Английская Википедия:Imaginary time

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Шаблон:Short description Imaginary time is a mathematical representation of time that appears in some approaches to special relativity and quantum mechanics. It finds uses in connecting quantum mechanics with statistical mechanics and in certain cosmological theories.Шаблон:Cn

Mathematically, imaginary time is real time which has undergone a Wick rotation so that its coordinates are multiplied by the imaginary unit i. Imaginary time is not imaginary in the sense that it is unreal or made-up (any more than, say, irrational numbers defy logic), it is simply expressed in terms of imaginary numbers.

Origins

In mathematics, the imaginary unit <math>i</math> is the square root of <math>-1</math>, such that <math>i^2</math> is defined to be <math>-1</math>. A number which is a direct multiple of <math>i</math> is known as an imaginary number.Шаблон:Rp

In certain physical theories, periods of time are multiplied by <math>i</math> in this way. Mathematically, an imaginary time period <math display="inline">\tau</math> may be obtained from real time <math display="inline"> t</math> via a Wick rotation by <math display="inline">\pi/2</math> in the complex plane: <math display="inline">\tau = it</math>.Шаблон:Rp

Stephen Hawking popularized the concept of imaginary time in his book The Universe in a Nutshell. Шаблон:Quote

In fact, the terms "real" and "imaginary" for numbers are just a historical accident, much like the terms "rational" and "irrational": Шаблон:Quote

In cosmology

Derivation

In the Minkowski spacetime model adopted by the theory of relativity, spacetime is represented as a four-dimensional surface or manifold. Its four-dimensional equivalent of a distance in three-dimensional space is called an interval. Assuming that a specific time period is represented as a real number in the same way as a distance in space, an interval <math>d</math> in relativistic spacetime is given by the usual formula but with time negated: <math display="block">d^2 = x^2 + y^2 + z^2 - t^2</math> where <math>x</math>, <math>y</math> and <math>z</math> are distances along each spatial axis and <math>t</math> is a period of time or "distance" along the time axis (Strictly, the time coordinate is <math>(ct)^2</math> where <math>c</math> is the speed of light, however we conventionally choose units such that <math>c=1</math>).

Mathematically this is equivalent to writing <math display="block">d^2 = x^2 + y^2 + z^2 + (it)^2</math>

In this context, <math>i</math> may be either accepted as a feature of the relationship between space and real time, as above, or it may alternatively be incorporated into time itself, such that the value of time is itself an imaginary number, denoted by <math>\tau</math>.Шаблон:Cn The equation may then be rewritten in normalised form: <math display="block">d^2 = x^2 + y^2 + z^2 + \tau^2</math>

Similarly its four vector may then be written as <math display="block">( x_0, x_1, x_2, x_3 )</math> where distances are represented as <math>x_n</math>, and <math>x_0 = ict</math> where <math>c</math> is the speed of light and time is imaginary.

Application to cosmology

Hawking noted the utility of rotating time intervals into an imaginary metric in certain situations, in 1971.

In physical cosmology, imaginary time may be incorporated into certain models of the universe which are solutions to the equations of general relativity. In particular, imaginary time can help to smooth out gravitational singularities, where known physical laws break down, to remove the singularity and avoid such breakdowns (see Hartle–Hawking state). The Big Bang, for example, appears as a singularity in ordinary time but, when modelled with imaginary time, the singularity can be removed and the Big Bang functions like any other point in four-dimensional spacetime. Any boundary to spacetime is a form of singularity, where the smooth nature of spacetime breaks down.Шаблон:Rp With all such singularities removed from the Universe, it thus can have no boundary and Stephen Hawking speculated that "the boundary condition to the Universe is that it has no boundary".Шаблон:Rp

However, the unproven nature of the relationship between actual physical time and imaginary time incorporated into such models has raised criticisms. Roger Penrose has noted that there needs to be a transition from the Riemannian metric (often referred to as "Euclidean" in this context) with imaginary time at the Big Bang to a Lorentzian metric with real time for the evolving Universe. Also, modern observations suggest that the Universe is open and will never shrink back to a Big Crunch. If this proves true, then the end-of-time boundary still remains.Шаблон:Rp

In quantum statistical mechanics

The equations of the quantum field can be obtained by taking the Fourier transform of the equations of statistical mechanics. Since the Fourier transform of a function typically shows up as its inverse, the point particles of statistical mechanics become, under a Fourier transform, the infinitely extended harmonic oscillators of quantum field theory. The Green's function of an inhomogeneous linear differential operator, defined on a domain with specified initial conditions or boundary conditions, is its impulse response, and mathematically we define the point particles of statistical mechanics as Dirac delta functions, which is to say impulses. At a finite temperature <math>T</math>, the Green's functions are periodic in imaginary time with a period of <math display="inline"> 2\beta = 2/T</math>. Therefore, their Fourier transforms contain only a discrete set of frequencies called Matsubara frequencies.

The connection between statistical mechanics and quantum field theory is also seen in the transition amplitude <math display="inline">\langle F\mid e^{-itH}\mid I\rangle </math> between an initial state Шаблон:Math and a final state Шаблон:Math, where Шаблон:Math is the Hamiltonian of that system. Comparing this with the partition function <math display="inline"> Z = \operatorname{Tr} e^{-\beta H}</math> shows that the partition function may be derived from the transition amplitudes by substituting <math display="inline"> t = \beta/i</math>, setting Шаблон:Math and summing over Шаблон:Math. This avoids the need to do twice the work by evaluating both the statistical properties and the transition amplitudes.

Finally, by using a Wick rotation one can show that the Euclidean quantum field theory in (D + 1)-dimensional spacetime is nothing but quantum statistical mechanics in D-dimensional space.

See also

• Euclidean quantum gravity
• Multiple time dimensions

Further reading

• Шаблон:Cite book
• Gerald D. Mahan. Many-Particle Physics, Chapter 3
• A. Zee Quantum field theory in a nutshell, Chapter V.2

External links

• The Beginning of Time — Lecture by Stephen Hawking which discusses imaginary time.
• Stephen Hawking's Universe: Strange Stuff Explained Шаблон:Webarchive — PBS site on imaginary time.