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Proper time

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Elapsed time between two events as measured by a clock that passes through both events

Inrelativity,proper time (from the Latinproprius, meaningown) along atimelike world line is defined as thetime as measured by aclock following that line. Theproper time interval between twoevents on a world line is the change in proper time, which is independent of coordinates, and is aLorentz scalar.^[1] The interval is the quantity of interest, since proper time itself is fixed only up to an arbitrary additive constant, namely the setting of the clock at some event along the world line.

The proper time interval between two events depends not only on the events, but also the world line connecting them, and hence on the motion of the clock between the events. It is expressed as an integral over the world line (analogous toarc length inEuclidean space). An accelerated clock will measure a smaller elapsed time between two events than that measured by a non-accelerated (inertial) clock between the same two events. Thetwin paradox is an example of this effect.^[2]

The dark blue vertical line represents an inertial observer measuring a coordinate time intervalt between eventsE₁ andE₂. The red curve represents a clock measuring its proper time intervalτ between the same two events.

By convention, proper time is usually represented by the Greek letterτ (tau) to distinguish it fromcoordinate time represented byt. Coordinate time is the time between two events as measured by an observer using that observer's own method of assigning a time to an event. In the special case of an inertial observer inspecial relativity, the time is measured using the observer's clock and the observer's definition of simultaneity.

The concept of proper time was introduced byHermann Minkowski in 1908,^[3] and is an important feature ofMinkowski diagrams.

Mathematical formalism

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The formal definition of proper time involves describing the path throughspacetime that represents a clock, observer, or test particle, and themetric structure of that spacetime. Proper time is thepseudo-Riemannian arc length ofworld lines in four-dimensional spacetime. From the mathematical point of view, coordinate time is assumed to be predefined and an expression for proper time as a function of coordinate time is required. On the other hand, proper time is measured experimentally and coordinate time is calculated from the proper time of inertial clocks.

Proper time can only be defined for timelike paths through spacetime which allow for the construction of an accompanying set of physical rulers and clocks. The same formalism for spacelike paths leads to a measurement ofproper distance rather than proper time. For lightlike paths, there exists no concept of proper time and it is undefined as the spacetime interval is zero. Instead, an arbitrary and physically irrelevantaffine parameter unrelated to time must be introduced.^[4]^[5]^[6]^[7]^[8]^[9]

In special relativity

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With thetimelike convention for themetric signature, theMinkowski metric is defined by $\eta _{\mu \nu }={\begin{pmatrix}1&0&0&0\\0&-1&0&0\\0&0&-1&0\\0&0&0&-1\end{pmatrix}},$ and the coordinates by $(x^{0},x^{1},x^{2},x^{3})=(ct,x,y,z)$ for arbitrary Lorentz frames.

In any such frame an infinitesimal interval, here assumed timelike, between two events is expressed as

ds^{2}=c^{2}dt^{2}-dx^{2}-dy^{2}-dz^{2}=\eta _{\mu \nu }dx^{\mu }dx^{\nu },

(1)

and separates points on a trajectory of a particle (think clock{?}). The same interval can be expressed in coordinates such that at each moment, the particle isat rest. Such a frame is called an instantaneous rest frame, denoted here by the coordinates $(c\tau ,x_{\tau },y_{\tau },z_{\tau })$ for each instant. Due to the invariance of the interval (instantaneous rest frames taken at different times are related by Lorentz transformations) one may write $ds^{2}=c^{2}d\tau ^{2}-dx_{\tau }^{2}-dy_{\tau }^{2}-dz_{\tau }^{2}=c^{2}d\tau ^{2},$ since in the instantaneous rest frame, the particle or the frame itself is at rest, i.e., $dx_{\tau }=dy_{\tau }=dz_{\tau }=0$ . Since the interval is assumed timelike (ie. $ds^{2}>0$ ), taking the square root of the above yields^[10] $ds=cd\tau ,$ or $d\tau ={\frac {ds}{c}}.$ Given this differential expression forτ, the proper time interval is defined as

$\Delta \tau =\int _{P}d\tau =\int _{P}{\frac {ds}{c}}.$ (2)

HereP is the worldline from some initial event to some final event with the ordering of the events fixed by the requirement that the final event occurs later according to the clock than the initial event.

