West Coast Tide Tables
West Coast tide information obtained from the SA Navy Hydrographic Office
Tides are the rise and fall of sea levels caused by the combined effects of the rotation of the Earth and the gravitational forces exerted by the Moon and the Sun. The tides occur with a period of approximately 12 and a half hours and are influenced by the shape of the near-shore bottom.
Most coastal areas experience two daily high (and two low) tides. This is because at the point right "under" the Moon (the sub-lunar point), the water is at its closest to the Moon; so it experiences stronger gravity and rises. On the opposite side of the Earth, the antipodal point, the water is at its farthest from the moon; so it is pulled less. As the Earth moves more toward the Moon than the water does—causing that water to "rise" (relative to the Earth) as well. In between, the force on the water is diagonal or transverse to the sub-lunar/antipodal axis (and always towards that axis), resulting in low tide.
Tide prediction is important for coastal navigation. The intertidal zone, the strip of seashore that high tide submerges and low tide exposes, is an important ecological product of ocean tides.
While tides are usually the largest source of short-term sea-level fluctuations, sea levels are also subject to forces such as wind and barometric pressure changes, resulting in storm surges, especially in shallow seas and near coasts.
Tidal phenomena are not limited to the oceans, but can occur in other systems whenever a gravitational field that varies in time and space is present. For example, the solid part of the Earth is affected by tides.
Tide changes proceed via the following stages:
* Over several hours sea level rises, covering the intertidal zone,
Tides produce oscillating currents known as tidal streams. The moment that the tidal current ceases is called slack water or slack tide. Then the tide reverses direction and is said to be turning. Slack water usually occurs near high water and low water. But there are locations where the moments of slack tide differ significantly from those of high and low water.
Tides are most commonly semidiurnal (two high waters and two low waters each day), or diurnal (one tidal cycle per day). The two high waters on a given day are typically not the same height (the daily inequality); these are the higher high water and the lower high water in tide tables. Similarly, the two low waters each day are the higher low water and the lower low water. The daily inequality is not consistent and is generally small when the Moon is over the equator.[6
Tidal changes are the net result of multiple influences that act over varying periods. These influences are called tidal constituents.
Tides vary on timescales ranging from hours to years. To make accurate
records tide gauges at fixed stations measure the water level over time.
The gauges ignore variations caused by waves with periods shorter than
minutes. These data are compared to the reference (or datum) level usually
called mean sea level.
In most locations, the largest constituent is the "principal lunar
semidiurnal", also known as the M2 (or M2) tidal constituent. Its
period is about 12 hours and 25.2 minutes, exactly half a tidal lunar
day, which is the average time separating one lunar zenith from the
next, and thus is the time required for the Earth to rotate once relative
to the Moon. This is the constituent tracked by simple tide clocks.
The lunar day is longer than the earth day because the Moon orbits in
the same direction the Earth spins. Compare this to the minute hand
on a watch crossing the hour hand at 12:00 and then again at about 1:05
(not at 1:00).
The semidiurnal tidal range (the difference in height between high and low waters over about a half day) varies in a two-week cycle. Around new and full moon when the Sun, Moon and Earth form a line (a condition known as syzygy), the tidal force due to the Sun reinforces that due to the Moon. The tide's range is then at its maximum: this is called the spring tide, or just springs. It is not named after the season but, like that word, derives from an earlier meaning of "jump, burst forth, rise" as in a natural spring. When the Moon is at first quarter or third quarter, the Sun and Moon are separated by 90° when viewed from the Earth, and the solar gravitational force partially cancels the Moon's. At these points in the lunar cycle, the tide's range is at its minimum: this is called the neap tide, or neaps (a word of uncertain origin). Spring tides result in high waters that are higher than average, low waters that are lower than average, slack water time that is shorter than average and stronger tidal currents than average. Neaps result in less extreme tidal conditions. There is about a seven day interval between springs and neaps.
The changing distance separating the Moon and Earth also affects tide
heights. When the Moon is at perigee the range increases, and when it
is at apogee the range shrinks. Every 7½ lunations (the full
cycle from full moon to new to full), perigee coincides with either
a new or full moon causing perigean spring tides with the largest tidal
range. If a storm happens to be moving onshore at this time, the consequences
(property damage, etc.) can be especially severe.
