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**History of Geo- and Space Sciences**
An open-access journal

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- Abstract
- Introduction
- The first theoretical treatment, 1928
- A first detection in 1929: Shortt–Synchronome clock
- Collective measurements 1940–1943: an ensemble of clocks
- Improved measurements in the 1960s: Fedchenko
- Digital data in 1984: Shortt–Boucheron
- Conclusions
- Data availability
- Competing interests
- Special issue statement
- Acknowledgements
- Review statement
- References

HGSS | Articles | Volume 11, issue 2

Hist. Geo Space. Sci., 11, 215–224, 2020

https://doi.org/10.5194/hgss-11-215-2020

© Author(s) 2020. This work is distributed under

the Creative Commons Attribution 4.0 License.

https://doi.org/10.5194/hgss-11-215-2020

© Author(s) 2020. This work is distributed under

the Creative Commons Attribution 4.0 License.

Special issue: Developments in the science and history of tides (OS/ACP/HGSS/NPG/SE...

** **
16 Sep 2020

16 Sep 2020

Time and tide: pendulum clocks and gravity tides

- Cecil H. and Ida M. Green Institute of Geophysics and Planetary Physics, Scripps Institution of Oceanography, University of California, San Diego, 9500 Gilman Drive, La Jolla, CA 92093-0225, USA

- Cecil H. and Ida M. Green Institute of Geophysics and Planetary Physics, Scripps Institution of Oceanography, University of California, San Diego, 9500 Gilman Drive, La Jolla, CA 92093-0225, USA

**Correspondence**: Duncan C. Agnew (dagnew@ucsd.edu)

**Correspondence**: Duncan C. Agnew (dagnew@ucsd.edu)

Abstract

Back to toptop
Tidal fluctuations in gravity will affect the period of a pendulum and hence the timekeeping of any such clock that uses one. Since pendulum clocks were, until the 1940s, the best timekeepers available, there has been interest in seeing if tidal effects could be observed in the best performing examples of these clocks. The first such observation was in 1929, before gravity tides were measured with spring gravimeters; at the time of the second (1940–1943), such gravimeters were still being developed. Subsequent observations, having been made after pendulum clocks had ceased to be the best available timekeepers and after reliable gravimeter measurements of tides, have been more of an indication of clock quality than a contribution to our knowledge of tides. This paper describes the different measurements and revisits them in terms of our current knowledge of Earth tides. Doing so shows that clock-based systems, though noisier than spring gravimeters, were an early form of an absolute gravimeter that could indeed observe Earth tides.

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Agnew, D. C.: Time and tide: pendulum clocks and gravity tides, Hist. Geo Space. Sci., 11, 215–224, https://doi.org/10.5194/hgss-11-215-2020, 2020.

1 Introduction

Back to toptop
The invention of the pendulum clock by Christiaan Huygens in 1657 tied precise time measurement and gravity together for almost the next 3 centuries, until the development of quartz and atomic frequency standards. Not only did Huygens' own research come from an investigation of how bodies fall (Yoder, 1989) but also the first indication that gravitational acceleration differed from place to place on Earth came from the finding, by Jean Richer in 1672, that a pendulum beating seconds (frequency 0.5 Hz) at Paris needed to be shortened by 0.3 % to do so at Cayenne, just north of the Equator (Olmsted, 1942). Some later measurements of gravity made direct use of clocks or otherwise driven pendula (Graham and Campbell, 1733; Mason and Dixon, 1768; Phipps, 1774; Sabine, 1821), though more usually, and especially after the work of Kater (1818, 1819), almost all measurements of gravity relied on freely swinging pendula (Lenzen and Multhauf, 1965). In a few cases these pendula were used to measure acceleration absolutely (Cook, 1965), but more usually their frequency was compared either to a local clock or to a reference pendulum at another location (Bullard and Jolly, 1936).

The purpose of this note is to describe the few
cases in which pendulum clocks have been used to measure
temporal changes in gravity at a fixed location,
specifically the changes in the intensity of gravity *g*
caused by the tidal effects created by the Moon
and Sun (Agnew, 2015).
It might be thought that these
changes, being at most 10^{−7} of the total
gravitational acceleration, would be too small
to measure and also that they could not be
measured without a time standard unaffected by
gravity.
While the second point is true, the first is not:
I have identified four occasions on which
clocks have had timekeeping stability good enough that
they have detected tidal gravity changes.
The first occasion is of interest as being,
I believe, also the first measurement of tidal changes in gravity,
while the second helped to determine the
Love numbers.
The other two, having been made after the
development of precise tidal gravimeters
using a mass on a spring, are not of great
geophysical import
but do serve to show what kind of
pendulum clock could measure the tides, sometimes very clearly,
as in Fig. 1, which shows the time
error from a clock discussed more fully in Sect. 6.
Getting this kind of performance from a pendulum clock
is anything but easy (Woodward, 1995; Matthys, 2004),
so it is interesting to see how it has been done.

