## Abstract

With the planning of new ambitious gravitational wave observatories, fully controlled laboratory experiments on dynamic gravitation become more and more important. Such experiments can provide new insights in potential dynamic effects such as gravitational shielding or energy flow and might contribute to bringing light into the mystery still surrounding gravity. Here we present a laboratory-based transmitter-detector experiment using two rotating bars as transmitter and a 42 Hz, high-Q bending beam resonator as detector. Using a precise phase control to synchronize the rotating bars, a dynamic gravitational field emerges that excites the bending motion with amplitudes up to 100 nm/s or 370 pm, which is a factor of 500 above the thermal noise. The two-bar design enables the investigation of different transmitter configurations. The detector movement is measured optically, using three commercial interferometers. Acoustical, mechanical, and electrical isolation, a temperature-stable environment, and lock-in detection are central elements of the setup. The moving load response of the detector is numerically calculated based on Newton’s law of gravitation via discrete volume integration, showing excellent agreement between measurement and theory both in amplitude and phase. The near field gravitational energy transfer is 10^{25} times larger than the one of the propagating gravitational wave component.

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## Introduction

Gravitation is the weakest of the four fundamental forces in physics. As a result, gravitation experiments in earth-based laboratories are very difficult to perform, in particular when it comes to precision measurements. This is exemplified by the relatively large scatter in the measurement of the gravitational constant *G* by different research groups^{1}. All of the experiments referred to in ref. ^{1} investigate gravitational interaction in (quasi)static situations.

Due to this scatter, which is not yet fully understood, and with increasing research efforts in gravitational waves^{2}, alternative, laboratory-based *dynamical* gravitational experiments become more and more important. Such an experiment typically consists of a transmitter which gravitationally excites the vibration of a detector, giving the experimenter full control over cause and effect, as opposed to having to wait for a gravitational event to happen in outer space. Besides adding an alternative technique to precision *G* measurements, dynamic experiments offer the possibility to investigate a number of effects like the influence of transmitter/detector distance on the interaction strength^{3}, or a potential attenuation of the gravitational interaction by masses placed in between transmitter and detector^{4,5,6}, for which only limited experimental evidence is available. Also, the energy flow from transmitter to detector can be quantified, which cannot be done by quasi-static experiments. Further, the full understanding of the gravitational interaction and possible side effects can help to establish a well-understood gravitational signal generator for calibration of gravitational wave (GW) observatories.

However, dynamic laboratory experiments are very rare, in particular when it comes to a full quantitative comparison between theory and experiment. This is illustrated in Table 1 summarizing as an overview the basic features of the few dynamic gravitational experiments reported during the last 50 years. It becomes apparent that there is a need for a flexible experimental setup that can be used to study as many of the aspects of dynamic gravitational interaction as possible.

To fill this gap, we presented in a previous work the dynamical gravitational coupling between two parallel beams vibrating in their first bending resonance at 42 Hz^{7}. This setup allowed for a quantitative investigation of the decay of the gravitational field strength with increasing transmitter/detector distance and the estimation of the gravitational constant *G*. Although this setup allowed for important advances in dynamic gravitation measurements, it features some drawbacks, such as the need for matching transmitter and detector resonance frequency or the generation of very low detector amplitudes.

Therefore, motivated by the pioneering works of Astone^{8,9}, and the Hirakawa group^{10,11,12}, who used a rotating transmitter, we introduce here a setup that combines the experimental and analytical advantages of our initial setup with the benefits of a rotational excitation and its elaborated theory. As illustrated in Table 1, all recent works use one single transmitter. In contrast, here we use two slender, 0.5 m long tungsten bars arranged symmetrically to a bending beam resonant detector. This double transmitter arrangement allows to easily investigate various configurations of the excitation, that is, rotation direction, frequency or even electronically controlled variable phase of the position of the rotating bars, within the same experimental setup.

Previous dynamic experiments encountered a relatively large measurement uncertainty for the estimation of *G*. This was mainly caused by electrical or mechanical, non-gravitational crosstalk and the fact that the measurement accuracy reaches its limit with the resulting small displacement amplitudes. In the setup presented here, some of these issues can be addressed using a precisely defined rigid body transmitter movement and considerably larger detector amplitudes. These advantages, however, come at the expense of high requirements on the balancing of the rotors and their motion control, in particular their phase accuracy and phase jitter. To demonstrate the potential of this setup, we use the same detector beam as in ref. ^{7} and the same measurement procedure. Thus we obtain the detector resonance amplitude and phase at different distances, as well as an estimation of the gravitational constant *G*.

While the motion of the rotating bars is trivial to model, its interaction with the detector beam is categorized as a nonstandard moving load problem with varying speeds and shapes of the moving force pulse. Its solution is greatly simplified by the periodicity of the loading and the restriction to the steady state and can be obtained by the methods outlined in ref. ^{13}. Considering the length scales of the experiment, the detector is placed in the near-field of the transmitter. Since the excitation is not necessarily purely quadrupole, Newton’s law has been directly applied to all relevant mass elements. We compute the results using a highly accurate three-dimensional (3D) finite element model and a simplified one-dimensional (1D) model for comparison.

This article presents a theoretical and experimental description of the experiment and shows its feasibility and enormous potential as well as technical pitfalls, without providing highly accurate *G* measurements yet. We show that the double transmitter approach provides a large variation of dynamic gravitational fields, and that the setup is able to accurately measure the resulting detector movement in amplitude and phase.