When there are two high tides each day but with different heights (and
two low tides also of different heights), the pattern is called a mixed
The shape of the shoreline and the ocean floor change the way that tides propagate, so there is no simple, general rule for predicting the time of high water from the Moon's position in the sky. Coastal characteristics such as underwater bathymetry and coastline shape mean that individual location characteristics affect tide forecasting; actual high water time and height may differ from model predictions due to the coastal morphology's effects on tidal flow. However, for a given location the relationship between lunar altitude and the time of high or low tide (the lunitidal interval) is relatively constant and predictable, as is the time of high or low tide relative to other points on the same coast. For example, the high tide at Norfolk, Virginia predictably occurs approximately two and a half hours before the moon passes directly overhead.
Land masses and ocean basins act as barriers against water moving freely
around the globe, and their varied shapes and sizes affect the size
of tidal frequencies. As a result, tidal patterns vary. For example,
in the U.S., the East coast has predominantly semi-diurnal tides, as
do Europe's Atlantic coasts, while the West coast predominantly has
Factors include gravitational effects due to the Sun, the obliquity (tilt) of the Earth's equator and rotational axis, the inclination of the plane of the lunar orbit and the elliptical shape of the orbits of the Moon and the Earth.
Variations with periods of less than half a day are called harmonic
constituents. Conversely, long period constituents cycle over days,
months, or years.
Because the M2 tidal constituent dominates in most locations, the stage or phase of a tide, denoted by the time in hours after high water is a useful concept. Tidal stage is also measured in degrees, with 360° per tidal cycle. Lines of constant tidal phase are called cotidal lines, analogous to lines on topographical maps. High water is reached simultaneously along the cotidal lines extending from the coast out into the ocean, and cotidal lines (and hence tidal phases) advance along the coast. Semidiurnal and long phase constituents are measured from high water, diurnal from maximum flood tide. This and the discussion that follows is precisely true only for a single tidal constituent.
For an ocean in the shape of a circular basin enclosed by a coastline, the cotidal lines point radially inward and must eventually meet at a common point, the amphidromic point. The amphidromic point is at once cotidal with high and low waters, which is satisfied by zero tidal motion. (The rare exception occurs when the tide encircles an island, as it does around New Zealand and Madagascar.) Tidal motion generally lessens moving away from continental coasts, so that crossing the cotidal lines are contours of constant amplitude (half the distance between high and low water) which decrease to zero at the amphidromic point. For a semidiurnal tide the amphidromic point can be thought of roughly like the center of a clock face, with the hour hand pointing in the direction of the high water cotidal line, which is directly opposite the low water cotidal line. High water rotates about the amphidromic point once every 12 hours in the direction of rising cotidal lines, and away from ebbing cotidal lines. This rotation is generally clockwise in the southern hemisphere and counterclockwise in the northern hemisphere, and is caused by the Coriolis effect. The difference of cotidal phase from the phase of a reference tide is the epoch. The reference tide is the hypothetical constituent equilibrium tide on a landless Earth measured at 0° longitude, the Greenwich meridian.
In the North Atlantic, because the cotidal lines circulate counterclockwise around the amphidromic point, the high tide passes New York harbor approximately an hour ahead of Norfolk harbor. South of Cape Hatteras the tidal forces are more complex, and cannot be predicted reliably based on the North Atlantic cotidal lines.
History of tidal physics
Isaac Newton laid the foundations of scientific tidal studies with his mathematical explanation of tide-generating forces in the Philosophiae Naturalis Principia Mathematica (1687). Newton first applied the theory of universal gravitation to account for the tides as due to the lunar and solar attractions, offering an initial theory of the tide-generating force. Newton and others before Pierre-Simon Laplace worked with an equilibrium theory, largely concerned with an approximation that describes the tides that would occur in a non-inertial ocean evenly covering the whole Earth. The tide-generating force (or its corresponding potential) is still relevant to tidal theory, but as an intermediate quantity rather than as a final result; theory has to consider also the Earth's dynamic tidal response to the force, a response that is influenced by bathymetry, Earth's rotation, and other factors.
In 1740, the Académie Royale des Sciences in Paris offered a prize for the best theoretical essay on tides. Daniel Bernoulli, Leonhard Euler, Colin Maclaurin and Antoine Cavalleri shared the prize.