Using(1) and again the invariance of the interval, one may write^[11]

${\begin{aligned}\Delta \tau &=\int _{P}{\frac {1}{c}}{\sqrt {\eta _{\mu \nu }dx^{\mu }dx^{\nu }}}\\&=\int _{P}{\sqrt {dt^{2}-{dx^{2} \over c^{2}}-{dy^{2} \over c^{2}}-{dz^{2} \over c^{2}}}}\\&=\int _{a}^{b}{\sqrt {1-{\frac {1}{c^{2}}}\left[\left({\frac {dx}{dt}}\right)^{2}+\left({\frac {dy}{dt}}\right)^{2}+\left({\frac {dz}{dt}}\right)^{2}\right]}}dt\\&=\int _{a}^{b}{\sqrt {1-{\frac {v(t)^{2}}{c^{2}}}}}dt\\&=\int _{a}^{b}{\frac {dt}{\gamma (t)}},\end{aligned}}$ (3)

where $(x^{0},x^{1},x^{2},x^{3}):[a,b]\rightarrow P$ is an arbitrary bijective parametrization of the worldlinePsuch that $(x^{0}(a),x^{1}(a),x^{2}(a),x^{3}(a))\quad {\text{and}}\quad (x^{0}(b),x^{1}(b),x^{2}(b),x^{3}(b))$ give the endpoints ofP and a < b;v(t) is the coordinate speed at coordinate timet; andx(t),y(t), andz(t) are space coordinates. The first expression ismanifestly Lorentz invariant. They are all Lorentz invariant, since proper time and proper time intervals are coordinate-independent by definition.

Ift,x,y,z, are parameterised by aparameterλ, this can be written as $\Delta \tau =\int {\sqrt {\left({\frac {dt}{d\lambda }}\right)^{2}-{\frac {1}{c^{2}}}\left[\left({\frac {dx}{d\lambda }}\right)^{2}+\left({\frac {dy}{d\lambda }}\right)^{2}+\left({\frac {dz}{d\lambda }}\right)^{2}\right]}}\,d\lambda .$

If the motion of the particle is constant, the expression simplifies to $\Delta \tau ={\sqrt {\left(\Delta t\right)^{2}-{\frac {\left(\Delta x\right)^{2}}{c^{2}}}-{\frac {\left(\Delta y\right)^{2}}{c^{2}}}-{\frac {\left(\Delta z\right)^{2}}{c^{2}}}}},$ where Δ means the change in coordinates between the initial and final events. The definition in special relativity generalizes straightforwardly to general relativity as follows below.

In general relativity

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Proper time is defined ingeneral relativity as follows: Given apseudo-Riemannian manifold with a local coordinatesx^μ and equipped with ametric tensorg_μν, the proper time intervalΔτ between two events along a timelike pathP is given by theline integral^[12]

\Delta \tau =\int _{P}\,d\tau =\int _{P}{\frac {1}{c}}{\sqrt {g_{\mu \nu }\;dx^{\mu }\;dx^{\nu }}}.

(4)

This expression is, as it should be, invariant under coordinate changes. It reduces (in appropriate coordinates) to the expression of special relativity inflat spacetime.

In the same way that coordinates can be chosen such thatx¹,x²,x³ = const in special relativity, this can be done in general relativity too. Then, in these coordinates,^[13] $\Delta \tau =\int _{P}d\tau =\int _{P}{\frac {1}{c}}{\sqrt {g_{00}}}dx^{0}.$

This expression generalizes definition(2) and can be taken as the definition. Then using invariance of the interval, equation(4) follows from it in the same way(3) follows from(2), except that here arbitrary coordinate changes are allowed.