## Results and discussion

### Theory of dynamic gravitational force fields generated by a rotating bar

The setup presented in this article consists of a transmitter and detector system, cf. Fig 1. The transmitter system is composed of two identical, slender bars of square cross-section that can rotate around the *z*-axis in their center of mass. The bars are arranged symmetrically to the middle of the detector beam at a distance *d*_{0}, that is, the *y*-distance between the central axis of the detector and the centers of rotation. The detector is designed as a resonator, with the first lateral bending mode to be the relevant vibration mode. We selected a slender beam of rectangular cross-section and twice the length of the transmitter bars. Due to the rectangular shape, it is ensured that horizontal and vertical bending do not have the same resonance frequency.

When the bars rotate, a dynamic gravitational force field develops due to the periodically changing distance between detector and transmitter mass elements. Hence, given that a suitable rotation frequency is selected, the dynamic gravitational force field periodically excites the first bending mode of the detector beam, which then develops a measurable deflection.

To investigate the force field acting on the detector, Newton’s law of gravitation is applied to each pair of transmitter/detector mass elements. The transmitter rotation is maintained at a constant frequency with very high accuracy using active rotation control, as detailed in the methods subsection on the rotational system. The much smaller gravitational forces acting on the transmitter bars do not affect the rotation. Newton’s law of gravitation yields a time dependent, three-dimensional gravitational body force on the detector generated by each bar. For a first analytical analysis of the gravitational effects a 1D approach is sought, where the body forces in *y*-direction are approximated by two line forces \({f}_{{{{{{{{\rm{y}}}}}}}}}^{(k)}({x}_{{{{{{{{\rm{d}}}}}}}}})\) acting on the central axis of the slender detector beam, where *x*_{d} denotes the *x* coordinate of the detector beam center line and *k* the number of the rotating bar, cf. Fig. 1. The detector’s bending movement can then be calculated using an Euler-Bernoulli beam model and a modal approach^{7,14}, in which the distributed force is reduced to the effective modal excitation force *F*_{y, b} of the first bending mode via

where *U*_{b,1} is the mode shape function of the first bending mode, normalized so that *U*_{b,1}(0) = 1.

To assess the frequency components of the excitation, a Fourier series is computed. Due to the nonlinear law of gravitation, higher harmonics must occur, which is illustrated by Fig. 2a, where the spectral components at multiples of the rotation frequency Ω are shown qualitatively (scaled to the DC value). It can be observed that the force field contains frequency components at even multiples of the rotation frequency only with decreasing contribution. Hence the excitation frequency Ω must be chosen 1/2 or 1/4 of the detector beam’s resonance frequency *ω*_{0} to achieve maximum detector excitation.

The use of higher harmonics as excitation and the possibility of different rotation arrangements (one/two bars, same/opposite direction, pos./neg. direction) enables different configurations that will be discussed briefly. While the motion of the rotating bars is trivial to model, its interaction with the detector beam is categorized as a nonstandard moving load problem with varying speeds and shapes of the moving force pulse. Its solution is greatly simplified by the periodicity of the loading and the restriction to the steady state and can be obtained by the methods outlined in ref. ^{13}. Considering one rotating bar only, the variation of the force distribution can be illustrated by a transverse pulse with varying speed and shape moving along the *x*-axis of the detector. Considering two bars rotating in opposite directions, the situation becomes symmetric and the net force in *x*-direction becomes zero. While the strength, that is, the amplitude of the force field, decreases with increasing transmitter/detector distance *d*_{0}, the behavior of the phase between transmitter rotation and detector vibration is less intuitive. Interpreting the phase as a measure for the angle of maximal excitation, it becomes obvious that such angle must not necessarily be at *φ*_{k} = 90^{∘} due to the mode shape of the first bending mode and that it will change with distance *d*_{0}.

When both bars rotate in the same direction, the maximum of the two force fields do not occur at the same time, therefore the force fields don’t superpose symmetrically, resulting in an approx. 8% smaller amplitude and a non-zero net force in *x*-direction. For the same reason, the angle of maximal excitation occurs exactly at *φ*_{k} = 90^{∘}, which eliminates the distance dependency of the phase. A phasor representation of the superposition of the modal forces is presented in Supp. Fig. 3.

Figure 2b,c show the result of an analytical calculation of *F*_{y, b} as a function of distance, illustrating the aforementioned effects. As it was expected from the spectrum in Fig. 2a, an excitation with Ω = *ω*_{0}/4 creates an amplitude of about 60% lower compared to Ω = *ω*_{0}/2.

To numerically assess the detector movement caused by the gravitational field, the modal force is applied as excitation force to the well-known equation of motion of a free-free Euler-Bernoulli beam. It is shown in ref. ^{7} that the complex detector bending velocity at resonance, *v*_{b,0} can be derived from the gravitational force between infinitesimal mass elements of transmitter and detector resulting in

where *G* is the gravitational constant, *Q*_{d} the Q factor of the detector beam and *ω*_{0} its first bending resonance frequency. Γ is a complex numerical coefficient which depends on the distance *d*_{0}, the detector beam and rotating bar’s dimensions and their relative position *x*_{0}, the rotating bar’s masses and mass distributions, the ratio *n* = *ω*_{0}/Ω, and the rotation configuration. It is calculated numerically for any given configuration. To avoid errors due to the 1D approximation, the calculation of Γ is based on a full 3D model (cf. method subsection “numerical model”), for which Eq. (2) holds as well.

The modulus of Γ can be approximated to follow a power law distance behavior \({{\Gamma }}\approx \gamma /{d}_{0}^{a}\). It has to be noted that the power law coefficient *a* considerably differs from the prediction *a* = 5 of the dynamic gravitational field around a rotating bar detected by a resonant antenna (quadrupole-quadrupole interaction)^{3,15}. The values of *a* for the setup, length scales, and configurations presented in this article are summarized in Table 2.