2 The first theoretical treatment, 1928

Back to toptop
The effect of tides on pendulum clocks appears to have first been examined by Jeffreys (1928), following a suggestion by the amateur horologist Clement O. Bartrum. He also examined the variations in Earth's rate of rotation caused by the long-period tides, something not detectable without better measurements of both time and Earth orientation. Harold Jefferys' response combined the astronomical expressions for the tides with the response of a clock; it is simpler to start with how changes in gravity affect timekeeping and then use the harmonic description of the tides.

With a few (and very imprecise) exceptions,
all clocks depend on an oscillator with some
frequency *f*(*t*), which is converted to phase
(e.g., the position of a clock hand on its dial)
according to

$$\mathit{\varphi}=\underset{\mathrm{0}}{\overset{T}{\int}}f\left(t\right)\mathrm{d}t,$$

which in turn is converted to time by the
assumed frequency of the oscillator *f*_{0}
to give a measured time *T*_{m}:

$${T}_{\mathrm{m}}={\displaystyle \frac{\mathit{\varphi}}{{f}_{\mathrm{0}}}}=\underset{\mathrm{0}}{\overset{T}{\int}}{\displaystyle \frac{f\left(t\right)}{{f}_{\mathrm{0}}}}\mathrm{d}t$$

so that if *f*(*t*)=*f*_{0}, *T*_{m} is the true time *T*.
If, however, there is a frequency error
${f}_{\mathrm{e}}\left(t\right)=f\left(t\right)-{f}_{\mathrm{0}}$, there will be a corresponding
error in phase *ϕ*, which in horological terms means a time error:

$$\begin{array}{}\text{(1)}& {T}_{\mathrm{e}}={T}_{\mathrm{m}}-T=\underset{\mathrm{0}}{\overset{T}{\int}}{\displaystyle \frac{{f}_{\mathrm{e}}\left(t\right)}{{f}_{\mathrm{0}}}}\mathrm{d}t.\end{array}$$

Clock performance can thus be described in terms of
fractional-frequency error *f*_{e}(*t*)∕*f*_{0}, known in horology as the rate
and usually expressed in seconds per day.
For pendulum clocks it is difficult to
measure this with high accuracy, and in all
the cases described here
the actual measurement was of *T*_{e}(*t*),
given by Eq. (1), from which an
average of *f*_{e}(*t*)∕*f*_{0} can be found for some interval
of observation.

The frequency of a pendulum is given, for small arcs of swing, by

$$\begin{array}{}\text{(2)}& f={\displaystyle \frac{\mathrm{1}}{\mathrm{2}\mathit{\pi}}}\sqrt{{\displaystyle \frac{l}{g}}}\left(\mathrm{1}-{\mathit{\theta}}^{\mathrm{2}}/\mathrm{16}\right),\end{array}$$

where *g* is the gravitational acceleration,
*l* the length of the equivalent simple pendulum
(with all mass at a point)
and 2*θ* is the total arc of swing (Baker and Blackburn, 2005).
Typically *θ* is less than 1^{∘},
or 0.02 rad, so the term in *θ*^{2} may be
disregarded for finding the derivative needed.
This is the partial derivative of
*f*_{e}∕*f*_{0},

$$\begin{array}{}\text{(3)}& {\displaystyle \frac{\mathrm{1}}{{f}_{\mathrm{0}}}}{\displaystyle \frac{\partial f}{\partial g}}={\displaystyle \frac{-\mathrm{1}}{\mathrm{2}}}\sqrt{{\displaystyle \frac{g}{l}}}\sqrt{{\displaystyle \frac{l}{{g}^{\mathrm{2}}}}}={\displaystyle \frac{-\mathrm{1}}{\mathrm{2}g}},\end{array}$$

so that ${f}_{\mathrm{e}}\left(t\right)/{f}_{\mathrm{0}}={g}_{c}\left(t\right)/\mathrm{2}g$,
where *g*_{c}(*t*) is the time-variable part of gravity
and *g* is its average value.

