Abstract
Current attempts to probe general relativistic effects in quantum mechanics focus on precision measurements of phase shifts in matter–wave interferometry. Yet, phase shifts can always be explained as arising because of an Aharonov–Bohm effect, where a particle in a flat space–time is subject to an effective potential. Here we propose a quantum effect that cannot be explained without the general relativistic notion of proper time. We consider interference of a 'clock'—a particle with evolving internal degrees of freedom—that will not only display a phase shift, but also reduce the visibility of the interference pattern. According to general relativity, proper time flows at different rates in different regions of space–time. Therefore, because of quantum complementarity, the visibility will drop to the extent to which the path information becomes available from reading out the proper time from the 'clock'. Such a gravitationally induced decoherence would provide the first test of the genuine general relativistic notion of proper time in quantum mechanics.
Introduction
In the theory of general relativity, time is not a global background parameter but flows at different rates depending on the space–time geometry. Although verified to high precision in various experiments^{1}, this prediction (as well as any other general relativistic effect) has never been tested in the regime where quantum effects become relevant. There is, in general, a fundamental interest in probing the interplay between gravity and quantum mechanics^{2}. The reason is that the two theories are grounded on seemingly different premises and, although consistent predictions can be extrapolated for a large range of phenomena, a unified framework is still missing and fundamentally new physics is expected to appear at some scale.
One of the promising experimental directions is to reveal, through interferometric measurements, the phase acquired by a particle moving in a gravitational potential^{3,4}. Typically considered is a Mach–Zehnder type interferometer (Fig. 1), placed in the Earth's gravitational field, where a particle travels in a coherent superposition along the two interferometric paths γ_{1}, γ_{2} that have different proper lengths. The two amplitudes in the superposition acquire different, trajectorydependent phases Φ_{i}, i=1, 2. In addition, the particle acquires a controllable relative phase shift ϕ. Taking into account the action of the first beam splitter and denoting by r_{i}〉 the mode associated with the respective path γ_{i}, the state inside the Mach–Zehnder setup Ψ_{MZ}〉, just before it is recombined, can be written as
Finally, the particle can be registered by one of the two detectors D_{±} with corresponding probabilities P_{±}:
where ΔΦ:=Φ_{1}−Φ_{2}. The phase Φ_{i} is proportional to the action along the corresponding (semiclassical) trajectory γ_{i} on which the particle moves. For a free particle on an arbitrary space–time background, the action can be written in terms of the proper time τ that elapsed during the travel, This might suggest that the measurement of ΔΦ is an experimental demonstration of the general relativistic time dilation.
There is, however, a conceptual issue in interpreting experiments measuring a gravitationally induced phase shift as tests of the relativistic time dilation. The action S_{i} above can be written in terms of an effective gravitational potential on a flat space–time. Thus, all the effects resulting from such an action are fully described by the Schödinger equation with the corresponding gravitational potential and where the time evolution is given with respect to the global time. Note that a particle in a field of arbitrary nature is subject to a Hamiltonian where the potential energy is proportional to the field's charge and a positiondependent potential. Therefore, even in a homogeneous field, the particle acquires a trajectorydependent phase although the force acting on it is the same at any point—the phase arises only because of the potential. For a homogeneous electric field, this relative phase is known as the electric Aharonov–Bohm effect^{5}. The case of Newtonian gravity is directly analogous—the role of the particle's electric charge and of the Coulomb potential are taken by the particle's mass and the Newtonian gravitational potential, respectively^{6}. All quantum interferometric experiments performed to date (see for example, refs 7,8,9) are fully explainable by this gravitational analogue of the electric Aharonov–Bohm effect. Moreover, even if one includes nonNewtonian terms in the Hamiltonian, this dichotomy of interpretations is still present. Again, one can interpret the phase shift ΔΦ as a type of an Aharanov–Bohm phase, which a particle moving in a flat space–time acquires because of an effective, nonNewtonian, gravitational potential (at least for an effective gravitational potential arising from the typically considered Kerr or Schwarzschild space–times).
