time variable. all on equal footing, and their relative evolution. The first example is e equally read it as the evolution of the variable T1 as a function of the the independent variable here?3

2 3

By doing so for 10 years for the bin of revolution of this system, which Just in case the reader is tempted only one in free fall is the orbiting

ary pulsar PSR 1913+16, R Hulse and J Taylor have b een able to measure the decrease of the p erio d is indirect evidence for gravitational waves emission, and have won the 1993 Nobel Prize in Physics. to take the clo ck on Earth as a "more natural" definition of time, recall that of the two clo cks the one.


3 The way evolution is treated in general relativity, is therefore more subtle than in pre-relativistic theory. Change is not described as evolution of physical variables as a function of a preferred independent observable time variable. Instead, it is described in terms of a functional relation among equal footing variables (such as the two clock readings (T1 , T2 ) or the various planet distances dp , or the two observed quantities n and N of the binary pulsar system). In general relativity, there isn't a preferred and observable quantity that plays the role of independent parameter of the evolution, as there is in non-relativistic mechanics. General relativity describes the relative evolution of observable quantities, not the evolution of quantities as functions of a preferred one. To put it pictorially: with general relativity we have understood that the Newtonian "big clock" ticking away the "true universal time" is not there. I think that this feature of general relativity must be taken seriously in view of the problems raised by the attempts to write a quantum theory in gravity. In the classical theory, the 4-dimensional spacetime continuum continues to give us a good intuition of a flowing time. But in the quantum theory the 4-dimensional continuum is most likely not anymore there (although some aspect of this could remain [15]), and notions such as "the quantum state of the system at time t" are quite unnatural in a general relativistic context. I think we can get a far more effective grasp on the system if we forget notions such as "evolution in the observable time t" or "the state of the system at time t", we take the absence of a preferred independent time notion seriously, and we re-think mechanics as a theory of relative evolution of variables, rather than a theory of the evolution of variables in time. In section IV below I show how this can be done. Before that, however, allow me to go back to non-relativistic mechanics for a moment.

A.

Back to Galileo and Newton

Clockmaking owes a lot to Galileo Galilei, who discovered that the small oscillations of a pendulum are isochronous. The story goes that Galileo was in the cathedral of Pisa during a religious function, watching a big chandelier oscillating. Using his own pulse as a clock, Galileo discovered that there was the same number of pulses within each oscillation of the chandelier. Sometime later, pendulum clocks become widespread, and doctors started using them to check the pulse of the ill. What is going on here? The oscillations of a pendulum are measured against pulse, and pulse is measured again the pendulum! How do we know that a clock measures time, if we can only check it against another clock? Isaac Newton provides a nice clarification of this issue in the Principia. According to Newton, we never directly measure the true time variable t. Rather, we always construct devises, the "clocks" indeed, that have observable quantities (say, the angle between the clock's hand and the direction of the digit "12"), that move proportionally to the true time, within an approximation good enough for our purposes. In other words, we can say, following Newton, that what we can observe are the system's quantities ai and the clock's quantity , and their relative evolution, namely the functions ai ( ); but we describe this in our theory by assuming the existence of a "true" time variable t. We can then write evolution equations ai (t) and (t), and compare these with the observed change of ai with the clock's hand ai ( ). Thus, it is true also in non-relativistic mechanics that what we measure is only relative evolution between variables. But it turns out to be convenient to assume, with Newton, that there exist a background variable t, such that all observables quantities evolve with respect to it, and equations are simple when written with respect to it. What I propose to do in the following is simply to drop this assumption.

IV.