Maclaurin used Newton’s theory to show that a smooth sphere covered by a sufficiently deep ocean under the tidal force of a single deforming body is a prolate spheroid (essentially a three dimensional oval) with major axis directed toward the deforming body. Maclaurin was the first to write about the Earth's rotational effects on motion. Euler realized that the tidal force's horizontal component (more than the vertical) drives the tide. In 1744 Jean le Rond d'Alembert studied tidal equations for the atmosphere which did not include rotation.
Pierre-Simon Laplace formulated a system of partial differential equations relating the ocean's horizontal flow to its surface height, the first major dynamic theory for water tides. The Laplace tidal equations are still in use today. William Thomson, 1st Baron Kelvin, rewrote Laplace's equations in terms of vorticity which allowed for solutions describing tidally-driven coastally-trapped waves, known as Kelvin waves.  
Others including Kelvin and Henri Poincare further developed Laplace's
theory. Based on these developments and the lunar theory of E W Brown,
Arthur Thomas Doodson developed and published in 1921 the first
modern development of the tide-generating potential in harmonic form:
Doodson distinguished 388 tidal frequencies. Some of his methods
remain in use.
The tidal force produced by a massive object (Moon, hereafter) on a
small particle located on or in an extensive body (Earth, hereafter)
is the vector difference between the gravitational force exerted by
the Moon on the particle, and the gravitational force that would be
exerted on the particle if it were located at the Earth's center of
mass. Thus, the tidal force depends not on the strength of the lunar
gravitational field, but on its gradient (which falls off approximately
as the inverse cube of the distance to the originating gravitational
body).  The solar gravitational force on the Earth is on average
179 times stronger than the lunar, but because the Sun is on average
389 times farther from the Earth, its field gradient is weaker. The
solar tidal force is 46% as large as the lunar. More precisely,
the lunar tidal acceleration (along the Moon-Earth axis, at the Earth's
surface) is about 1.1 × 10-7 g, while the solar tidal acceleration
(along the Sun-Earth axis, at the Earth's surface) is about 0.52 ×
10-7 g, where g is the gravitational acceleration at the Earth's surface.
Venus has the largest effect of the other planets, at 0.000113 times
the solar effect.
Tidal forces can also be analyzed this way: each point of the Earth experiences the Moon's radially decreasing gravity differently; they are subject to the tidal forces of Figure 6, which dominate. Finally, most importantly, only the tidal forces' horizontal components actually tidally accelerate the water particles since there is small resistance. The tidal force on a particle equals about one ten millionth that of Earth's gravitational force.
The ocean's surface is closely approximated by an equipotential surface,
(ignoring ocean currents) commonly referred to as the geoid. Since the
gravitational force is equal to the potential's gradient, there are
no tangential forces on such a surface, and the ocean surface is thus
in gravitational equilibrium. Now consider the effect of massive external
bodies such as the Moon and Sun. These bodies have strong gravitational
fields that diminish with distance in space and which act to alter the
shape of an equipotential surface on the Earth. This deformation has
a fixed spatial orientation relative to the influencing body. The Earth's
rotation relative to this shape causes the daily tidal cycle. Gravitational
forces follow an inverse-square law (force is inversely proportional
to the square of the distance), but tidal forces are inversely proportional
to the cube of the distance. The ocean surface moves to adjust to changing
tidal equipotential, tending to rise when the tidal potential is high,
which occurs on the part of the Earth nearest to and furthest from the
Moon. When the tidal equipotential changes, the ocean surface is no
longer aligned with it, so that the apparent direction of the vertical
shifts. The surface then experiences a down slope, in the direction
that the equipotential has risen.
Ocean depths are much smaller than their horizontal extent. Thus, the response to tidal forcing can be modelled using the Laplace tidal equations which incorporate the following features:
1. The vertical (or radial) velocity is negligible, and there is no
vertical shear—this is a sheet flow.
The boundary conditions dictate no flow across the coastline and free slip at the bottom.
The Coriolis effect steers waves to the right in the northern hemisphere
and to the left in the southern allowing coastally trapped waves. Finally,
a dissipation term can be added which is an analog to viscosity.