The gravitational constant *G* can be estimated from Eq. (2), using the measured detector amplitude *v*_{b,0}, the detector’s vibration properties (*Q*_{d}, *ω*_{0}), and the numerical coefficient Γ. Since this will result in a complex number, only the modulus is taken as estimation for *G*. The angle gives information about the phase difference between measurement and theory, cf. Supp. Fig. 2.

### Experiment design and measurement procedure

Figure 3a shows the experimental setup as it was already introduced and used in ref. ^{7}, now with the rotating bars located in the transmitter chamber. The transmitter bars are made of tungsten both with length of 499.86(1) mm and a quadratic cross section of 10.06(1) mm edge length, each driven by a 50W maxon EC-i 40 brushless motor to rotate with frequency Ω. The distance between the rotation centers is *x*_{0} = 800.0(3) mm. The bars’ mass has been measured equal to 970.8(1) g and 971.8(1) g, respectively. The detector is made of titanium with dimensions 1000.00(1) mm × 16.97(1) mm × 8.49(1) mm and a Q factor of *Q*_{d} = 44819(535) at a detector chamber pressure of about 0.03 mbar. The geometrical and mechanical parameters of transmitter and detectors are summarized in Supp. Table 1. The detector is hanging on two EPDM rubber strings glued to the beam at the nodal points of the first bending mode, which minimizes both external damping and force transmission, and enables the use of a free-free beam model. A mass of 7.1 g at the center of each rubber wire provides additional decoupling. The beam’s movement is measured optically using three Polytec OFV-5000/505 laser Doppler interferometers (LDV) placed on a separate, spring-suspended platform. The output signals of the laser interferometers are fed into individual digital lock-in amplifiers (Zurich Instruments MFLI) via a 12 dB attenuator. The lock-in amplifiers use eight cascaded low-pass filters with time constant of 31 s to extract the velocity amplitude and phase at the measurement frequency *ω*. The reference is provided by a high-precision signal generator (SRS FS740 with Rubidium time base, frequency error < 10 pHz, phase accuracy: delay < 1 ns). From the movement at three different positions one can distinguish between two rigid body motions (translation in *y* and rotation around *z*) and the lateral bending motion, assuming a known bending mode shape *U*_{b,1}.

Both detector and transmitter system have been placed in separate aluminum vacuum chambers to avoid acoustic coupling effects or any excitation other than gravitation. Using two separate Edwards nXDS 10i vacuum scroll pumps running continuously, the pressure inside the detector and transmitter chambers was kept constant at 0.027(3) mbar and 0.103(5) mbar, respectively. No disturbing influence of the vibrations produced by the pumps was identified. The chamber containing the detector was fixed to a vibration isolation table using an 80 mm thick aluminum base plate of 70 kg mass. The transmitter chamber is hanging on steel springs (Durovis 20/8/5) from a movable bar attached to a solid frame with high damping. This way, the distance *d*_{0} can be varied between 0.3 m and 0.6 m. Accelerometers mounted on both chambers give information about remaining movement of the chambers.

To investigate the gravitational coupling and to compare it with the numerical solution, the frequency response of the detector is measured around the first bending resonance *ω*_{0}. We use a 24-point frequency sweep with step times of 75 min to account for the large time constant of the detector beam (*τ* ≈ 5.5 min) and the lock-in amplifiers (99% settling time approx. 9 min). By averaging the last 16 min of each step, a signal-to-noise ratio (SNR) ratio of up to 500 can be achieved. After fitting the frequency response of a single-degree-of freedom (SDOF) oscillator^{7}, the following parameters are obtained: amplitude and phase at resonance, resonance frequency, the detector’s Q factor, and a complex offset constant.

The low bandwidth of the detector and the need for synchronization of both beams imposes extremely high requirements on the resolution and stability of the rotation frequencies. Since this cannot be realized using the motor’s built-in encoder, a custom rotation control and synchronization based on two light barriers (LB) have been implemented, cf. Fig. 3b,c. The rotation control provides a stable rotation with a RMS phase jitter < 0.03^{∘}. Details on the rotation control can be found in the corresponding methods subsection.

Due to the long-time measurement, it must be ensured that resonance frequency and Q factor of the detector beam remain stable during the measurement period. Therefore, the whole setup has been placed in an underground laboratory in the Swiss Alps where a very stable temperature can be guaranteed, resulting in an average temperature span of 0.004 ^{∘}C per measurement point (75 min). Remaining temperature variations have been subsequently compensated based on the linear temperature dependency of the frequency. Further details can be found in ref. ^{7}.

Despite rotating with a fraction of the measurement frequency *ω*, minimal unbalances of the bars, motor friction, material inhomogeneities etc. can generate small vibrations of the transmitter chamber with amplitudes up to 2 μms^{−1} (8 nm) at *ω*. These disturbances can propagate to the detector chamber most likely via acoustical transmission and structure borne sound. Therefore, as the decoupling of the detector is not perfect, unwanted, non-gravitationally induced detector vibrations can occur. Accelerometers mounted on both chambers reveal that the use of Ω = *ω*/2 and Ω = *ω*/4 produces detector chamber velocity amplitudes at the frequency of measurement of approx. 2 nms^{−1} and 0.5 nms^{−1}, respectively, cf. Supp. Fig. 1.