FORMAL STRUCTURE OF TIMELESS MECHANICS

In its conventional formulation, mechanics describes the evolution of states and observables in time. This evolution is governed by a Hamiltonian. (This is also true for special relativistic theories and field theories: evolution is governed by a representation of the Poincar´ group, and one of the generators of this group is the Hamiltonian.) e This conventional formulation is not sufficiently broad, because general relativistic systems ­in fact, the world in which we live­ do not fit in this conceptual scheme. Therefore we need a more general formulation of mechanics than the conventional one. This formulation must be based on notions of "observable" and "state" that maintain a clear meaning in a general relativistic context. I describe here how such a formulation can be defined.4

4

The formalism defined here is based on well known works. For instance, Arnold [16] identifies the (presymplectic) space with coordinates (t, q i , pi ) (time, lagrangian variables and their momenta) as the natural home for mechanics. Souriau has develop ed a b eautiful and little known relativistic formalism [17]. Probably the first to consider the p oint of view used here was Lagrange himself, in p ointing out that the most convenient definition of "phase space" is the space of the physical motions [18]. Many of the tools used below are also


4
A. The harmonic oscillator revisited

Say we want to describe the small oscillations of a pendulum. To this aim, we need two measuring devices. A clock and a device that reads the elongation of the pendulum. Let be the reading of the device measuring the elongation of the pendulum and be the reading of the clock (say the angle between the clock's hand and the "12".) Call the variables and the partial observables of the pendulum. A physically relevant observation is a reading of and , together. Thus, an observation yields a pair (, ). Call a pair obtained in this manner an event. Let C be the two-dimensional space with coordinates and . Call C the event space of the pendulum. Experience shows that we can find mathematical laws characterizing sequences of events. (This is the reason we can do science.) These laws have the following form. Call a unparametrized curve in C a motion of the system. Perform a sequence of measurements of pairs (, ), and find that the points representing the measured pairs sit on a motion . Then we say that is a physical motion . We express a motion as a relation in C f (, ) = 0. (1)

Thus a motion is a relation (or a correlation) between partial observables. Then, disturb the pendulum (push it with a finger) and repeat the entire experiment over. At each repetition of the experiment, a different motion is found. That is, a different mathematical relation of the form (1) is found. Experience shows that the space of the physical motions is very limited: it is just a two-dimensional subspace of the infinite dimensional space of all motions. Only a two-dimensional space of curves is realized in nature. In the case of the small oscillations of a frictionless pendulum, we can coordinatize the physical motions by the two real numbers A 0 and 0 < 2 , and (1) is given by f (, ; A, ) = - A sin( + ) = 0. (2)

This equation gives a curve in C for each couple (A, ). Equation (2) is the mathematical law that captures the entire empirical information we have on the dynamics of the pendulum. Let be the two-dimensional space of the physical motions, coordinatized by A and . is the relativistic phase space of the pendulum (or the space of the motions ). A point in , is a relativistic state. A relativistic state is determined by a couple (A, ). It determines a curve in the (, ) plane. That is, it determines a correlations between the two partial observables and , via (2).
B. General structure of the dynamical systems.

The (C , , f ) language described above is general. On the one hand, it is sufficient to describe all predictions of conventional mechanics. On the other hand, it is broad enough to describe general relativistic systems. All fundamental systems, including the general relativistic ones, can be described (to the accuracy at which quantum effects can be disregarded) by making use of these concepts: (i) The relativistic configuration space C , of the partial observables. (ii) The relativistic phase space of the relativistic states. (iii) The evolution equation f = 0, where f : â C V . V is a linear space. The state in the phase space is fixed until the system is disturbed. Each state in determines (via f = 0) a motion of the system, namely a relation, or a set of relations, between the observables in C .5 Once the state is determined (or guessed), the evolution equation predicts all the possible events, namely all the allowed correlations between the observables, in any subsequent measurement. Notice that this language makes no reference to a special "time" variable. The definitions of observable, state, configuration space and phase space given here are different from the conventional definition. In particular, notions of instantaneous state, evolution in time, observable at a fixed time, play no role here. These notions make no sense in a general relativistic context.

5

used in hamiltonian treatments of general covariant theories as constrained systems, on the basis of Dirac's theory, but generally within a rather obscure interpretative cloud, which I make an effort here to simplify and clarify. A motion is not necessarily a one-dimensional curve in C : it can b e a surface in C of any dimension k. If k > 1, we say that there is gauge invariance. Here I take k = 1. See [14] for the general case with gauge invariance.