The theoretical amplitude of oceanic tides caused by the Moon is about 54 centimetres (21 in) at the highest point, which corresponds to the amplitude that would be reached if the ocean possessed a uniform depth, there were no landmasses, and the Earth were not rotating. The Sun similarly causes tides, of which the theoretical amplitude is about 25 centimetres (9.8 in) (46% of that of the Moon) with a cycle time of 12 hours. At spring tide the two effects add to each other to a theoretical level of 79 centimetres (31 in), while at neap tide the theoretical level is reduced to 29 centimetres (11 in). Since the orbits of the Earth about the Sun, and the Moon about the Earth, are elliptical, tidal amplitudes change somewhat as a result of the varying Earth–Sun and Earth–Moon distances. This causes a variation in the tidal force and theoretical amplitude of about ±18% for the Moon and ±5% for the Sun. If both the Sun and Moon were at their closest positions and aligned at new moon, the theoretical amplitude would reach 93 centimetres (37 in).
Real amplitudes differ considerably, not only because of depth variations
and continental obstacles, but also because wave propagation across
the ocean has a natural period of the same order of magnitude as the
rotation period: if there were no land masses, it would take about 30
hours for a long wavelength surface wave to propagate along the equator
halfway around the Earth (by comparison, the Earth's lithosphere has
a natural period of about 57 minutes).
Earth's tidal oscillations introduce dissipation at an average rate of about 3.75 terawatt. About 98% of this dissipation is by marine tidal movement. Dissipation arises as basin-scale tidal flows drive smaller-scale flows which experience turbulent dissipation. This tidal drag creates torque on the Moon that gradually transfers angular momentum to its orbit, and a gradual increase in Earth–Moon separation. The equal and opposite torque on the Earth correspondingly decreases its rotational velocity. Thus, over geologic time, the Moon recedes from the Earth, at about 3.8 centimetres (1.5 in)/year, lengthening the terrestrial day. Day length has increased by about 2 hours in the last 600 million years. Assuming (as a crude approximation) that the deceleration rate has been constant, this would imply that 70 million years ago, day length was on the order of 1% shorter with about 4 more days per year.
From ancient times, tidal observation and discussion has increased in sophistication, first marking the daily recurrence, then tides' relationship to the Sun and Moon. Pytheas travelled to the British Isles about 325 BC and seems to be the first to have related spring tides to the phase of the Moon.
In the 2nd century BC, the Babylonian astronomer, Seleucus of Seleucia, correctly described the phenomenon of tides in order to support his heliocentric theory. He correctly theorized that tides were caused by the Moon, although he believed that the interaction was mediated by the pneuma. He noted that tides varied in time and strength in different parts of the world. According to Strabo (1.1.9), Seleucus was the first to link tides to the lunar attraction, and that the height of the tides depends on the Moon's position relative to the Sun.
The Naturalis Historia of Pliny the Elder collates many tidal observations, e.g., the spring tides are a few days after (or before) new and full moon and are highest around the equinoxes, though Pliny noted many relationships now regarded as fanciful. In his Geography, Strabo described tides in the Persian Gulf having their greatest range when the Moon was furthest from the plane of the equator. All this despite the relatively small amplitude of Mediterranean basin tides. (The strong currents through the Strait of Messina and between Greece and the island of Euboea through the Euripus puzzled Aristotle). Philostratus discussed tides in Book Five of The Life of Apollonius of Tyana. Philostratus mentions the moon, but attributes tides to "spirits". In Europe around 730 AD, the Venerable Bede described how the rising tide on one coast of the British Isles coincided with the fall on the other and described the time progression of high water along the Northumbrian coast.
In the 9th century, the Arabian earth-scientist, Al-Kindi (Alkindus), wrote a treatise entitled Risala fi l-Illa al-Failali l-Madd wa l-Fazr (Treatise on the Efficient Cause of the Flow and Ebb), in which he presents an argument on tides which "depends on the changes which take place in bodies owing to the rise and fall of temperature." He describes a clear and precise laboratory experiment that proved his argument.
The first tide table in China was recorded in 1056 AD primarily for visitors wishing to see the famous tidal bore in the Qiantang River. The first known British tide table is thought to be that of John, Abbott of Wallingford (d. 1213), based on high water occurring 48 minutes later each day, and three hours earlier at the Thames mouth than upriver at London.