### Examination of gravitationally induced detector vibration

Over a period of two months, 28 measurement runs were conducted at different beam distances and rotation/frequency configurations. Each measurement corresponds to a 24-point frequency sweep of 36 h duration, where resonance amplitude and phase, as well as the resonance frequency and Q factor, have been extracted by fitting the frequency response function of a SDOF oscillator, cf. Supp. Fig. 4. To detect measurements that were affected by unstable conditions, the following quality criteria have been applied: Detector chamber pressure span < 0.01 mbar, detector chamber temperature span < 0. 1^{∘}C, SDOF fit coefficient of determination *R*^{2} > 99%.

The results of the measured complex bending velocity at resonance *v*_{b,0} are summarized in Fig. 4. Additionally, the results of the 3D simulation are displayed. Since the simulation uses a fixed detector Q factor and resonance frequency, the measured amplitudes are scaled to these values using the linear dependency of the velocity on *Q* and \({\omega }_{0}^{-1}\), cf. Eq. (2). As shown in the first row of Fig. 4 (panels a, b), the measured amplitudes match the numerical prediction very well for all configurations. Considering the uncertainty of the theoretical prediction that comprises statistical and systematic uncertainties as summarized in Table 3, the measured amplitudes mostly lie within the 95% tolerance band of the theory/simulation. In the second row of Fig. 4 (panels c, d) experimental and theoretical results of the phase of the detector vibration are depicted. Although producing potentially higher disturbances due to an increased movement of the transmitter assembly, measurements using the same rotation direction have been performed, since the phase for this configuration (yellow lines in Fig. 4) should be independent on the distance. Therefore, this phase can be used as reference to assess system phase delays or crosstalk. The experimental phase values show the predicted number range and trend, but do not match the theory exactly. Besides the measurement system that might introduce some uncertainties, mechanical crosstalk, which is more pronounced in the phase, is suspected to be the main reason for the observed deviation. A small movement of the detector chamber was measured, as shown in Supp. Fig. 1, where the average velocity amplitudes of both detector and transmitter chamber are displayed. However, the mechanism and magnitude of the force transmission from detector chamber to detector beam are not yet fully understood. Therefore, a rough estimate of a 1% contribution to the systematic uncertainties due to mechanical crosstalk has been added to the error budget.

Finally, *G* was estimated from each measurement result using Eq. (2) (modulus), where the detector’s Q factor has been incorporated individually for each measurement. In Fig. 5, the single results are depicted with standard deviation from statistical errors (colored patches). Combining the single measurements of *G* by means of inverse-variance weighting yields *G*^{*} = 6.6816 × 10^{−11} m^{3}kg^{−1}s^{−2} with a relative standard deviation of 0.02% based on statistical errors only (black dashed line in Fig. 5). The overall 95% confidence band (black dotted line in Fig. 5) represents the extended combined measurement uncertainty (k = 1.96) based on the statistical and systematic uncertainties as summarized in Table 3. From this, *G* is estimated with *G*^{*} = 6.68(10) × 10^{−11} m^{3}kg^{−1}s^{−2}. We would like to note that although the mean value we obtain is only about 0.1% higher than the CODATA 2018 value^{1}, the values obtained from the single measurements are distributed with a standard deviation of 1.32% around the mean. This can be partially attributed to the uncertainty of the elements of the measurement chain. As an example, the laser interferometer systems have not yet been calibrated for the amplitudes and frequencies used in this experiment.

The observation of a mean value close to the expected value but a strong variation mainly due to systematic errors might lead to the assumption that the systematic errors vary strongly with configuration and distance. It was observed that the accelerations on the vacuum chambers are influenced by these parameters (Supp. Fig. 1), such that the mechanical crosstalk is also influenced. The crosstalk uncertainty appears to be of statistical nature in Fig. 5, where a lot of different conditions are summarized. Based on this observation, one might, as an alternative to the above evaluation, consider the crosstalk contribution as a statistical error for the estimation of *G*. Thereby the related uncertainty reduces with \(1/\sqrt{28}\), which yields a combined standard uncertainty of 1.05%.

Supplementary Figure 2 illustrates the phase difference between measurement and theory, increasing with larger distances, supporting the assumption of remaining mechanical, non-gravitational coupling.

Based on a power balance analysis, the near field gravitational energy flow between transmitter and detector can be computed^{7}. At steady state, the incoming energy is equal to the dissipated energy according to the Q factor of the beam. An upper bound of the gravitational power transmitted from the bars to the beam was computed to be 3.75 × 10^{−18} W at *d*_{0} = 296 mm, Ω = *ω*_{0}/2 for a clockwise (CW) rotation of bar nr. 1 and counter-clockwise (CCW) rotation of bar nr. 2, assuming that all incoming power is gravitational. This is about 10^{25} times higher than the expected power of gravitational waves radiated from two equivalent quadrupole gravitational wave generators^{16}, as detailed in the methods subsection on gravitational wave generation.

## Conclusion

In the last couple of years, fully characterized dynamic gravitation experiments turned out to be a promising approach to better understand gravitational interactions^{17}. They open up the path to an investigation of dynamic gravitational effects, covering for example the gravitational wave high-frequency band^{18}.

The combination of two nearly identical rotating bars as transmitter system and a bending beam as detector system proves to be a considerable improvement to previous experiments, cf. Table 1. The velocity amplitudes are one order of magnitude higher compared to ref. ^{7}. The double-transmitter setup enables the investigation of numerous configurations, based on rotation direction combinations and the use of different harmonics as excitation.