5
C. Hamiltonian mechanics

It appears that all elementary physical systems can be described by hamiltonian mechanics.6 Once ­that is, the space C of the partial observables q a ­ is known, the dynamics ­that is, and f ­ is fully giving a surface in the space of the observables q a and their momenta pa . The surface can giving a function H : R. is then define d by H = 0.7 Denote a curve in (observables and ~ its restriction to C (observables alone). H determines the physical motions via the following

the kinematics determined by be specified by momenta) and

a a Variational principle. A curve connecting the events q1 and q2 is a physical motion if extremizes ~ a the action S [ ] = pa dq in the class of the curves satisfying H (q a , pa ) = 0whose restriction to C ~ ~ ~ a a connects q1 and q2 .

All known physical (relativistic and nonrelativistic) hamiltonian systems can be formulated in this manner. Notice that no notion of time has been used in this formulation. I call H the relativistic hamiltonian, or, if there is no ambiguity, simply the hamiltonian. I denote the pair (C , H ) as a relativistic dynamical system. A nonrelativistic system is a system where one of the partial observables, called t, is singled out as playing a special role. And the Hamiltonian has the particular structure H = pt + H0 (qi , pi , t) (3)

where pt is the momentum conjugate to t and (qi , pi ) are the other variables. This structure is not necessary in order to have a well-defined physical interpretation of the formalism. The relativistic hamiltonian H is related to, but should not be confused with, the usual nonrelativistic hamiltonian H0 . In the case of the pendulum, for instance, H has the form H = p + 12 m 2 2 p + . 2m 2 (4)

H always exists, while H0 exists only for the non-general-relativistic systems.
V. FORMAL STRUCTURE OF TIMELESS QUANTUM MECHANICS

A formulation of QM slightly more general than the conventional one ­ or a quantum version of the relativistic classical mechanics discussed above­ is needed to describe systems where no preferred time variable is specified. Here I sketch the possibility of such a formulation. For a detailed discussion of the issues raised by this formulation, see [14]. The quantum theory can be defined in terms of the following quantities. Kinematical states. Kinematical states form a space S in a rigged Hilbert space S K S . Partial observables. A partial observable is represented by a self-adjoint operator in K. Common eigenstates |s of a complete set of commuting partial observables are denoted quantum events. Dynamics. Dynamics is defined by a self-adjoint operator H in K, the (relativistic) hamiltonian. The operator from S to S P= d e-i
H

(5)

is (sometimes improperly) called the pro jector. (The integration range in this integral depends on the system.) Its matrix elements W (s, s ) = s|P |s are called transition amplitudes. (6)

6 7

Perhaps because they are the classical limit of a quantum system. Different H 's that vanish on the same surface define the same physical system.


6 Probability. Assume discrete spectrum for simplicity. The probability of the quantum event s given the quantum event s is Pss = |W (s, s )|2 where |s is normalized by s|P |s = 1. To this we may add: States. A physical state is a solution of the Wheeler-DeWitt equation H = 0. Equivalently, it is an element of the Hilbert space H defined by the quadratic form · |P | · on S . (8) (7)

Complete observables. A complete observable A is represented by a self-adjoint operator on H. A self-adjoint operator A in K defines a complete observable if [A, H ] = 0. (9)

Projection. If the observable A takes value in the spectral interval I , the state becomes then the state PI , where PI is the spectral pro jector on the interval I . If an event corresponding to a sufficiently small region R is detected, the state becomes |R . A relativistic quantum system is defined by a rigged Hilbert space of kinematical states K a nd a set of partial observables Ai including a relativistic hamiltonian operator H . Alternatively, it is defined by giving the pro jector P . The structure defined above is still tentative and perhaps incomplete. There are aspects of this structure that deserve to be better understood, clarified, and specified. Among these is the correct treatment of repeated measurements. On the other hand, the conventional structure of QM is certainly physically incomplete, in the light of GR. The above is an attempt to complete it, making it general relativistic.

A.