Examples in special relativity

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Example 1: The twin paradox

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For atwin paradox scenario, let there be an observerA who moves between theA-coordinates (0,0,0,0) and (10 years, 0, 0, 0) inertially. This means thatA stays at $x=y=z=0$ for 10 years ofA-coordinate time. The proper time interval forA between the two events is then $\Delta \tau _{A}={\sqrt {(10{\text{ years}})^{2}}}=10{\text{ years}}.$

So being "at rest" in a special relativity coordinate system means that proper time and coordinate time are the same.

Let there now be another observerB who travels in thex direction from (0,0,0,0) for 5 years ofA-coordinate time at 0.866c to (5 years, 4.33 light-years, 0, 0). Once there,B accelerates, and travels in the other spatial direction for another 5 years ofA-coordinate time to (10 years, 0, 0, 0). For each leg of the trip, the proper time interval can be calculated usingA-coordinates, and is given by $\Delta \tau _{leg}={\sqrt {({\text{5 years}})^{2}-({\text{4.33 years}})^{2}}}={\sqrt {6.25\;\mathrm {years} ^{2}}}={\text{2.5 years}}.$

So the total proper time for observerB to go from (0,0,0,0) to (5 years, 4.33 light-years, 0, 0) and then to (10 years, 0, 0, 0) is $\Delta \tau _{B}=2\Delta \tau _{leg}={\text{5 years}}.$

Thus it is shown that the proper time equation incorporates thetime dilation effect. In fact, for an object in a SR (special relativity) spacetime traveling with velocity $v {\displaystyle v}$ for a time $\Delta T$ , the proper time interval experienced is $\Delta \tau ={\sqrt {\Delta T^{2}-\left({\frac {v_{x}\Delta T}{c}}\right)^{2}-\left({\frac {v_{y}\Delta T}{c}}\right)^{2}-\left({\frac {v_{z}\Delta T}{c}}\right)^{2}}}=\Delta T{\sqrt {1-{\frac {v^{2}}{c^{2}}}}},$ which is the SR time dilation formula.

Example 2: The rotating disk

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An observer rotating around another inertial observer is in an accelerated frame of reference. For such an observer, the incremental ( $d\tau$ ) form of the proper time equation is needed, along with a parameterized description of the path being taken, as shown below.

Let there be an observerC on a disk rotating in thexy plane at a coordinate angular rate of $\omega$ and who is at a distance ofr from the center of the disk with the center of the disk atx =y =z = 0. The path of observerC is given by $(T,\,r\cos(\omega T),\,r\sin(\omega T),\,0)$ , where $T {\displaystyle T}$ is the current coordinate time. Whenr and $\omega$ are constant, $dx=-r\omega \sin(\omega T)\,dT$ and $dy=r\omega \cos(\omega T)\,dT$ . The incremental proper time formula then becomes $d\tau ={\sqrt {dT^{2}-\left({\frac {r\omega }{c}}\right)^{2}\sin ^{2}(\omega T)\;dT^{2}-\left({\frac {r\omega }{c}}\right)^{2}\cos ^{2}(\omega T)\;dT^{2}}}=dT{\sqrt {1-\left({\frac {r\omega }{c}}\right)^{2}}}.$

So for an observer rotating at a constant distance ofr from a given point in spacetime at a constant angular rate ofω between coordinate times $T_{1}$ and $T_{2}$ , the proper time experienced will be $\int _{T_{1}}^{T_{2}}d\tau =(T_{2}-T_{1}){\sqrt {1-\left({\frac {r\omega }{c}}\right)^{2}}}=\Delta T{\sqrt {1-v^{2}/c^{2}}},$ as $v=r\omega$ for a rotating observer. This result is the same as for the linear motion example, and shows the general application of the integral form of the proper time formula.