William Thomson (Lord Kelvin) led the first systematic harmonic analysis of tidal records starting in 1867. The main result was the building of a tide-predicting machine using a system of pulleys to add together six harmonic time functions. It was "programmed" by resetting gears and chains to adjust phasing and amplitudes. Similar machines were used until the 1960s.
The first known sea-level record of an entire spring–neap cycle was made in 1831 on the Navy Dock in the Thames Estuary. Many large ports had automatic tide gage stations by 1850.
William Whewell first mapped co-tidal lines ending with a nearly global
chart in 1836. In order to make these maps consistent, he hypothesized
the existence of amphidromes where co-tidal lines meet in the mid-ocean.
These points of no tide were confirmed by measurement in 1840 by Captain
Hewett, RN, from careful soundings in the North Sea.
In most places there is a delay between the phases of the Moon and the effect on the tide. Springs and neaps in the North Sea, for example, are two days behind the new/full Moon and first/third quarter. This is called the tide's age.
The local bathymetry greatly influences the tide's exact time and height at a particular coastal point. There are some extreme cases: the Bay of Fundy, on the east coast of Canada, features the world's largest well-documented tidal ranges, 16 metres (52 ft) because of its shape. Some experts believe Ungava Bay in northern Quebec to have even higher tidal ranges, but it is free of pack ice for only about four months every year, while the Bay of Fundy rarely freezes.
Southampton in the United Kingdom has a double high water caused by the interaction between the region's different tidal harmonics. This is contrary to the popular belief that the flow of water around the Isle of Wight creates two high waters. The Isle of Wight is important, however, since it is responsible for the 'Young Flood Stand', which describes the pause of the incoming tide about three hours after low water.
Because the oscillation modes of the Mediterranean Sea and the Baltic
Sea do not coincide with any significant astronomical forcing period,
the largest tides are close to their narrow connections with the Atlantic
Ocean. Extremely small tides also occur for the same reason in the Gulf
of Mexico and Sea of Japan. On the southern coast of Australia, because
the coast is mainly straight (partly because of the tiny quantities
of runoff flowing from rivers), tidal ranges are equally small.
Isaac Newton's theory of gravitation first enabled an explanation of why there were generally two tides a day, not one, and offered hope for detailed understanding. Although it may seem that tides could be predicted via a sufficiently detailed knowledge of the instantaneous astronomical forcings, the actual tide at a given location is determined by astronomical forces accumulated over many days. Precise results require detailed knowledge of the shape of all the ocean basins—their bathymetry and coastline shape.
Current procedure for analysing tides follows the method of harmonic analysis introduced in the 1860s by William Thomson. It is based on the principle that the astronomical theories of the motions of Sun and Moon determine a large number of component frequencies, and at each frequency there is a component of force tending to produce tidal motion, but that at each place of interest on the Earth, the tides respond at each frequency with an amplitude and phase peculiar to that locality. At each place of interest, the tide heights are therefore measured for a period of time sufficiently long (usually more than a year in the case of a new port not previously studied) to enable the response at each significant tide-generating frequency to be distinguished by analysis, and to extract the tidal constants for a sufficient number of the strongest known components of the astronomical tidal forces to enable practical tide prediction. The tide heights are expected to follow the tidal force, with a constant amplitude and phase delay for each component. Because astronomical frequencies and phases can be calculated with certainty, the tide height at other times can then be predicted once the response to the harmonic components of the astronomical tide-generating forces has been found.
The main patterns in the tides are
* the twice-daily variation
The Highest Astronomical Tide is the perigean spring tide when both the Sun and the Moon are closest to the Earth.
When confronted by a periodically varying function, the standard approach is to employ Fourier series, a form of orthogonal analysis that uses sinusoidal functions as a basis set, having frequencies that are zero, one, two, three, etc. times the frequency of a particular fundamental cycle. These multiples are called harmonics of the fundamental frequency, and the process is termed harmonic analysis. If the basis set of sinusoidal functions suit the behaviour being modelled, relatively few harmonic terms need to be added. Orbital paths are very nearly circular, so sinusoidal variations are suitable for tides.
For the analysis of tide heights, the Fourier series approach has in practice to be made more elaborate than the use of a single frequency and its harmonics. The tidal patterns are decomposed into many sinusoids having many fundamental frequencies, corresponding (as in the lunar theory) to many different combinations of the motions of the Earth, the Moon, and the angles that define the shape and location of their orbits.