Therefore, gravitational and remaining non-gravitational coupling can be better distinguished, making the results more reliable. The precise rotation control, necessary for the double excitation, has the additional merit of enabling an accurate phase measurement between rotation and detector response, which can be very helpful to further understand dynamic, non-gravitational coupling. This experiment does not yet claim to be highly precise: The one-sigma error budget was estimated to 1.46%. Nonetheless, the discrepancy between theory and averaged measurement results of the velocity amplitude is considerably less than 1%, proving the potential of the method. To further increase the measurement quality and reliability, future work focuses on improvements that comprise a more precise distance control between transmitter and detector, reduced temperature sensitivity, characterization of mass distributions, passive and active crosstalk cancellation, and improved model accuracy. The latter requires narrower tolerances and a better understanding of the material structure and behavior of both the rotating bars (material homogeneity, ultra-precise mass measurement, etc.) and detector (temperature behavior, influences on structural damping, etc.). An unexplored resource for the cross-talk characterization involves the investigation of phase-offsets between the rotating transmitter bars. Specifically, a phase offset of 90^{∘} and the resulting predominantly anti-symmetric force field can help to further improve the estimation of the systematic error due to parasitic cross-talk. Since the setup allows for the use of even larger transmitter bars the signal level can be increased by about one order of magnitude. Although higher amplitudes reduce problems associated with the optical vibration measurement of such small amplitudes^{7,19,20,21}, an individual calibration of the interferometric measurement system in the nm/s range is still necessary to considerably reduce the measurement uncertainty. Alternatively, a custom made demodulation of the laser output might enable to directly trace back the detector displacement to the wavelength of light.

We believe that these improvements can bring the experiment way beyond a proof-of-concept state towards a highly precise measurement that might become a standard in dynamic gravitational experiments. It will help to reveal insights in dynamic gravitation, such as frequency dependency or amplitude/phase effects due to objects between transmitter and detector (gravitational shielding). The results and findings of this and future related works can also help to advance the research and application of Newtonian calibrators that are used in gravitational-wave detectors^{9,10,22,23,24,25}.

## Methods

### Superposition of force fields

The situation of the superposition of the force fields generated by the two identical rotating bars has been described only qualitatively in the main article. To mathematically confirm this description, it is useful to look at the Fourier component at *ω* of the individual 1D force components

that are summed up to build the total modal force *F*_{y, b}, cf. Eq. (1). The variable *k* denotes the number of the rotating bar. The Fourier series yields the complex amplitude at the detection frequency *ω*, given by the coefficient *c*_{k}. Assuming identical bars, perfect symmetry with respect to the detector beam and a perfectly symmetric first bending mode shape *U*_{b,1}, the amplitudes ∣*c*_{k}∣ of both complex forces must be equal. The argument of the coefficient *c*_{k}, denoted *∠**c*_{k}, however, differs in sign depending on the rotation direction. It can be shown that, for opposite rotation direction, *c*_{1} equals *c*_{2}, hence the total force has twice the amplitude and the same phase as the single components *c*_{k}. Considering the bars rotating in the same direction \({c}_{1}={c}_{2}^{* }\), where ^{*} denotes the complex conjugate. Consequently, *c*_{1} + *c*_{2} is a real value, which means that no phase shift occurs between the transmitter rotation and the modal force. However, the amplitude gets smaller since the contribution of the imaginary part vanishes. As an example, an excitation with Ω = *ω*/2 with a transmitter/detector distance of *d*_{0} = 300 mm results in *∠**c*_{k} = ± 23^{∘}, which yields an amplitude reduction of 8%, as observed both experimentally and theoretically, cf. Figs. 2 and 4. Supplementary Figure 3 illustrates the superposition of the forces qualitatively.

The situation of both bars rotating in the same direction is thus very convenient to test both the numerical and experimental results. Numerical errors can be detected easily as a phase shift ≠ 0, while experimentally measured phase shift variations indicate either crosstalk or a deviation from the ideal situation of two identical, perfectly synchronized, symmetrically oriented bars. Likewise, differences between the bars can be tested by using one rotating bar only.

### Numerical model

The one dimensional Euler-Bernoulli approach assumes a line distribution of the mass of the detector beam. For the setup presented here this approximation gives reasonable results only if the rotating bars are far away from the detector beam (*d*_{0} > 0.5 m). For improved accuracy, a numerical, 3D finite element (FE) simulation of the transmitter/detector setup is necessary to accurately predict the gravitationally induced motion of the detector beam and to compute the coefficient Γ in Eq. (2) for all distances *d*_{0}.

The detector beam is modeled as a freely suspended, homogeneous, linear-elastic beam, attached to two linear springs in the nodes of its first bending mode. Due to the lock-in measurement technique, the experimentally measured response of the detector is available at the excitation frequency *ω* only. Hence, it suffices to solve for the steady state response of the FE model. The damping of the system is modeled using modal damping^{14}.

Since the force field generated by the rotating bars, illustrated as a transverse force pulse moving along the *x*-axis of the detector beam, represents a moving load problem, it is possible that higher bending modes of the detector are excited as well^{13}. This, in turn, could lead to an additional contribution to the motion measured at the frequency of the first bending mode, which would require an adjustment of Eq. (2), which is based on a SDOF approximation of the detector.

Therefore, the contribution of higher order modes was investigated numerically: Since the modal damping allows to assign experimentally measured Q factors to the first three in-plane bending modes, that is, *Q*_{1} = 45000, *Q*_{2} = 381, *Q*_{3} = 5150, as well as for the rigid body modes of the beam, *Q*_{rb} = 2900, a comparison was performed between a simulation using specific modal Q factors *Q*_{i} and a simulation where all modes have the same damping. The results revealed that the influence of higher modes is negligible for the setup presented in this article, thus the first bending mode can be assumed to be fully decoupled from the other modes. Consequently, Eq. (2) represents a valid approximation of the structural resonance.