A sense of the tidal effects is best gotten by using a
harmonic expansion of the tide and looking at
individual harmonics.
This can be done using Eqs. (7), (8), (11) and (18) of Agnew (2015);
note that Eq. (18) is missing a factor of 2.
The fractional change in pendulum frequency
from a tidal harmonic of
amplitude *A*, frequency *ζ* and phase *α* is

$$\begin{array}{}\text{(4)}& \begin{array}{rl}{\displaystyle \frac{\mathit{\delta}f}{{f}_{\mathrm{0}}}}& ={\displaystyle \frac{\mathit{\delta}g}{\mathrm{2}g}}={\displaystyle \frac{{\mathit{\delta}}_{n}A{g}_{\mathrm{e}}}{{a}_{\mathrm{e}}g}}{N}_{n}^{m}{P}_{n}^{m}\left(\mathrm{cos}\mathit{\phi}\right)\left[\mathrm{cos}\right(\mathrm{2}\mathit{\pi}\mathit{\zeta}t+\mathit{\alpha}\left)\mathrm{cos}\right(m\mathit{\lambda})\\ & +\mathrm{sin}(\mathrm{2}\mathit{\pi}\mathit{\zeta}t+\mathit{\alpha})\mathrm{sin}\left(m\mathit{\lambda}\right)],\end{array}\end{array}$$

where *n* and *m* are the degree and order of the tide;
for the tides considered here, *n*=2.
The other variables are *a*_{e} (Earth's equatorial radius),
*g*_{e} (gravitational acceleration there),
*g* (local gravitational acceleration),
*δ*_{n} (gravimetric factor),
${N}_{n}^{m}$ (normalization coefficient)
and ${P}_{n}^{m}$ (associated Legendre polynomial).
The location is given by the colatitude *φ* and longitude *λ*.
For *n*=2 the gravimetric factor is given by
${\mathit{\delta}}_{\mathrm{2}}=\mathrm{1}+{h}_{\mathrm{2}}-\mathrm{1.5}{k}_{\mathrm{2}}$,
where *h*_{2} and *k*_{2} are the Love numbers for
vertical displacement and potential change.
For the Preliminary Reference Earth Model, *δ*_{2}=1.1562.

Taking the integral of Eq. (4) gives, for the time-independent amplitude,

$$\begin{array}{}\text{(5)}& {\displaystyle \frac{{\mathit{\delta}}_{n}}{\mathrm{2}\mathit{\pi}\mathit{\zeta}}}{\displaystyle \frac{A{g}_{\mathrm{e}}}{{a}_{\mathrm{e}}g}}{N}_{n}^{m}{P}_{n}^{m}\left(\mathrm{cos}\mathit{\phi}\right).\end{array}$$

Letting *g*=*g*_{e} for simplicity, Table 1
gives the resulting values for the largest tidal harmonics
(all those with amplitudes more than 10^{−4} s).
The largest harmonic by far is that associated with the
nodal tide (period of 18.6 years).
All of the diurnal and semidiurnal tides have
amplitudes less than a millisecond.

Jeffreys (1928) obtained similar results;
perhaps because of a mistake in normalization,
the final amplitudes he gave for the tidal harmonics of *T*_{e} are
about 1.4 times those in Table 1.
He stated that
while the long-period effects are the largest, their
detection would require a level of long-term stability
not seen in pendulum clocks and described the shorter-term changes
as “within the limits of error of the most accurate time-measurements,
but perhaps not so far within them as to be entirely devoid of interest”.

One further point can be made about tidal measurements with
pendula.
Equation (3) means changes in *g*
can be inferred from changes in *f* directly:
the scale factor from fractional frequency
to gravity is just 2*g*, which can easily
be determined to a precision and accuracy
of 10^{−4}.
Since the pendulum is a kind of falling-weight
measurement, it is not surprising that it provides
a measure of changes in *g* that can be tied back to standards
of length and time.
This is not at all the case with spring gravimeters,
the calibration of which was difficult until
portable and highly precise free-fall
absolute gravimeters were developed.
It is now routine to use absolute gravimeters to check the drift
and scale factor of spring gravimeters intended for
tidal measurements (Hinderer et al., 2007).
But a pendulum that can record the tides needs no
calibration.

3 A first detection in 1929: Shortt–Synchronome clock

Back to toptop
As noted above, it is not possible to measure the effects of gravity tides on pendulum clocks without another clock that is not affected by gravity. No such clock of adequate accuracy existed until the 1920s, when electronically maintained oscillators such as tuning forks and quartz crystals were developed. The first quartz-crystal clock was developed by Warren Marrison in 1927 (Katzir, 2016); very soon after (1929) it was used for the study of pendulum clocks. This project was initiated (and funded) by Alfred L. Loomis (Conant, 2002), who turned to various scientific investigations after a very successful legal and financial career had brought him great wealth.

Loomis' study of pendulum clocks comprised three elements (Loomis, 1931).
The first was an electrical signal maintained at 1000 Hz by
the quartz oscillator operated by Marrison at Bell
Telephone Laboratory in Manhattan
and provided (over a dedicated telephone line)
to Loomis' private laboratory, 65 km away in Tuxedo Park
(41.1835^{∘} N, 74.2144^{∘} W).
The second was three of the highest-quality pendulum
clocks then available, the Shortt–Synchronome clock
(described below).
The third was a chronograph developed by Loomis,
which used a rotating arm driven by the 1000 Hz signal
at 10 revolutions per second,
which could cause a spark to burn a hole in a slowly moving paper
record whenever a signal was received.
The least count of this system (to use the current term) was 10^{−3} s;
signals from the three Shortt–Synchronome
clocks were recorded every 30 s,
and changes between them or between them
and the quartz oscillator could easily be monitored.