Here we predict a quantum effect that cannot be explained without the general relativistic notion of proper time and thus show how it is possible to unambiguously distinguish between the two interpretations discussed above. We consider a Mach–Zehnder interferometer placed in the gravitational potential and with a 'clock' used as an interfering particle. By 'clock' we mean some evolving internal degree of freedom of the particle. If there is a difference in proper time elapsed along the two trajectories, the 'clock' will evolve into different quantum states for the two paths of the interferometer. Because of quantum complementarity between interference and whichpath information the interferometric visibility will decrease by an amount given by the whichway information accessible from the final state of the clock^{10,11,12}. Such a reduction in the visibility is a direct consequence of the general relativistic time dilation, which follows from the Einstein equivalence principle. Seeing the Einstein equivalence principle as a corner stone of general relativity, observation of the predicted loss of the interference contrast would be the first confirmation of a genuine general relativistic effect in quantum mechanics.
One might sustain the view that the interference observed with particles without evolving degrees of freedom is a manifestation of some intrinsic oscillations associated with the particle and that such oscillations can still be seen as the ticking of a clock that keeps track of the particle's time. If any operational meaning was to be attributed to this clock, it would imply that whichway information is, in principle, accessible. One should then either assume that proper time is a quantum degree of freedom, in which case, there should be a drop in the interferometric visibility, or that the quantum complementarity relation (between whichpath information and interferometric visibility) would be violated when general relativistic effects become relevant. Our proposed experiment allows to test these possibilities. The hypothesis that proper time is a degree of freedom has indeed been considered in various works^{13,14,15}.
The above considerations are also relevant in the context of the debate over ref. 16 (determination of the gravitational redshift by reinterpreting interferometric experiment^{9} that measured the acceleration of free fall). It was pointed out in refs 17,18,19,20 that only states nontrivially evolving in time can be referred to as 'clocks'. In ref. 18, the interference in such a case was discussed, however, the role of the interferometric visibility as a witness of proper time in quantum mechanics and as a tool to test new hypotheses has not been previously considered.
In the present paper, we discuss an interferometric experiment in the gravitational field where the interfering particle can be operationally treated as a 'clock'. We predict that as a result of the quantum complementarity between interference and whichpath information the general relativistic time dilation will cause the decrease in the interferometric visibility. The observation of such a reduction in the visibility would be the first confirmation of a genuinely general relativistic effect in quantum mechanics, in particular, it would unambiguously probe proper time as predicted by general relativity. The proposed experiment can also lead to a conclusive test of theories in which proper time is treated as a quantum degree of freedom.
Results
Whichway information from proper time
Consider an interferometric experiment with the setup as in Fig. 1, but in a situation where the particle in superposition has some internal degree of freedom that can evolve in time. In such a case, state (1) is no longer the full description of the system. Moreover, if this degree of freedom can be considered as a 'clock', according to the general relativistic notion of proper time it should evolve differently along the two arms of the interferometer in the presence of gravity. For a trajectory γ_{i}, let us call τ_{i}〉 the corresponding state of the 'clock'. The superposition (1) inside the interferometer now reads
In general, the state (3) is entangled and according to quantum mechanics interference in the path degrees of freedom should correspondingly be washed away. The reason is that one could measure the 'clock' degrees of freedom and in that way read out the accessible whichpath information. Tracing out the 'clock' states in equation (3) gives the detection probabilities
where 〈τ_{1}τ_{2}〉=〈τ_{1}τ_{2}〉e^{iα}. When the ancillary phase shift ϕ is varied, the probabilities P_{±} oscillate with the amplitude , called the visibility (contrast) of the interference pattern. Formally
Whereas without the 'clock' the expected contrast is always maximal (equation (2) yields ), in the case of equation (4) it reads
The distinguishability of the trajectories is the probability to correctly guess which path was taken in the twoway interferometer by measuring the degrees of freedom that serve as a whichway detector^{12} (in mathematical terms it is the trace norm distance between the final states of the detectors associated with different paths). In our case, these are the 'clock' degrees of freedom and we obtain The amount of the whichway information that is potentially available sets an absolute upper bound on the fringe visibility and we recover the wellknown duality relation^{10,11,12} in the form as expected for pure states.