The coefficient Γ from Eq. (2) has been calculated individually for all different configurations and 37 discrete distance values *d*_{0} between 290 mm and 600 mm using COMSOL Multiphysics 5.6 and MATLAB R2020b. If necessary, amplitude values at the specific distances are interpolated using a power law fit with the coefficients from Table 2, while the phase is interpolated linearly.

The detector beam is modeled as a linear-elastic rectangular beam with Young’s modulus *E* = 107.4 MPa and Poisson’s ratio of *ν* = 0.37, using the solid mechanics module. The Young’s modulus is determined through a fit to the first resonance frequency of the beam. All other properties of the beam are the same as described in ref. ^{7}. The beam is attached to two linear springs in the nodes of its first bending mode. These springs have a nonzero stiffness in *y*-direction only and their stiffness is set such that it matches the experimentally determined resonance frequency of the beam’s translational pendulum motion in *y*-direction of *f* = 858.3 mHz.

The computation of the detector beam velocity is a three-step process: In a first step, the resonance frequency *ω*_{0} of the beam is computed in the absence of external fields. This resonance frequency is later used to run the frequency space simulation exactly at the resonance frequency of the beam. In a second step, the gravitational force field is computed. The gravitation force on the beam is given by the integral of Newton’s force law over the volume of each rotating bar. Since the force is periodic in time, it can be written as a Fourier series, where the Fourier coefficients are computed in every node of the FE model. In the last step, the FE model of the beam is solved in frequency space at the resonance frequency *ω*_{0}. Depending on the selection of the Fourier coefficient, the solution corresponds to different rotation speeds *ω* of the bars relative to the resonance frequencies.

A convergence study has been performed to ensure the numerical accuracy of the simulation. The gravitational force of the rotating bars has been computed by discretizing the bars into 396 mass elements. For the ensuing discrete Fourier transform of the force, the rotation period of the bars was evaluated at 64 points per rotation. Finally, the FE model is solved for approximately 35,000 tetrahedral elements using quadratic interpolation (DOF ≈ 170000). Taking all three discretization steps into account, we have found the numerical error of the simulation to be far below the measurement errors in the experiment and can thus be neglected in the error budget.

### Gravitational waves generated by rotating bars

The setup of a rotating bar is a classical textbook example of a laboratory quadrupole generator of gravitational waves^{16,26}, in which the power of a slender bar radiated as gravitational waves can be approximately calculated via

where *I*_{z} denotes the rotational inertia of the bar rotating around the *z* axis with frequency Ω and the speed of light *c*. For one of the rotating bars presented in this setup rotating with Ω = *ω*_{0}/2, this power calculates to *L*_{GW} ≈ 4.2 × 10^{−43} W.

In contrast, the power transmitted from two oppositely rotating bars to a detector in a distance *d*_{0} = 296 mm resonating at *ω*_{0} has been estimated to 3.75 × 10^{−18} W, based on the measured resonance amplitude and Q factor of the detector^{7}.

Hence it can be concluded that the generated movement of the detector beam is not attributed to gravitational waves, emitted by the rotating beams but by the dynamic gravitational (near) field.

### Rotational system-mechanics and control

The rotation system is composed of two independent, identical rotary units, of which one system is exemplarily described in this section.

The rotating bar is placed on a turntable, where it can be adjusted and fixated using a clamping cover with alignment pins. The bar exhibits a precisely manufactured indentation in its center of rotation for additional fixation. The rotary unit is mounted with two preloaded spindle bearings (HQW Precision GmbH SV7902) that are clamped to a bearing bracket mounted to a massive aluminum base plate of 15 mm thickness. Attached to the shaft is a maxon EC-i 40 brushless 50 W electric motor with ENC 16 EASY encoder, connected to the base plate as well.

The motor is internally controlled by a maxon EPOS4 50/5 controller. To have full control over the rotation, a master controller based on an Arduino MEGA 2560 is additionally used that communicates with the EPOS system via CAN bus. Both the master and EPOS controller and the power supply are placed outside of the vacuum chamber.

For the gravitational excitation it is of utmost importance that the rotation of both bars is synchronized to a reference signal as precisely as possible. For this task, the built-in controller and rotation sensors are not suitable, due to their limited resolution and non-synchronized clock rates. Therefore, two independent light barriers are embedded in the base plate (cf. Fig. 3c). The light barriers are built from a high-speed PIN photodiode (SFH 2701, 730 nm), a 500 MHz LTC6268 operational amplifier and a 280 MHz LTC6752 comparator. A TLC555 timer is used as line driver, producing a delay of the pulse of 244 ns. The emitted light is reflected from a small aluminum patch (0.035 g) glued to the rotating bar. To ensure mechanical balancing, the same patch is also glued to the opposite side of the bar.

To establish a rotation with a frequency Ω being a fraction of the frequency of a sinusoidal reference signal *ω*, that is, the frequency of measurement provided by a frequency generator, a comparator converts the reference signal to a rectangular signal of frequency Ω, which can then be fed into a digital, flip-flop-based frequency divider. Finally, a PID controller adjusts the frequency of rotation by synchronizing the edges of both the rectangular signal and the pulse of the light barrier with a time resolution of 62.5 ns.