Shortt–Synchronome clocks will appear three times in this account,
so a brief description of them is appropriate;
much more detail is available in Hope-Jones (1940) and Miles (2019),
though the most accessible description is given by Woodward (1995).
The double name reflects the nature of these clocks,
which consisted of a pair of pendulum systems.
One was the Synchronome, an electromechanical clock
manufactured by the company of that
name to serve as a controller of many subsidiary clocks,
sending out signals at regular intervals.
The other pendulum, designed by engineer William H. Shortt,
was the heart of the system:
it swung freely in a container evacuated to a pressure of 3 kPa.
The only exception to its free motion was that every 30 s,
in response to a signal from the Synchronome clock,
a pivoted lever was lowered onto a small wheel attached to the Shortt
pendulum.
As the pendulum swung away from the lever, the lever fell off the wheel,
applying a slight horizontal force to the pendulum;
in horological terminology, this is called impulsing the pendulum.
The lever's fall was arrested by contact with a switch
which performed two actions:
it caused the lever to be raised and reset, ready for the next
30 s signal, and it actuated a mechanism to speed
up the Synchronome clock if it had fallen behind, which it was
deliberately designed to do.
So the Shortt free pendulum controlled the overall timekeeping but
did so in a way that involved minimal interaction with the Synchronome clock,
thus approximating as much as possible a completely free and undamped
pendulum – and
thanks to the evacuation of the pendulum chamber, the *Q* factor of
the free pendulum was approximately 10^{5}.

Loomis supported not just the measurements
but also the associated data analysis,
conducted by Ernest W. Brown (developer of lunar theory)
and his student Dirk Brouwer (Brown and Brouwer, 1931),
with, as was usual in those days, “a large amount of
calculation, most of which was performed by Mrs. D. Brouwer.”
Of the various results, the one of interest for this
paper was the effort to look for a lunar effect in the
difference between the pendulum and quartz timekeeping.
This was done by using a form of stacking of the data
(Brown, 1915).
The values were taken at hourly intervals and
each was assigned to the nearest “lunar hour”:
that is, 0.04167 of the lunar day of 24.83 h.
All values for a particular lunar hour were summed and
averaged.
This procedure, viewed as a digital filter, has a response
close to one at multiples of the M_{1} tidal frequency of
0.9664463 cycles d^{−1} and so should mostly show the effect of the
M_{2} tide.

Figure 2 shows the results plotted in Fig. 3 of
Brown and Brouwer (1931), specifically the result of an analysis of
147 d of data of the difference between one of the Shortt
clocks (since it was denoted as “Clock 1”, it was probably
serial number 20) and the quartz frequency standard.
As would be expected,
a similar analysis of the three pendulum clocks relative to each
other did not show any clear variation.
Fitting sinusoids with frequencies of 1 and 2 cycles per lunar
day removes all of the variation;
the diurnal sinusoid has
an amplitude of $\mathrm{0.097}\times {\mathrm{10}}^{-\mathrm{3}}$ s with a phase of 178^{∘};
the semidiurnal sinusoid has
an amplitude of $\mathrm{0.161}\times {\mathrm{10}}^{-\mathrm{3}}$ s with a phase of 166^{∘}.

Brown and Brouwer (1931) noted that the variation was approximately that expected on a rigid Earth, something they found puzzling because of their mistaken idea that gravity variations on an elastic Earth would be $\mathrm{1}+h+k=\mathrm{1.87}$ times the rigid-Earth variations. They attempted to explain their observation by a large ocean-loading effect but seem to have decided that their results were inconclusive.

In order to re-evaluate their results, I produced a simulation of the tidal
time changes at this location and time, using the “SPOTL” (Some Programs for Ocean-Tide Loading)
package (Agnew, 2012);
ocean loading was computed from the TPXO7.2 global model
and the OSU (Oregon State University) local model for eastern North America,
though this loading turns out to alter the predicted time by less than 5 %.
Figure 2 also shows the result of an analysis
of this predicted tide done by averaging values assigned to
the same lunar hour.
The two series appear similar;
again fitting two sinusoids,
the diurnal sinusoid has
an amplitude of $\mathrm{0.023}\times {\mathrm{10}}^{-\mathrm{3}}$ s with a phase of −161^{∘}
not in agreement with the fit to the data.
But the semidiurnal sinusoid has
an amplitude of $\mathrm{0.178}\times {\mathrm{10}}^{-\mathrm{3}}$ s with a phase of 170^{∘},
which is to say 10 % larger and almost exactly in phase with the
analyzed data. Given the quality of the measurements, this is excellent agreement.