The above result demonstrates that general relativistic effects in quantum interferometric experiments can go beyond previously predicted corrections to the nonrelativistic phase shift. When proper time is treated operationally we anticipate the gravitational time dilation to result in the reduction of the fringe contrast. This drop in the visibility is expected independently of how the proper time is measured and which system and interaction are used for the 'clock'. Moreover, when the information about the time elapsed is not physically accessible, the drop in the visibility will not occur. This indicates that the effect unambiguously arises because of the proper time as predicted by general relativity, in contrast to measurements of the phase shift alone. The gravitational phase shift occurs independently of whether the system can or cannot be operationally treated as a 'clock', just as the phase shift acquired by a system in the electromagnetic potential. Therefore, the notion of proper time is not probed in such experiments.
Massive quantum 'clock' in an external gravitational field
In the next paragraphs, we present how the above idea can be realized when the 'clock' degrees of freedom are implemented in internal states of a massive particle (neglecting the finitesize effects). Let be the Hamiltonian that describes the internal evolution. In the rest reference frame, the time coordinate corresponds to the proper time τ, and the evolution of the internal states is given by Changing coordinates to the laboratory frame, the evolution is given by where describes how fast the proper time flows with respect to the coordinate time. For a general metric g_{μν}, it is given by where we use the signature (−+++) and summation over repeated indices is understood. The energy–momentum tensor of a massive particle described by the action S can be defined as the functional derivative of S with respect to the metric, that is, (see, for example, ref. 21). Since the particle's energy E is defined as the T_{00} component, it reads E=g_{0 μ}g_{0ν}T^{μν}. In the case of a free evolution in a space–time with a stationary metric (in coordinates such that g_{0j}=0 for j=1, 2, 3), we have
where m is the mass of the particle. Space–time geometry in the vicinity of Earth can be described by the Schwarzschild metric. In isotropic coordinates (x, θ, ν) and with it takes the form^{21}
where is the Earth's gravitational potential (G denotes the gravitational constant and M is the mass of Earth). We consider the limit of a weak field and of slowly moving particles. In the final result, we therefore keep up to quadratic terms in the kinetic and potential energy. In this approximation, the metric components read^{21}
so that
The total Hamiltonian in the laboratory frame is given by where the operator H_{0} describes the dynamics of the external degrees of freedom of the particle and is obtained by canonically quantizing the energy (6), that is, the particle's coordinate x and kinematic momentum p = mẋ become operators satisfying the canonical commutation relation Thus, approximating up to the second order also in the internal energy, H_{Lab} reads
where
and
We consider a semiclassical approximation of the particle's motion in the interferometer. Therefore, all terms in H_{Lab}, apart from the internal Hamiltonian , appear as purely numerical functions defined along the fixed trajectories.
In a setup as in Figure 1, the particle follows in superposition two fixed nongeodesic paths γ_{1}, γ_{2} in the homogeneous gravitational field. The acceleration and deceleration, which the particle undergoes in the x direction, is assumed to be the same for both trajectories, as well as the constant velocity along the y axis. This assures that the trajectories have different proper length, but there will be no time dilation between the paths stemming from special relativistic effects. The particle inside the interferometer will thus be described by the superposition where the states Ψ_{i}〉 associated with the two paths γ_{i} are given by applying the Hamiltonian (7) to the initial state, which we denote by x^{in}〉τ^{in}〉. Up to an overall phase, these states read
For a small size of the interferometer, the central gravitational potential φ(x) can be approximated to linear terms in the distance Δh between the paths:
where denotes the value of the Earth's gravitational acceleration in the origin of the laboratory frame, which is at distance R from the centre of Earth.