Quantization and classical limit

If we are given a classical system defined by a non relativistic configuration space C with coordinates q a and by a relativistic hamiltonian H (q a , pa ), a solution of the quantization problem is provided by the multiplicative operators q a , the derivative operators pa = -i¯ a and the Hamiltonian operator H = H q a , -i¯ a on the Hilbert space hq hq K = L2 [C , dq a ], or more precisely, the Gelfand triple determined by C and the measure dq a . The physics is entirely contained in the transition amplitudes W (q a , q a ) = q a |P |q
a

(10)

where the states |q a are the eigenstates of the multiplicative operators q a . In the limit h 0 the Wheeler-DeWitt ¯ equation becomes the relativistic Hamilton-Jacobi equation ([14]). An example of relativistic formalism is provided by the quantization of the pendulum described in the previous section: The kinematical state space is K = L2 [R2 , d d ]. The partial observable operators are the multiplicative operators and acting on the functions (, ) in K. Dynamics is defined by the operator H given in (4). The Wheeler-DeWitt equation becomes the Schrodinger equation. H is the space of solutions of this equation. The ¨ "pro jector" operator P : K H defined by H defines the scalar product in H. Its matrix elements W (, t, , t ) between the common eigenstates of and t are given by the oscillator's propagator. They express all predictions of the theory. Because of the specific form of H , these define a probability density in but not in .8 This example is of course trivial, since the system admits also a conventional hamiltonian quantization. But the point here is that the formalism above remains viable also for general relativistic systems that do not admit a conventional hamiltonian quantization, because they do not have a preferred time variable.

8

For more details, see [14]. For a related approach, see [22], [23].


7
VI. RECOVERY OF TIME

If we formulate the fundamental theory of nature in a timeless language, we have then the problem of recovering the familiar notion of time. There are two aspects of this problem. The first aspect is simply to see if the general theory admits a regime or an approximation where the Hamiltonian can be approximated by an Hamiltonian of the form (3) for some partial observable t. If this is the case, the system is described within this regime and this approximation precisely as a standard nonrelativistic system, and we can therefore identify t with the nonrelativistic time. The second aspect is far more subtle. The time of our experience is associated with a number of peculiar features that make it a very special physical variable. Intuitively (and imprecisely) speaking, time "flows", we can never "go back in time", we remember the past but not the future, and so on. Where do all these very peculiar features of the time variable come from? I think that these features are not mechanical. Rather they emerge at the thermodynamical level. More precisely, these are all features that emerge when we give an approximate statistical description of a system with a large number of degrees of freedom. We represent our incomplete knowledge and assumptions in terms of a statistical state . The state can be represented as a normalized positive function on the relativistic phase space :


R+ ,

(11) (12)

ds (s) = 1.

(s) represents the assumed probability density of the state s in . Then the expectation value of any observable A : R in the state is [A] =


ds A(s) (s).

(13)

The fundamental postulate of statistical mechanics is that a system left free to thermalize reaches a time independent equilibrium state that can be represented by means of the Gibbs statistical state 0 (s) = N e-
H0 (s)

.

(14)

where = 1/T is a constant ­the inverse temperature­ and H0 is the nonrelativistic hamiltonian. Classical thermodynamics follows from this postulate. Time evolution is determined by At (s) = A(t(s)) where s(t) is the hamiltonian flow of H0 on . The correlation probability between At and B is W
AB

(t) = 0 [t (A)B ] =


ds A(s(t)) B (s) e-

H0 (s)

.

(15)

I have argued that mechanics does not single out a preferred variable, because all mechanical predictions can be obtained using the relativistic hamiltonian H , which treats all variables on equal footing. Is this true also for statistical mechanics? Eqs (12-13) are meaningful also in the relativistic context, where is the space of the solutions of the equations of motion. But this is not true for (14) and (15). These depend on the nonrelativistic hamiltonian. They single out t as a special variable. With purely mechanical measurement we cannot recognize the time variable. With statistical or thermal measurements, we can. In principle, we can figure out H0 simply by repeated microscopic measurements on copies of the system, without any need of observing time evolution. Indeed, if we find out the distribution of microstates 0 , then, up to an irrelevant additive constant we have H0 = - 1 ln 0 . (16)

Therefore, in a statistical context we have in principle an operational procedure for determining which one is the time variable: Measure 0 ; compute H0 from (16); compute the hamiltonian flow s(t) of H0 on : the time variable t is the parameter of this flow. The multiplicative constant in front of H0 just sets the unit in which time is measured. Up to this unit, we can find out which one is the time variable just by measuring 0 . This is in contrast with the purely mechanical context, where no operational procedure for singling out the time variable is available. Now, consider a truly relativistic system where no partial observable is singled out as the time variable. We find that the statistical state describing the system is given by a certain arbitrary 9 state . Define the quantity H = - ln . (17)

9

For the (17) to make sense, assume that nowhere vanishes on .