So these pendulum clocks were able to detect and accurately measure
tidal changes in the amplitude of gravitational
acceleration *g*.
At this time almost all Earth tide measurements were of tilt,
which is to say changes in the direction of gravity.
Lambert (1931) does not mention any observations
of tidal changes in *g*,
while Lambert (1940) describes only some measurements made
in the US in 1938–1939.
The first successful observation of tidal changes in *g* that I have
found is that by Tomaschek and Schaffernicht (1932),
who showed a few days of data and analyzed 2 months worth,
but they would appear to have had a calibration problem,
since their result for *δ* was 0.64, 55 % of the true value.
As noted in Sect. 2, pendulum measurements
are free from calibration uncertainties.

4 Collective measurements 1940–1943: an ensemble of clocks

Back to toptop
The next attempt to measure tidal effects with pendulum clocks
was by Stoyko (1949) and explicitly aimed at using tidal
gravity to determine *δ*, which when combined with tidal
tilt measurements could provide values for the two Love numbers
*h* and *k*.
The measurements were made at the Paris Observatory
(48.8364^{∘} N, 2.3365^{∘} E),
a good choice in two ways.
First of all,
it was the location of the Bureau Internationale de l'Heure (BIH),
the entity responsible for defining a unified time system by
determining corrections (after the fact) to the time signals
broadcast by different countries and based on timekeeping from
different observatories.
Broadcast time signals showed unexpectedly large deviations
between different timekeepers, and the BIH was established to
deal with this (Kershaw, 2019).
Given this mandate, the BIH maintained a relatively large
ensemble of clocks.
These were housed in a vault at 23 m depth,
much deeper than most other timekeepers, a setting where even annual variations in temperature
would be small and ground noise would be attenuated.

In looking for tides, six of the BIH clocks were used. One was a Shortt–Synchronome clock (number 44), while four were precision pendulum clocks built by the French firm of Leroy et Cie (Roberts, 2004). These were as simple as the Shortt–Synchronome clock was complex: a single pendulum driven by an escapement that used springs to provide a nearly invariant impulse to the pendulum (Martin, 2003), only two wheels in the gear train and a gravity drive using a 7 g weight electrically rewound every 30 s. As in the Shortt–Synchronome clock, the pendulum operated inside a sealed tank, though at a pressure (80 kPa) not far below atmospheric. The sixth timekeeper was a tuning-fork frequency standard built by the electronics firm of Belin.

The differences between these timekeepers was recorded twice
daily, at 08:10:30 and 20:10:30 universal time,
on a high-speed chronograph, recording on paper at 0.25 m s^{−1}.
These 12 h samples were then (in today's terms)
convolved with a high-pass filter with weights (1, −3, 3, −1)
(removing any constant, linear or quadratic behavior)
and then, it appears, analyzed as daily samples.
The Nyquist frequency was thus reduced to 0.5 cycles d^{−1},
so the M_{2} tide would have been aliased to a period of 14.7 d,
while
the K_{1} and P_{1} harmonics would both have been aliased
to a frequency of 1 cycle per year.
Monthly means were created, with an annual variation fit to them to determine the size of
these diurnal tides.
For the M_{2} tide each difference was assigned to the nearest
lunar hour, and a year of these was summed.
Comparison with equivalently processed rigid-Earth tides
then allowed the gravimetric factor *δ* to be found
for each year from 1940 through 1943.

Figure 3 shows the values of *δ* (normalized
against what we now know is the true value) determined for the
five clocks over 4 years for both the K_{1} − P_{1} and M_{2}
tides.
While there is a great deal of scatter, the median value
of the normalized *δ* is 1.05.
It is notable that the scatter of the estimates increases for the
last 2 years compared to the first 2 years:
given that Paris was under German occupation,
it can easily be imagined that replacement parts
for delicate instruments of this kind
might have been difficult to get.
But these results, at the time they were published,
were not drastically worse than what had been attained
by gravimeter measurements.
It does not appear that the Leroy clocks were significantly
worse at measuring tides than the Shortt–Synchronome clock,
though it is likely that the extremely stable environment
they were operated in played a part in allowing this.

5 Improved measurements in the 1960s: Fedchenko

Back to toptop
While quartz clocks became the best measurers of time in the 1940s, pendulum clocks remained popular in some settings, since they did not require specialized electronics expertise to maintain. Judging by the sales of the Shortt–Synchronome clocks, this was particularly the case in Communist countries: of the 31 such clocks sold after 1945 (Miles, 2019), 19 went to the People's Republic of China, eastern Europe or the Soviet Union (USSR). Indeed, the USSR built its own version of the Shortt–Synchronome clock, the “Etalon” clocks (Roberts, 2004). And in addition, the USSR introduced and manufactured an alternate design of pendulum clock, one very different from the Shortt–Synchronome clock.