For a particle having two internal states 0〉, 1〉 with corresponding energies E_{0}, E_{1}, the rest frame Hamiltonian of the internal degrees of freedom can be written as
and if we choose the initial state of this internal degrees to be
the detection probabilities read
where ΔT is the time (as measured in the laboratory frame) for which the particle travels in the interferometer in a superposition of two trajectories at constant heights, ΔV:=gΔh is the difference in the gravitational potential between the paths, represents the corrections from equation (7) averaged over the two trajectories and ΔE:=E_{1}−E_{0}. The expectation value is taken with respect to the state (11). The corresponding visibility (5) is
The introduction of the 'clock' degrees of freedom results in two new quantum effects that cannot be explained without including general relativity: the change of the interferometric visibility and the extra phase shift proportional to the average internal energy (Fig. 2; equation (12)). The drop in the visibility is a consequence of a direct coupling of the particle's internal degrees of freedom to the potential in the effective Hamiltonian (7). Such a coupling is never found in Newtonian gravity, and it is the mathematical expression of the prediction that the 'clock' ticks at different rates when placed in different gravitational potentials. This coupling can directly be obtained from the Einstein equivalence principle. Recall that the latter postulates that accelerated reference frames are physically equivalent to those in the gravitational field of massive objects. When applied within special relativity, this exactly results in the prediction that initially synchronized clocks subject to different gravitational potentials will show different times when brought together. The proposed experiment probes the presence of such a gravitational time dilation effect for a quantum system—it directly shows whether the 'clock' would tick at different rates when taken along the two possible trajectories in the interferometer. On the other hand, to obtain the correct phase shift, it is sufficient to consider a semiclassical coupling of the average total energy of the system to the gravitational potential. With such a coupling, the time displayed by the 'clock' used in the experiment will not depend on the path taken. This means that a gravitationally induced phase shift can probe general relativistic corrections to the Newtonian gravitational potential but is always consistent with having an operationally welldefined notion of global time, that is, with a flat space–time.
The effect described in our work follows directly from the Einstein equivalence principle, which is itself crucial for the formulation of general relativity as a metric theory^{22}. Thus, the drop in the fringe contrast is not only genuinely quantum mechanical but also a genuine general relativistic effect that in particular unambiguously probes the general relativistic notion of proper time.
General 'clocks' and gravitational fields
Let us call t_{⊥} the orthogonalization time of a quantum system, that is, the minimal time needed for a quantum state to evolve under a given Hamiltonian into an orthogonal one^{23,24}. For the initial state (11) subject to the rest frame Hamiltonian given by equation (10) we obtain
A system with finite t_{⊥} can be seen as a clock that ticks at a rate proportional to t_{⊥}^{−1}. Thus, the orthogonalization time gives also the precision of a considered 'clock'. From the expression for in the approximation (9), it follows that the total time dilation Δτ between the trajectories is
We can, therefore, phrase the interferometric visibility solely in terms of t_{⊥} and Δτ:
The total time dilation Δτ is a parameter capturing the relevant information about the paths, and t_{⊥} grasps pertinent features of the 'clock'. It is, only their ratio that matters for the fringe visibility. Equation (16) is a generalization of the result (13) to the case of an arbitrary initial state, 'clock' Hamiltonian and a nonhomogeneous gravitational field: whenever the time dilation Δτ between the two trajectories through the Mach–Zehnder interferometer is equal to the orthogonalization time t_{⊥} of the quantum mechanical system that is sent through the setup, the physically accessible proper time difference will result in the full loss of fringe contrast. There are several bounds on the orthogonalization time based on energy distribution moments^{23,25,26}. Such bounds can through equation (16) give some estimates on the gravityinduced decoherence rates in more general situations. As an example, for mixed states one generally has^{26}:
α>0 (provided the initial state is in the domain of (H−E_{gr})^{α}) where H denotes the internal Hamiltonian and E_{gr} the energy of its ground state.