Examples in general relativity

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The difference between SR and general relativity (GR) is that in GR one can use any metric which is a solution of theEinstein field equations, not just the Minkowski metric. Because inertial motion in curved spacetimes lacks the simple expression it has in SR, the line integral form of the proper time equation must always be used.

Example 3: The rotating disk (again)

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An appropriatecoordinate conversion done against the Minkowski metric creates coordinates where an object on a rotating disk stays in the same spatial coordinate position. The new coordinates are $r={\sqrt {x^{2}+y^{2}}}$ and $\theta =\arctan \left({\frac {y}{x}}\right)-\omega t.$

Thet andz coordinates remain unchanged. In this new coordinate system, the incremental proper time equation is $d\tau ={\sqrt {\left[1-\left({\frac {r\omega }{c}}\right)^{2}\right]dt^{2}-{\frac {dr^{2}}{c^{2}}}-{\frac {r^{2}\,d\theta ^{2}}{c^{2}}}-{\frac {dz^{2}}{c^{2}}}-2{\frac {r^{2}\omega \,dt\,d\theta }{c^{2}}}}}.$

Withr,θ, andz being constant over time, this simplifies to $d\tau =dt{\sqrt {1-\left({\frac {r\omega }{c}}\right)^{2}}},$ which is the same as in Example 2.

Now let there be an object off of the rotating disk and at inertial rest with respect to the center of the disk and at a distance ofR from it. This object has acoordinate motion described bydθ = −ωdt, which describes the inertially at-rest object of counter-rotating in the view of the rotating observer. Now the proper time equation becomes $d\tau ={\sqrt {\left[1-\left({\frac {R\omega }{c}}\right)^{2}\right]dt^{2}-\left({\frac {R\omega }{c}}\right)^{2}\,dt^{2}+2\left({\frac {R\omega }{c}}\right)^{2}\,dt^{2}}}=dt.$

So for the inertial at-rest observer, coordinate time and proper time are once again found to pass at the same rate, as expected and required for the internal self-consistency of relativity theory.^[14]

Example 4: The Schwarzschild solution – time on the Earth

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TheSchwarzschild solution has an incremental proper time equation of $d\tau ={\sqrt {\left(1-{\frac {2m}{r}}\right)dt^{2}-{\frac {1}{c^{2}}}\left(1-{\frac {2m}{r}}\right)^{-1}dr^{2}-{\frac {r^{2}}{c^{2}}}d\phi ^{2}-{\frac {r^{2}}{c^{2}}}\sin ^{2}(\phi )\,d\theta ^{2}}},$ where

t is time as calibrated with a clock distant from and at inertial rest with respect to the Earth,
r is a radial coordinate (which is effectively the distance from the Earth's center),
ɸ is a co-latitudinal coordinate, the angular separation from theNorth Pole inradians.
θ is a longitudinal coordinate, analogous to the longitude on the Earth's surface but independent of the Earth'srotation. This is also given in radians.
m is thegeometrized mass of the Earth,m =GM/c²,
- M is the mass of the Earth,
- G is thegravitational constant.

To demonstrate the use of the proper time relationship, several sub-examples involving the Earth will be used here.

For theEarth,M =5.9742×10²⁴ kg, meaning thatm =4.4354×10⁻³ m. When standing on the North Pole, we can assume $dr=d\theta =d\phi =0$ (meaning that we are neither moving up or down or along the surface of the Earth). In this case, the Schwarzschild solution proper time equation becomes ${\textstyle d\tau =dt\,{\sqrt {1-2m/r}}}$ . Then using the polar radius of the Earth as the radial coordinate (or $r={\text{6,356,752 metres}}$ ), we find that $d\tau ={\sqrt {\left(1-1.3908\times 10^{-9}\right)\;dt^{2}}}=\left(1-6.9540\times 10^{-10}\right)\,dt.$