These clocks were invented by Feodosii Mikhailovich Fedchenko;
Feinstein (2004) is the fullest English-language
description.
Three models were produced, the AchF-1, AchF-2 and AchF-3,
all of which used a pendulum suspension
that removed the *θ*^{2} term in the frequency expression
given in Eq. (2).
This term exists because the restoring force on a pendulum
varies as sin *θ* rather than *θ*, creating
a slightly nonlinear system in which the frequency depends
on the amplitude of swing.
From Eq. (2), the dependence of a normalized
frequency on the angle of swing is

$$\frac{\mathrm{1}}{{f}_{\mathrm{0}}}}{\displaystyle \frac{\partial f}{\partial \mathit{\theta}}}={\displaystyle \frac{\mathit{\theta}}{\mathrm{8}}},$$

which, for a typical arc of swing of $\mathrm{1}{}^{\circ}=\mathrm{1.75}\times {\mathrm{10}}^{-\mathrm{2}}$ rad,
is $\mathrm{2.18}\times {\mathrm{10}}^{-\mathrm{3}}$.
So a variation of fractional frequency
of 10^{−8} would be produced by a fractional change
in arc of approximately $\mathrm{5}\times {\mathrm{10}}^{-\mathrm{6}}$.

For small arcs, the change in height of the bob is proportional
to the square of the arc, so
the arc is approximately proportional to the square root of the energy of
the pendulum.
In a steady state, this energy is proportional
to the energy input,
so a frequency change of 10^{−8} would be created
by a fractional change in energy input of $\mathrm{2}\times {\mathrm{10}}^{-\mathrm{3}}$,
a stability that is difficult to achieve.
Fedchenko's accomplishment was to devise a method for
eliminating the *θ*^{2} term in Eq. (2),
making the pendulum what is termed isochronous. He accomplished this by suspending the pendulum
from three steel strips, with one longer than the other two;
this created an additional elastic restoring force that
could be adjusted to cancel the *θ*^{2} term
(Woodward, 1999).
While there had been earlier proposals for elastic
devices to make a pendulum isochronous
(Phillips, 1891, 1892; Bush and Jackson, 1951),
Fedchenko's seems to have been the only one to see actual use.

The pendulum of the AchF-3 swung in a low vacuum (0.4 kPa); its position was sensed, and a force was applied to it electromagnetically. Permanent magnets were mounted on the pendulum and passed through a pair of coils at the bottom of its arc. These coils were fixed to a rod that would expand and contract with temperature in parallel with the pendulum, keeping the geometry of the magnet-coil system unchanged. As the magnets moved past the coils, they generated a voltage in one coil, and on alternate swings this voltage was applied to a two-stage transistor amplifier that produced a current in the second coil in the opposite sense to that induced in the first, applying a small force to the pendulum. The amplifier in this feedback system was driven by a small constant-voltage battery: the power consumption was about 60 µW.

The best evidence for the detection of tidal fluctuations of this
clock comes from Agaletskii et al. (1970);
the senior author was a metrologist with an interest in absolute measurements of *g* (Cook, 1965),
who wished to present the clock as a direct measurement of the
tidal fluctuations that would affect any determination of *g*.
The data were collected at the
All-Union Scientific Research Institute for Physical-Engineering and Radiotechnical Metrology in
Mendeleyevo, outside of Moscow
(56.038^{∘} N, 37.232^{∘} E).
A total of 6 months of records were shown
for September through December of 1968 and 1969.
The data curves are clearly hand-drawn.
Agaletskii et al. (1970) state that it was not until after 6 months
of “hunting” by the feedback mechanism that the rate became steady;
this was probably because of the high *Q* of the pendulum,
probably several times 10^{5} (Bateman, 1977).

Figure 4 shows the data from the clock: the tides are clearly visible. I again computed the theoretical tide for this location using SPOTL and shifted the time of observations by subtracting 3 h to go from Moscow to Universal Time. Subtracting this from the data produces a series with a noticeably lower variance. Shifting the times further (1.25 more hours for the 1968 data and 1.75 more hours for the 1969 data) produces the lowest variance and the least amount of visible tidal signal in the residual: this is an acceptable adjustment, given the crudeness in digitizing a hand-drawn curve. Allowing for a scale factor between the theoretical tides and the observations produces a factor of 0.9 for both years. Clearly the clock data measure the diurnal and semidiurnal tides. Alexeev and Kolosnitsyn (1994) used these data and a longer set of daily data to show that the Mf tide could also be detected.