Discussion
Current approaches to test general relativistic effects in quantum mechanics mainly focus on high precision measurements of the phase induced by the gravitational potential. Although such experiments would probe the potential and thus could verify nonNewtonian corrections in the Hamiltonian, they would not constitute an unambiguous proof of the gravitational time dilation, because they are also explainable without this concept by the Aharonov–Bohm effect: a trajectorydependent phase acquired by a particle moving in a flat space–time in the presence of a positiondependent potential.
In our proposed experiment, the effects arising from general relativistic proper time can be separated and probed independently from the Aharonov–Bohm type of effects. Unlike the phase shift, which occurs independently of whether the interfering particle can be treated as a 'clock', the change of the interferometric visibility (equation (13)) is a quantum effect that arises if and only if general relativistic proper time has a well defined operational meaning. Indeed, if one prepares the initial state τ^{in}〉 as an eigenstate of the internal energy Hamiltonian only the phase of such a state would change during the time evolution and, according to equation (16), interferometric visibility would be maximal. This 'clock' would not 'tick' (it has orthogonalization time t_{⊥}=∞) so the concept of proper time would have no operational meaning in this case. Moreover, reasoning that any (even just an abstract) frequency which can be ascribed to the particle allows considering proper time as a physical quantity would imply that interference should always be lost, as the whichpath information is stored 'somewhere'. This once again shows that, in quantum mechanics, it makes no sense to speak about quantities without specifying how they are measured.
The interferometric experiment proposed in this work can also be used to test whether proper time is a new quantum degree of freedom. This idea was discussed in the context of, for example, the equivalence principle in refs 13,14 and a mass–proper time uncertainty relation^{15}. The equations of motion for proper time treated dynamically, as put forward in refs 13,14,15, are in agreement with general relativity. Therefore, the predictions of equation (5) would also be valid, if the states τ_{i}〉, introduced in equation (3), stand for this new degree of freedom. Already performed experiments, like in refs 7,16, which measured a gravitational phase shift, immediately rule out the possibility that the state of proper time was sharply defined in those tests, in the sense of 〈τ_{1}τ_{2}〉=δ(τ1−τ_{2}). However, such experiments can put a finite bound on the possible uncertainty in the state of proper time. The phase shift measured in those experiments can be phrased in terms of the difference in the proper time Δτ between the paths. Denote by the experimental error with which the visibility of the interference pattern was measured in those tests. As a result, a Gaussian state of the proper time degree of freedom of width σ_{τ} such that is consistent with the experimental data. An estimate of the proper time uncertainty can be based on the Heisenberg uncertainty principle for canonical variables and the equation of motion for the proper time. In such an analysis, the rest mass m can be considered as a canonically conjugated momentum to the proper time variable τ, that is, one assumes ^{13,14,15}. In Table 1, we discuss what can be inferred about proper time as a quantum degree of freedom from an experiment in which the measured visibility would be and where is the visibility predicted by quantum mechanics, as given by equation (13).
In conclusion, we predicted a quantum effect in interferometric experiments that, for the first time, allows probing general relativistic proper time in an unambiguous way. In the presence of a gravitational potential, we showed that a loss in the interferometric visibility occurs, if the time dilation is physically accessible from the state of the interfered particle. This requires that the particle is a 'clock' measuring proper time along the trajectories, therefore revealing the whichway information. Our predictions can be experimentally verified by implementing the 'clock' in some internal degrees of freedom of the particle (see Methods). The proposed experiment can also lead to a conclusive test of theories in which proper time is treated as a quantum degree of freedom. As a final remark, we note that decoherence due to the gravitational time dilation may have further importance in considering the quantum to classical transition and in attempts to observe collective quantum phenomena in extended, complex quantum systems because the orthogonalization time may become small enough in such situations to make the predicted decoherence effect prominent.