At theequator, the radius of the Earth isr =6378137 m. In addition, the rotation of the Earth needs to be taken into account. This imparts on an observer an angular velocity of $d\theta /dt$ of 2π divided by thesidereal period of the Earth's rotation, 86162.4 seconds. So $d\theta =7.2923\times 10^{-5}\,dt$ . The proper time equation then produces $d\tau ={\sqrt {\left(1-1.3908\times 10^{-9}\right)dt^{2}-2.4069\times 10^{-12}\,dt^{2}}}=\left(1-6.9660\times 10^{-10}\right)\,dt.$

From a non-relativistic point of view this should have been the same as the previous result. This example demonstrates how the proper time equation is used, even though the Earth rotates and hence is not spherically symmetric as assumed by the Schwarzschild solution. To describe the effects of rotation more accurately theKerr metric may be used.

Footnotes

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^Zwiebach 2004, p. 25
^Hawley, John F.; Holcomb, J Katherine A. (2005).Foundations of Modern Cosmology (illustrated ed.). Oxford University Press. p. 204.ISBN 978-0-19-853096-1.Extract of page 204
^Minkowski 1908, pp. 53–111
^Lovelock & Rund 1989, pp. 256
^Weinberg 1972, pp. 76
^Poisson 2004, pp. 7
^Landau & Lifshitz 1975, p. 245
^Some authors include lightlike intervals in the definition of proper time, and also include the spacelike proper distances as imaginary proper times e.gLawden 2012, pp. 17, 116
^Kopeikin, Efroimsky & Kaplan 2011, p. 275
^Zwiebach 2004, p. 25
^Foster & Nightingale 1978, p. 56
^Foster & Nightingale 1978, p. 57
^Landau & Lifshitz 1975, p. 251
^Cook 2004, pp. 214–219

References

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Cook, R. J. (2004)."Physical time and physical space in general relativity".Am. J. Phys.72 (2):214–219.Bibcode:2004AmJPh..72..214C.doi:10.1119/1.1607338.ISSN 0002-9505.
Foster, J.; Nightingale, J.D. (1978).A short course in general relativity. Essex:Longman Scientific and Technical.ISBN 0-582-44194-3.
Kleppner, D.; Kolenkow, R.J. (1978).An introduction to mechanics.McGraw–Hill.ISBN 0-07-035048-5.
Kopeikin, Sergei; Efroimsky, Michael; Kaplan, George (2011).Relativistic Celestial Mechanics of the Solar System. John Wiley & Sons.ISBN 978-3-527-40856-6.
Landau, L. D.;Lifshitz, E. M. (1975).The classical theory of fields. Course of theoretical physics. Vol. 2 (4th ed.). Oxford:Butterworth–Heinemann.ISBN 0-7506-2768-9.
Lawden, Derek F. (2012).An Introduction to Tensor Calculus: Relativity and Cosmology. Courier Corporation.ISBN 978-0-486-13214-3.
Lovelock, David;Rund, Hanno (1989),Tensors, Differential Forms, and Variational Principles, New York:Dover Publications,ISBN 0-486-65840-6
Minkowski, Hermann (1908),"Die Grundgleichungen für die elektromagnetischen Vorgänge in bewegten Körpern",Nachrichten von der Königlichen Gesellschaft der Wissenschaften und der Georg-August-Universität zu Göttingen, Göttingen, archived fromthe original on 2012-07-08
Poisson, Eric (2004),A Relativist's Toolkit: The Mathematics of Black-Hole Mechanics,Cambridge University Press,ISBN 978-0521537803
Weinberg, Steven (1972),Gravitation and Cosmology: Principles and Applications of the General Theory of Relativity, New York:John Wiley & Sons,ISBN 978-0-471-92567-5
Zwiebach, Barton (2004).A First Course in String Theory (first ed.).Cambridge University Press.ISBN 0-521-83143-1.

Time

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