### Measurement uncertainty

Assuming uncorrelated input quantities, the combined standard uncertainty associated with estimating *G* can be calculated from Eq. (2) and Table 2 using a first-order Taylor approximation for each measurement individually. The uncertainties associated with estimating *Q*_{d} and *ω*_{0} result directly from the SDOF fit of the measurement. Initially, the distance *d*_{0} was manually adjusted, where a systematic error of 0.5 mm was assumed. The automatic positioning system itself works very precisely with an error of 1 μm. As mentioned in ref. ^{7}, the uncertainty of the measured velocity *v*_{b,0} is yet unclear for the extremely small amplitudes relevant in the measurements presented here. Therefore, the uncertainties reported in the data sheets of the laser vibrometers have been used for a first assessment. Since the detector bending amplitude is calculated from a linear combination of three laser measurement signals, the contribution to the combined uncertainty reduces by a factor 0.58. Further, an angular misalignment of the laser beam with respect to the detector/transmitter surface of max. 1^{∘} contributes to the uncertainty. Errors that can be attributed to a non-gravitational detector excitation, most likely due to mechanical crosstalk, are estimated with a 1.00% systematic error, based on an evaluation of the detector chamber acceleration. To estimate the variance of the model parameter *γ*, a quasi-Monte Carlo method has been applied, using 2000 quasi-random sequences drawn from the probability distributions specified for the input parameters (Sobol method)^{27,28}. The used input parameters are assumed to be normally distributed with the following standard uncertainties: detector and transmitter dimensions, 0.01 mm, measured using standard precision measuring tools; transmitter masses, measured with a Mettler-Toledo XP6002S scale with 100.00 mg combined uncertainty; an (estimated) uncertainty of *x*, *y* and *z* position of the rotation centers of each 0.20 mm; an eccentricity of ± 10.0 μm of the rotating bars, a constant angle offset between the transmitter bars of ± 0.10^{∘} and an angular misalignment of 0.03^{∘} between the detector’s central axis and the transmitter axis given by the centers of rotation. The bars have been centered using a dial gauge with 10 μm resolution fixed to the rotating bar mount, thus providing a relative measure of the bar’s end faces. The density distribution of the bars has been assumed to be homogeneous. The Monte Carlo simulation has been performed for each setup variation and distance used in the experiments. Therefore, an individual combined uncertainty results for each measurement. In Table 2 the maximum values are exemplarily reported, resulting in a combined standard error of max. 1.46% for an individual measurement.

In this work, the distance *d*_{0} has the highest contribution to the uncertainty of *G*, since the distance uncertainty scales with a factor of up to 5.83, cf. Table 2. To achieve an uncertainty Δ*G*/*G* ≪ 1%, future activities must therefore focus primarily on the distance *d*_{0}, crosstalk elimination, the velocity measurement, and the Q factor determination. Further, influences that are not yet included such as material inhomogeneities, form tolerances, numerical errors etc. must be considered as well.

### Dynamic influence of phase jitter

To achieve a rotation of both bars exactly at a fraction of the resonance frequency, a control loop is necessary that enables the synchronization of the bars’ rotation frequencies to an external reference signal. However, a certain disturbance of this rotation, quantified by a phase jitter *J*_{p}(*t*), might influence the resonance excitation of the detector. Therefore, the influence of a certain phase variation on the detector shall be discussed briefly.

To estimate the errors associated with said disturbance, one can reduce the bending motion to a single-degree-of-freedom oscillator with an external, harmonic excitation *F*. This is a valid approach since the Q factor of the first bending mode is very large (*Q*_{d} ≈ 45,000) and resonance frequencies are well separated. Considering excitation at resonance *ω*_{0}, we can introduce the jitter as phase modulation to the excitation, that is,

The response *x*(*t*) of the oscillator is described by its amplitude and phase \(x(t)=A{{{{{{{{\rm{e}}}}}}}}}^{{{{{{{{\rm{i}}}}}}}}{\omega }_{0}t+{{{{{{{\rm{i}}}}}}}}\phi }\). The effects of the phase noise *J*_{p}(*t*) on the output phase can be analyzed using the transfer function^{29,30}

where \({{\Delta }}\bar{\phi }\) denotes the absolute variation of the detector’s phase around the value at resonance in the frequency domain (indicated by the overbar). The response of the amplitude, however, cannot be easily described by the transfer function of a linear time-invariant system. It can be shown, however, that the amplitude approximately shows a similar low-pass behavior^{31}.

As a consequence, the detector acts as a low-pass filter to disturbances of the excitation phase. Disturbances transmit in the phase via a first-order low-pass filter with a cut-off frequency of *ω*_{c} = *ω*_{0}/(2*Q*_{d}) ≈ 0.5 mHz. Numerical simulations with MATLAB Simulink show a relative amplitude deviation < 1 × 10^{−4} for a white phase noise corresponding to 0.03^{∘} RMS jitter. In summary, phase variations of the excitation force have a negligible effect on the detector’s behavior, since they are minimized by the inertia of the transmitter bars, the motor control system and the high-Q detector itself.

## Data availability

Source data are provided with this paper. The data that support the findings of this study are available as an open access dataset^{32} or from the corresponding author upon reasonable request.

## References

Tiesinga, E., Mohr, P. J., Newell, D. B. & Taylor, B. N. Codata recommended values of the fundamental physical constants: 2018.

*Rev. Modern Phys.***93**, 025010 (2021).The LIGO Scientific Collaboration. Advanced ligo.

*Classical Quantum Gravity***32**, 074001 (2015).Oide, K., Tsubono, K. & Hirakawa, H. The gravitational field of a rotating bar.

*Japanese J. Appl. Phys.***19**, L123–L125 (1980).Majorana, Q. XLVIII. on gravitation. theoretical and experimental researches.