6 Digital data in 1984: Shortt–Boucheron

Back to toptop
The final measurement discussed here returns to
the Shortt–Synchronome clock, only without the Synchronome.
In 1932, Shortt–Synchronome serial number 41 was installed
in the U.S. Naval Observatory (USNO; 38.922^{∘} N, 77.067^{∘} W)
as a sidereal time standard:
that is, a clock that could be directly compared with
astronomical observations.
By 1946, all pendulum clocks at USNO had been replaced
by quartz-crystal clocks (Sollenberger and Mikesell, 1945)
but were left in the specially built clock vault (Dick, 2003).
Almost 40 years later, Pierre Boucheron,
an engineer and amateur horologist,
visited USNO to look for information on their clocks'
performance.
While there, he visited the clock vault and
found that the original Shortt pendulum for number
41 was there and still under vacuum;
he also found that a mirror had been attached to
the pendulum and an optical-flat window had been installed
in the bell jar that was the top part of the vacuum
enclosure.
With USNO's permission, he set up an
optical lever to measure the pendulum's motion,
sending current from a photocell to some simple
logic circuits that, every 30 s, dropped
the impulsing lever just as the Synchronome had.
A second photocell sent timing pulses to a counter
which was read every hour and compared with the
USNO atomic master clock (Boucheron, 1985).
Boucheron called this system, like the Synchronome
part of the Shortt–Synchronome clock, a “slave” system;
but unlike the Synchronome, it did not have any
timekeeping ability, and the position of the Shortt pendulum
was used directly to release the impulse lever.
As Boucheron pointed out, the optical-sensing system probably
had less variability in sensing the time of swing
than the electromechanical switches and contacts
of the Shortt–Synchronome clock.

This system operated for just under a year, from 1984:292 (year:day of year) through 1985:278. Boucheron (1986, 1987) described the clock's performance. As a timekeeper it was poorer than might be expected, showing variations of up to 1.5 s over the course of the year. But the clock's short-term stability was good enough that Earth tides were visible in plots of the hourly rate. Boucheron (1987) discussed the tidal response in more detail, although his analysis did not go much beyond that of Brown and Brouwer (1931).

These data were transcribed by Philip Woodward in order to perform a spectral analysis (Woodward, 1995); in keeping with earlier results (and standard horological practice) he differenced the times to produce hourly rates. Machine-readable hourly rate data are available over the full span of observation; the time differences plotted in Fig. 1 are available only for the first 3 months. Again, to compare rates with the tidal fluctuations I computed the theoretical gravity tide using SPOTL; here too the ocean load tide does not have a large effect. Parallel harmonic analyses of the gravity signal and the hourly rates give, for the major tides, the complex value of the ratio of observed to theoretical tides (the admittance).

Table 2 gives the results for
the larger tidal harmonics.
Except for M_{2},
all the admittance amplitudes
are a few percent below one, with phase differences
scattered about zero.
A 2^{∘} phase shift is the same magnitude as a 4 %
change in amplitude,
so it is reasonable to believe that
this scatter comes from background noise at the tidal
frequencies.

To determine this noise level I computed the power spectral density of the rate data in two ways. First, I computed the periodogram of the data: that is, computing the discrete Fourier transform and finding the amplitude at each frequency. While this estimate of the PSD (power spectral density) can be biased and is always inconsistent (in the statistical sense), it is the best way to show narrowband signals such as the tide.

Fitting tidal harmonics to the data leaves no tidal lines visible in the periodogram, which means that more averaging of the spectral estimates is appropriate. The second set of spectrum estimates were found using the adaptive multitaper method described by Barbour and Parker (2013). This minimizes a combination of the local bias caused by curvature of the power spectrum and the uncertainty of the estimates. The relative weighting of these two components of spectral error is adjustable, and Fig. 5 shows the spectrum for three different values of the parameter. As less weight is given to minimizing local bias, the spectrum becomes less smooth; in this case the main effect is to reduce bias at the very lowest frequencies.

Along with the tides, the spectra show several peaks at periods around 2.8 to 3.5 h, which are clearest in the multitaper estimate. These periods are much longer than the period of the gravest normal mode, which itself is far too small to be visible in these data. The source of these spectral peaks is not understood but is assumed to be some irregularity in the mechanical system that drives the pendulum. Loomis (1931) noted that each of his clocks showed a characteristic pattern of short-term variations.

The noise level of the Shortt–Boucheron clock can be described
by a PSD which varies as
a power of frequency *f*^{β} over three different frequency bands.
For frequencies
less than $\mathrm{4}\times {\mathrm{10}}^{-\mathrm{6}}$ Hz (periods longer than 70 h),
the exponent of the power law is $\mathit{\beta}=-\mathrm{1.9}$:
essentially the same random-walk
behavior found by Woodward using the Allan variance
(see chap. 18 of Rawlings, 1993)
and (though not identified as such) by Greaves and Symms (1943).
This behavior is undesirable because it diverges with time, and
its integral, the time error (what clocks are supposed to
measure), diverges even more rapidly.
For periods from 70 to 28 h, $\mathit{\beta}=-\mathrm{0.6}$, which is close to
flicker noise; for periods less than 28 h, *β*=0.2, which is
close to white noise, though clearly increasing with frequency.
It is quite possible that
this increase (and the mystery peaks) comes from
variations at even shorter periods that
appear to be at longer ones because of the hourly sampling.