Methods
Systems for the implementation of the interferometric setup
Here we briefly discuss various systems for the possible implementation of the interferometric setup. Interferometry with many different massive quantum systems has been achieved, for example, with neutrons^{7,8}, atoms^{16,27}, electrons^{28,29} and molecules^{30,31}. In our framework, further access to an internal degree of freedom is paramount, as to initialize the 'clock' which measures the proper time along the interferometric path. Therefore, the experimental requirements are more challenging. To observe full loss of the interferometric visibility, the proper time difference in the two interferometric arms needs to be Δτ=t_{⊥}. For a two level system, the revival of the visibility due to the indistinguishability of the proper time in the two arms occurs when Δτ=2t_{⊥}.
The best current atomic clocks operate at optical frequencies ω around 10^{15} Hz. For such systems, we have , and one would therefore require an atomic superposition with ΔhΔT∼10 ms to see full disappearance of the interferometric visibility. For example, the spatial separation would need to be of the order of 1 m, maintained for about 10 s. Achieving and maintaining such large superpositions of atoms still remains a challenge, but recent rapid experimental progress indicates that this interferometric setup could be conceivable in the near future. For neutrons, a separation of Δh∼10^{−2} m with a coherence time of t∼10^{−4} s has been achieved^{8}. To implement our 'clock' in neutron interferometry, one can use spin precession in a strong, homogeneous magnetic field. However, such a 'clock' could reach frequencies up to ω∼10^{9} Hz (for a magnetic field strength of order of 10T (ref. 32)), which is still a few orders of magnitude lower than necessary for the observation of full decoherence owing to a proper time difference. Improvements in the coherence time and the size of the interferometer would still be necessary. Other systems, such as molecules, could be used as well and Table 2 summarizes the requirements for various setups (note again that the particles are assumed to travel at fixed height during the time ΔT).
The effect we predict can be measured even without achieving full orthogonalization of the 'clocks'. Note that even for Δτ<t_{⊥} the small reduction of visibility can already be sufficient to prove the accessibility of whichpath information due to the proper time difference. With current parameters in atom interferometry, an accuracy of the measurement of the visibility of would have to be achieved for the experimental confirmation of our predictions. A very good precision measurement of the interferometric visibility and a precise knowledge about other decoherence effects would therefore make the requirements for the other parameters less stringent.
Additional information
How to cite this article: Zych, M. et al. Quantum interferometric visibility as a witness of general relativistic proper time. Nat. Commun. 2:505 doi: 10.1038/ncomms1498 (2011).
References
Hafele, J. C. & Keating, R. E. Aroundtheworld atomic clocks: predicted relativistic time gains. Science 177, 166–168 (1972).
Chiao, R. Y., Minter, S. J., WegterMcNelly, K. & Martinez, L. A. Quantum incompressibility of a falling Rydberg atom, and a gravitationallyinduced charge separation effect in superconducting systems. Found. Phys. 1–19, DOI: 10.1007/s1070101095312 (2011).
Wajima, S., Kasai, M. & Futamase, T. PostNewtonian effects of gravity on quantum interferometry. Phys. Rev. D 55, 1964–1970 (1997).
Dimopoulos, S., Graham, P. W., Hogan, J. M. & Kasevich, M. A. General relativistic effects in atom interferometry. Phys. Rev. D 78, 042003 (2008).
Aharonov, Y. & Bohm, D. Significance of electromagnetic potentials in the quantum theory. Phys. Rev. 115, 485–491 (1959).
Ho, V. B. & Morgan, M. J. An experiment to test the gravitational AharonovBohm effect. Aust. J. Phys. 47, 245–253 (1994).
Colella, R., Overhauser, A. W. & Werner, S. A. Observation of gravitationally induced quantum interference. Phys. Rev. Lett. 34, 1472–1474 (1975).
Zawisky, M., Baron, M., Loidl, R. & Rauch, H. Testing the world's largest monolithic perfect crystal neutron interferometer. Nucl. Instrum. Methods Phys. Res. A 481, 406–413 (2002).
Peters, A., Chung, K. Y. & Chu, S. Measurement of gravitational acceleration by dropping atoms. Nature 400, 849–852 (1999).
Wootters, W. K. & Zurek, W. H. Complementarity in the doubleslit experiment: Quantum nonseparability and a quantitative statement of Bohr's principle. Phys. Rev. D 19, 473–484 (1979).