*The London, Edinburgh, and Dublin Philosophical Magazine and Journal of Science***39**, 488–504 (1920).Braginsky, V. B., Rudenko, V. N. & Rukman, G. I. An experimental investigation of the effect of an intermediate medium on gravitational interaction.

*Sov. Phys. JETP***16**, 36–41 (1963).Unnikrishnan, C. S. & Gillies, G. T. New limits on the gravitational majorana screening from the zürich G experiment.

*Phys. Rev. D***61**, 101101 (2000).Brack, T. et al. Dynamic measurement of gravitational coupling between resonating beams in the hertz regime.

*Nat. Phys.***18**, 952–957 (2022).Astone, P. et al. Evaluation and preliminary measurement of the interaction of a dynamical gravitational near field with a cryogenic gravitational wave antenna.

*Zeitschrift für Physik C Particles and Fields***50**, 21–29 (1991).Astone, P. et al. Experimental study of the dynamic newtonian field with a cryogenic gravitational wave antenna.

*Eur Phys J. C - Particles Fields***5**, 651–664 (1998).Hirakawa, H., Tsubono, K. & Oide, K. Dynamical test of the law of gravitation.

*Nature***283**, 184–185 (1980).Ogawa, Y., Tsubono, K. & Hirakawa, H. Experimental test of the law of gravitation.

*Phys. Rev. D***26**, 729 (1982).Kuroda, K. & Hirakawa, H. Experimental test of the law of gravitation.

*Phys. Rev. D***32**, 342 (1985).Fryba, L.

*Vibration of solids and structures under moving loads*(Springer Dordrecht, 1973).Hagedorn, P. & DasGupta, A.

*Vibrations and Waves in Continuous Mechanical Systems*(Wiley, 2007).Hirakawa, H., Narihara, K. & Fujimoto, M.-K. Theory of antennas for gravitational radiation.

*J. Phys. Society Japan***41**, 1093–1101 (1976).Thorne, K. S., Misner, C. W. & Wheeler, J. A.

*Gravitation*(Princeton University Press, 2017).Rothleitner, C. Good vibrations.

*Nature Phys.***18**, 856–857 (2022).Thorne, K. S. Gravitational waves (1995).

Hou, W. & Wilkening, G. Investigation and compensation of the nonlinearity of heterodyne interferometers.

*Precision Eng.***14**, 91–98 (1992).Weichert, C. et al. A heterodyne interferometer with periodic nonlinearities smaller than ± 10 pm.

*Meas. Sci. Technol.***23**, 094005 (2012).Pisani, M. et al. Comparison of the performance of the next generation of optical interferometers.

*Metrologia***49**, 455 (2012).Ross, M. P. et al. Initial results from the ligo newtonian calibrator.

*Phys. Rev. D***104**, 082006 (2021).Kawasaki, A. Measurement of the newtonian constant of gravitation g by precision displacement sensors.

*Classical Quant. Gravity***37**, 075002 (2020).Matone, L. et al. Benefits of artificially generated gravity gradients for interferometric gravitational-wave detectors.

*Classical Quant. Gravity***24**, 2217–2229 (2007).Mio, N., Tsubono, K. & Hirakawa, H. Experimental test of the law of gravitation at small distances.

*Phys. Rev. D***36**, 2321–2326 (1987).Giulini, D. & Kiefer, C.

*Gravitationswellen*(Springer Spektrum, 2017).Morokoff, W. J. & Caflisch, R. E. Quasi-monte carlo integration.

*J. Comput. Phys.***122**, 218–230 (1995).Sobol’, I. M. On the distribution of points in a cube and the approximate evaluation of integrals.

*USSR Comput. Mathematics Mathematical Phys.***7**, 86–112 (1967).Rubiola, E.

*Phase Noise and Frequency Stability in Oscillators*(Cambridge University Press, 2008).Brack, T., Kern, D. & Dual, J. Dynamics and stability of phase controlled oscillators.

*J. Dyn. Sys. Measurement, Control***138**, 071007 (2016).Brack, T.

*Multi-Frequency Phase Control of a Torsional Oscillator for Applications in Dynamic Fluid Sensing*. Ph.D. thesis, ETH Zürich (2017).Brack, T. Dataset for the article “dynamic gravitational excitation of structural resonances in the hertz regime using two rotating bars" (2023-07-04).

Sinsky, J. A. Generation and detection of dynamic newtonian gravitational fields at 1660 cps.

*Phys. Rev.***167**, 1145–1151 (1968).Astone, P. et al. Long-term operation of the rome “explorer" cryogenic gravitational wave detector.

*Phys. Rev. D***47**, 362–375 (1993).

## Acknowledgements

We gratefully acknowledge the support of ETH Zurich, maxon motor ag, ZC Ziegler Consultants AG, and Zurich Instruments AG. We received no specific funding for this work.

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T.B., B.Z., F.P., J.-C.T., S.B., D.S. and J.D. designed and constructed the experiment. T.B., B.Z. and J.D. conducted the experiments, T.B. and J.D. evaluated the data and analyzed the results. T.B, J.D. and F.B. performed the statistical assessment. T.B., S.K., J.F. and J.D. derived and evaluated the theory. J.F. and T.B. performed numerical simulations. All the authors wrote and reviewed the manuscript.

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### Cite this article

Tobias, B., Jonas, F., Bernhard, Z. *et al.* Dynamic gravitational excitation of structural resonances in the hertz regime using two rotating bars.
*Commun Phys* **6**, 270 (2023). https://doi.org/10.1038/s42005-023-01389-5

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DOI: https://doi.org/10.1038/s42005-023-01389-5

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