8 Let s(t ) be the hamiltonian flow of H . Call t "thermal time". Call "thermal clock" any measuring devise whose reading grows linearly with this flow. Given an observable A, consider the one-parameter family of observables At defined by At (s) = A(t (s)). Then it follows that the correlation probability between the observables At and B is W
AB

(t ) =


ds A(t (s))B (s)e-H

(s)

.

(18)

Notice that there is no difference between the physics described by (14-15) and the one described by (17-18). Whatever the statistical state is, there exists always a variable t , measured by the thermal clock, with respect to which the system is in equilibrium and physics is the same as in the conventional nonrelativistic statistical case ! This observation leads us to the following hypothesis. The thermal time hypothesis. In nature, there is no preferred physical time variable t. There are no equilibrium states 0 preferred a priori. Rather, all variables are equivalent; we can find the system in an arbitrary state ; if the system is in a state , then a preferred variable is singled out by the state of the system. This variable is what we call time. In other words, it is the statistical state that determines which variable is physical time, and not any a priori hypothetical "flow" that drives the system to a preferred statistical state. When we say that a certain variable is "the time", we are not making a statement concerning the fundamental mechanical structure of reality. Rather, we are making a statement about the statistical distribution we use to describe the macroscopic properties of the system that we describe macroscopically. The "thermal time hypothesis" is the idea that what we call "time" is the thermal time of the statistical state in which the world happens to be, when described in terms of the macroscopic parameters we have chosen. Time is, that is to say, the expression of our ignorance of the full microstate.10 The thermal time hypothesis works surprisingly well in a number of cases. For example, if we start from radiation filled covariant cosmological model, with no preferred time variable and write a statistical state representing the cosmological background radiation, then the thermal time of this state turns out to be precisely the Friedmann time [20]. Furthermore, this hypothesis extends in a very natural way to the quantum context, and even more naturally to the quantum field theoretical context, where it leads also to a general abstract state-independent notion of time flow. In QM, the time flow is given by At = t (A) = eitH0 Ae-itH0 . (19)

A statistical state is described by a density matrix . It determines the expectation values of any observable A via [A] = T r[A]. (20)

This equation defines a positive functional on the observables' algebra. The relation between a quantum Gibbs state 0 and H0 is the same as in equation (14). That is Correlation probabilities can be written as W
AB 0

= N e-

H0

.

(21)

(t) = [t (A)B ] = T r[eitH0 Ae-itH0 B e-

H0

],

(22)

Notice that it follows immediately from the definition that 0 [t (A)B ] = 0 [( Namely W
AB -t-i )

(B )A],

(23)

(t) = W

BA

(-t - i )

(24)

A state 0 over an algebra, satisfying the relation (23) is said to be K M S with respect to the flow t .

10

It seems to me that the general p oint of view I am adopting here might b e compatible with the p ersp ectival one presented by Jenann Ismael in [25] and, recently, in [26].


9 We can now generalize the thermal time hypothesis. Given a generic state the thermal hamiltonian is defined by H = - ln and the thermal time flow is defined by At = t (A) = eit
H

(25) Ae-it
H

.