Greenberger, D. M. & Yasin, A. Simultaneous wave and particle knowledge in a neutron interferometer. Phys. Lett. A 128, 391–394 (1988).
Englert, B. G. Fringe visibility and whichway information: An inequality. Phys. Rev. Lett. 77, 2154–2157 (1996).
Greenberger, D. M. Theory of particles with variable mass. I. Formalism. J. Math. Phys. 11, 2329 (1970).
Greenberger, D. M. Theory of particles with variable mass. II. Some physical consequences. J. Math. Phys. 11, 2341 (1970).
Kudaka, S. & Matsumoto, S. Uncertainty principle for proper time and mass. J. Math. Phys. 40, 1237 (1999).
Müller, H., Peters, A. & Chu, S. A precision measurement of the gravitational redshift by the interference of matter waves. Nature 463, 926–929 (2010).
Wolf, P. et al. Atom gravimeters and gravitational redshift. Nature 467, E1 (2010).
Sinha, S. & Samuel, J. Atom interferometers and the gravitational redshift. Class. Quantum Grav. 28, 145018 (2011).
Giulini, D. Equivalence principle, quantum mechanics, and atominterferometric tests. arXiv:1105.0749v1 (2011).
Wolf, P. et al. Does an atom interferometer test the gravitational redshift at the Compton frequency? Class. Quantum Grav. 28, 145017 (2011).
Weinberg, S. Gravitation and Cosmology, (John Wiley & Sons, 1972).
Will, C. M. Theory and Experiment in Gravitational Physics, (Cambridge University Press, 1993).
Mandelstam, L. & Tamm, I. The uncertainty relation between energy and time in nonrelativistic quantum mechanics. Journ. Phys. (USSR) 9, 249 (1945).
Fleming, G. N. A unitarity bound on the evolution of nonstationary states. Nuovo Cim. A 16, 232–240 (1973).
Margolus, N. & Levitin, L. B. The maximum speed of dynamical evolution. Physica D 120, 188–195 (1998).
Zielinski, B. & Zych, M. Generalization of the MargolusLevitin bound. Phys. Rev. A 74, 034301 (2006).
Müller, H., Chiow, S., Herrmann, S. & Chu, S. Atom interferometers with scalable enclosed area. Phys. Rev. Lett. 102, 240403 (2009).
Neder, I., Heiblum, M., Mahalu, D. & Umansky, V. Entanglement, dephasing, and phase recovery via crosscorrelation measurements of electrons. Phys. Rev. Lett. 98, 036803 (2007).
Ji, Y. et al. An electronic MachZehnder interferometer. Nature 422, 415–418 (2003).
Arndt, M. et al. Waveparticle duality of C 60 molecules. Nature 401, 680–682 (1999).
Gerlich, S. et al. Quantum interference of large organic molecules. Nat. Commun. 2:263 doi: 10.1038/ncomms1263 (2011).
Miller, J. R. The NHMFL 45T hybrid magnet system: past, present, and future. IEEE Trans. Appl. Supercond. 13, 1385–1390 (2003).
Acknowledgements
We thank M. Arndt, B. Dakic, S. Gerlich, D. M. Greenberger, H. Müller, S. Nimmrichter, A. Peters, and P. Wolf for insightful discussions. The research was funded by the Austrian Science Fund (FWF) projects: W1210, P19570N16 and SFBFOQUS, the Foundational Questions Institute (FQXi) and the European Commission Project QESSENCE (No. 248095). F.C., I.P. and M.Z. are members of the FWF Doctoral Program CoQuS.
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M.Z., F.C., I.P. and Č.B. contributed to all aspects of the research with the leading input from M.Z.
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Zych, M., Costa, F., Pikovski, I. et al. Quantum interferometric visibility as a witness of general relativistic proper time. Nat Commun 2, 505 (2011). https://doi.org/10.1038/ncomms1498
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DOI: https://doi.org/10.1038/ncomms1498
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