Figure 5 also shows the PSD of the two residual series of the Fedchenko data, plotted in Fig. 4. To obtain the equispaced data needed for these spectra, a local regression (loess) was done on the point cloud, and the results linearly interpolated to a 0.05 d interval, which is comparable to the original 2 h spacing. I estimated the PSD using the same adaptive method; given that the series was derived from hand-plotted data, the true PSD is very likely below the ones shown. It is clear that the Fedchenko clock, in this frequency band, is definitely less noisy than the Shortt–Boucheron system.

7 Conclusions

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Despite the extreme difficulty of making clock pendula respond
only to changes in gravity and nothing else,
the best pendulum clocks have shown the ability to detect tides,
with the first example preceding any gravimeter measurements.
And pendulum measurements, like other falling-mass systems,
provide a result that is easily calibrated: the result of
Brown and Brouwer (1931), properly interpreted, would have given an
accurate value of the factor *δ* for the gravity tides.

The observations reviewed here also make a horological point, namely that there is more than one way for a pendulum clock to have the performance demanded – something recently demonstrated by the excellent performance of a clock deliberately designed to make use of the nonlinear part of Eq. (2) to compensate for environmental changes (McEvoy and Betts, 2020).

The developers of the Shortt clock emphasized that it used a free pendulum, which was only impulsed at longer intervals and in a way that required no input from the pendulum. But neither the Leroy nor the Fedchenko clock had this feature: in both, the pendulum was used to time the impulse, and this impulse was given frequently. It also does not seem to have been necessary for the pendulum to swing in an evacuated space, since the range of vacua in these clocks was from 0.4 to 80 kPa. The Littlemore clock of Hall (2004), built in the 1990s, aimed at improved performance by having an even freer pendulum operating in a high vacuum ($\mathrm{2}\times {\mathrm{10}}^{-\mathrm{4}}$ Pa) and being impulsed electromagnetically. Though over 250 d its timing error was within 50 ms, its short-term stability was poor: a spectrum of the rate data, if plotted in Fig. 5, would be a white spectrum at −88 dB.

While the first measurements of gravity tides were better made by clocks than by gravimeters, the latter rapidly improved, partly thanks to the stimulus of military and industrial funding (Warner, 2005). Figure 5 shows a gravimeter noise spectrum from 1962; at tidal frequencies this is comparable to the best clock performance. Modern superconducting gravimeters have a much lower noise level: for fractional gravity change, it is −155 dB for periods of 12 to 24 h, while modern spring gravimeters are only about 6 dB noisier (Rosat et al., 2004, 2015; Calvo et al., 2014).

So “tide from time” is now not at all the best measurement of gravity changes but a signal that can demonstrate good short-term oscillator performance. Horological measurements of gravity span over 3 and a half centuries; even though their utility is now gone, it has been an interesting journey.

Data availability

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Data availability.

The data shown in Figs. 1 and 2 are available from the author. The data shown in Fig. 4 are available from Agnew (2020, https://doi.org/10.5281/zenodo.3978746).

Competing interests

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Competing interests.

The author declares that there is no conflict of interest.

Special issue statement

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Special issue statement.

This article is part of the special issue “Developments in the science and history of tides (OS/ACP/HGSS/NPG/SE inter-journal SI)”. It is not associated with a conference.

Acknowledgements

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Acknowledgements.

I thank Bob Holmström and Tom Van Baak for discussions: more specifically I thank Bob Holmström for alerting me to the 1949 paper by Stoyko (Stoyko, 1949) and the 1994 paper by Alexeev (Alexeev and Kolosnitsyn, 1994) and Tom Van Baak for providing me with the Shortt 41 rate and Littlemore time data and for reminding me about the need to consider time shifts in data fitting. The gravimeter data used for the spectrum in Fig. 5 were provided to Walter Munk by Louis B. Slichter in 1964; their preservation over the next half century is due to the efforts of Florence Oglebay Dormer and David Horwitt. I thank Walter Zürn and another referee for their helpful reviews.

Review statement

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Review statement.

This paper was edited by Mattias Green and reviewed by Walter Zürn and one anonymous referee.

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Short summary

Tides from the Moon and Sun change the force of gravity. Pendulum clocks that use pendula are affected by this, but the resulting time errors are less than a millisecond over a day. These errors were measured by a few precision pendulum clocks between 1929 (the first data showing tidal gravity signals) and 1985. This paper shows the original results of each measurement and also compares these with simulations using modern tidal models.

Tides from the Moon and Sun change the force of gravity. Pendulum clocks that use pendula are...

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