(26)

is a KMS state with respect to the thermal time flow it defines. In QFT, finite temperature states do not live in the same Hilbert space as the zero temperature states. H0 is a divergent operator on these states. Therefore equation (21) make no sense. But Gibbs states can still be characterized by (23): a Gibbs state 0 over an algebra of observables is a KMS state with respect to the time flow (t). A celebrated theorem by Tomita states precisely that given any11 state over a von Neumann algebra12 , there is always a flow t , called the Tomita flow of , such that (23) holds. This theorem allows us to extend (17) to QFT: the thermal time flow t is defined in general as the Tomita flow of the statistical state . Thus the thermal times hypothesis can be readily extended to QFT. What we call the flow of "time" is the Tomita flow of the statistical state in which the world happens to be, when described in terms of the macroscopic parameters we have chosen.13
VI I. CONCLUSION

I have presented a certain number of ideas and results: 1. It is possible to formulate classical mechanics in a way in which the time variable is treated on equal footings with the other physical variables, and not singled out as the special independent variable. I have argued that this is the natural formalism for describing general relativistic systems. 2. It is possible to formulate quantum mechanics in the same manner. I think that this may be the effective formalism for quantum gravity. 3. The peculiar properties of the time variable are of thermodynamical origin, and can be captured by the thermal time hypothesis. Within quantum field theory, "time" is the Tomita flow of the statistical state in which the world happens to be, when described in terms of the macroscopic parameters we have chosen 4. In order to build a quantum theory of gravity the most effective strategy is therefore to forget the notion of time all together, and to define a quantum theory capable of predicting the possible correlations between partial observables. Before concluding, I must add that the views expressed are far from being entirely original. I have largely drawn from the ideas of numerous scientists, and in particular Bryce DeWitt, John Wheeler, Chris Isham, Abhay Ashtekar, Jorge Pullin, Rodolfo Gambini, Don Marolf, Don Page, Bianca Dittrich, Julian Barbour and Karel Kuchar, William Wootters, Jean-Marie Souriau, Lee Smolin, John Baez, Jonathan Halliwell, Jim Hartle, Alain Connes, and certainly others that I forget here. I have here attempted to combine a coherent view about the problem of time in quantum gravity, starting from what others have understood. On the other hand, I also see well that the view I present here is far from being uncontroversial. Several authors maintain the idea that the notion of time is irreducible, and cannot be eliminated from fundamental physics. See for instance [24]. I could of course be wrong, but my own expectation is that the notion of time is extremely natural to us, but only in the same manner in which other intuitive ideas are rooted in our intuition because they are features of the small garden in which we are accustomed to living (for instance: absolute simultaneity, absolute velocity, or the idea of a flat Earth and an absolute up and down). Intuition is not a good guide for understanding natural regimes so distant from our daily experience. The best guide is provided by the theories of the world that have proven empirically effective, and therefore summarize the knowledge we have about Nature. In particular, general relativity challenges strongly our intuitive notion of a universal flow of time. I think we must take its lesson seriously.

11 12 13

Any separating state . A separating density matrix has no zero eigenvalues. This is the QFT equivalent of the condition stated in the footnote 9. The observable algebra is in general a C algebra. We obtain a von Neumann algebra by closing in the Hilb ert norm of the quantum state space. A von Neumann algebra p osses also a more abstract notion of time flow, indep endent from . This is given by the one-parameter group of outer automorphisms, formed by the equivalence classes of of automorphisms under inner (unitary) automorphisms. Alain Connes has shown that this group is indep endent from . It only dep ends on the algebra itself. Connes has stressed the fact that this group provides an abstract notion of time flow that depends only on the algebraic structure of the observables, and nothing else.


10
APPENDIX A: GEOMETRIC FORMALISM.

The timeless mechanical formalism can be expressed in a beautiful and compact manner using the geometric form. The variables (q a , pa ) are coordinates on the cotangent space = T C . Equation H = 0 defines a surface in this space. The cotangent space carries the natural one-form ~ = pa dq a . ~ Denote the restriction of to the surface . The two-form = d on is integral surfaces of these null directions are the orbits of on . Each such surface in C . These surfaces are the motions. has dimension 2n - 1, the kernel of is, generically, one-dimensional, dimensional. Let , be a motion on and X a vector tangent to the motion. ~ (X ) = 0. (A1) degenerate: it has null directions. The orbit pro jects from T C to C to give a and the motions are, generically, oneThen (A2)

To find the motions, we have just t o integrate this equation. Equation (A2) is the equation of motion. X is defined by the homogeneous equation (A2) only up to a multiplicative factor. Therefore the tangent of the orbit is defined only up to a multiplicative factor, and therefore the parametrization of the the orbit is not determined by equation (A2): what matters is only the relation that the orbits establish between the different variables.

[1] [2] [3] [4] [5] [6] [7] [8] [9] [10]

[11] [12] [13] [14] [15] [16] [17] [18] [19] [20] [21] [22] [23]

[24] [25] [26]

A Ashtekar, "Gravity and the quantum", New J Phys. 7 (2005) 198. C Rovelli, "Time in quantum gravity: an hypothesis", Phys Rev D43 (1991) 442. C Rovelli, "Quantum mechanics without time: a model", Phys Rev D42 (1991) 2638. C Rovelli, "Quantum evolving constants", Phys Rev D44 (1991) 1339. C Rovelli, "What is observable in classical and quantum gravity?", Class and Quantum Grav 8 (1991) 297. C Rovelli, "Quantum reference systems", Class and Quantum Grav 8 (1991) 317. C Rovelli, "Is there incompatibility between the ways time is treated in general relativity and in standard quantum mechanics?", in Conceptual Problems of Quantum Gravity, A Ashtekar, J Stachel eds (Birkhauser, New York, 1991). C Rovelli, "Analysis of the different meaning of the concept of time in different physical theories", Il Nuovo Cimento 110B (1995) 81. C Rovelli, "Partial observables", Phy Rev D65 (2002) 124013; gr-qc/0110035. C Rovelli, "A note on the foundation of relativistic mechanics. I: Relativistic observables and relativistic states", to appear in the proceedings of the 15th SIGRAV Conference on General Relativity and Gravitational Physics, Rome, September 2002, gr-qc/0111037. C Rovelli, "A note on the foundation of relativistic mechanics. II: Covariant hamiltonian general relativity", gr-qc/0202079. C Rovelli, "Covariant Hamiltonian Formalism for Field Theory: Symplectic Structure and Hamilton-Jacobi Equation on the Space G", to appear on the proceedings of the conference DICE 2002, Piombino, September 2002. gr-qc/0207043. M Reisenberger, C Rovelli, "Spacetime states and covariant quantum theory", Phys Rev D65 (2002) 124013; gr-qc/0111016. D Marolf, C Rovelli, "Relativistic quantum measurement", Phys Rev D66 (2002) 023510; gr-qc/0203056. C Rovelli, Quantum Gravity (Cambridge University Press, 2004.) JC Baez, "Spin foam models," Class Quant Grav 15 (1998) 1827. VI Arnold, Matemati ceskie metody klassi ceskoj mechaniki (Moscow, Mir, 1979). See in particular Chapter IX, Section C. JM Souriau, Structure des systemes dynamics (Paris, Dunod, 1969) JL Lagrange, "M´ oires de la premi` classe des sciences mathematiques et physiques" (Paris, Institute de France, 1808) em ere C Rovelli, "Statistical mechanics of gravity and thermodynamical origin of time", Class Quantum Grav 10 (1993) 1549. C Rovelli, "The statistical state of the universe", Class and Quantum Grav 10 (1993) 1567. A Connes, C Rovelli, "Von Neumann algebra automorphisms and time versus thermodynamics relation in general covariant quantum theories", Class and Quantum Grav 11 (1994) 2899. J Hartle, "Spacetime quantum mechanics and the quantum mechanics of spacetime" in Proceedings on the 1992 Les Houches School, Gravitation and Quantisation, B Julia, J Zinn-Justin, eds, pg 285 (Elsevier Science, Paris 1995). J Halliwell, "The Wheeler-deWitt equation and the path integral in minisuperspace quantum cosmology", in Conceptual problems of quantum gravity, A Ashtekar, J Stachel eds (Birkhauser, New York, 1991); "The Interpretation of Quantum Cosmology and the Problem of Time", to appear in Proceedings of Stephen Hawking's 60th Birthday Conference, grqc/0208018. L Smolin, "The present moment in quantum cosmology: Challenges to the arguments for the elimination of time," arXiv:grqc/0104097. J Ismael, "The Situated Self" (Oxford University Press, 2006). J Ismael, "Temporal Experience", in Oxford Handbook on Time, to appear.