For tides, then, harmonic analysis is not limited to harmonics of a single frequency. In other words, the harmonies are multiples of many fundamental frequencies, not just of the fundamental frequency of the simpler Fourier series approach. Their representation as a Fourier series having only one fundamental frequency and its (integer) multiples would require many terms, and would be severely limited in the time-range for which it would be valid.
The study of tide height by harmonic analysis was begun by Laplace, William Thomson (Lord Kelvin), and George Darwin. A.T. Doodson extended their work, introducing the Doodson Number notation to organise the hundreds of resulting terms. This approach has been the international standard ever since, and the complications arise as follows: the tide-raising force is notionally given by sums of several terms. Each term is of the form
A·cos(w·t + p)
where A is the amplitude, w is the angular frequency usually given in degrees per hour corresponding to t measured in hours, and p is the phase offset with regard to the astronomical state at time t = 0 . There is one term for the Moon and a second term for the Sun. The phase p of the first harmonic for the Moon term is called the lunitidal interval or high water interval. The next step is to accommodate the harmonic terms due to the elliptical shape of the orbits. Accordingly, the value of A is not a constant but also varying with time, slightly, about some average figure. Replace it then by A(t) where A is another sinusoid, similar to the cycles and epicycles of Ptolemaic theory. Accordingly,
A(t) = A·(1 + Aa·cos(wa·t + pa)) ,
which is to say an average value A with a sinusoidal variation about it of magnitude Aa , with frequency wa and phase pa . Thus the simple term is now the product of two cosine factors:
A·[1 + Aa·cos(wa + pa)]·cos(w·t + p)
Given that for any x and y
cos(x)·cos(y) = ½·cos( x + y ) + ½·cos( x–y ) ,
it is clear that a compound term involving the product of two cosine
terms each with their own frequency is the same as three simple cosine
terms that are to be added at the original frequency and also at frequencies
which are the sum and difference of the two frequencies of the product
term. (Three, not two terms, since the whole expression is (1 + cos(x))·cos(y)
.) Consider further that the tidal force on a location depends also
on whether the Moon (or the Sun) is above or below the plane of the
equator, and that these attributes have their own periods also incommensurable
with a day and a month, and it is clear that many combinations result.
With a careful choice of the basic astronomical frequencies, the Doodson
Number annotates the particular additions and differences to form the
frequency of each simple cosine term.
Remember that astronomical tides do not include weather effects. Also, changes to local conditions (sandbank movement, dredging harbour mouths, etc.) away from those prevailing at the measurement time affect the tide's actual timing and magnitude. Organisations quoting a "highest astronomical tide" for some location may exaggerate the figure as a safety factor against analytical uncertainties, distance from the nearest measurement point, changes since the last observation time, ground subsidence, etc., to avert liability should an engineering work be overtopped. Special care is needed when assessing the size of a "weather surge" by subtracting the astronomical tide from the observed tide.
Careful Fourier data analysis over a nineteen-year period (the National Tidal Datum Epoch in the U.S.) uses frequencies called the tidal harmonic constituents. Nineteen years is preferred because the Earth, Moon and Sun's relative positions repeat almost exactly in the Metonic cycle of 19 years, which is long enough to include the 18.613 year lunar nodal tidal constituent. This analysis can be done using only the knowledge of the forcing period, but without detailed understanding of the mathematical derivation, which means that useful tidal tables have been constructed for centuries. The resulting amplitudes and phases can then be used to predict the expected tides. These are usually dominated by the constituents near 12 hours (the semidiurnal constituents), but there are major constituents near 24 hours (diurnal) as well. Longer term constituents are 14 day or fortnightly, monthly, and semiannual. Semidiurnal tides dominated coastline, but some areas such as the South China Sea and the Gulf of Mexico are primarily diurnal. In the semidiurnal areas, the primary constituents M2 (lunar) and S2 (solar) periods differ slightly, so that the relative phases, and thus the amplitude of the combined tide, change fortnightly (14 day period).
In the M2 plot above, each cotidal line differs by one hour from its neighbors, and the thicker lines show tides in phase with equilibrium at Greenwich. The lines rotate around the amphidromic points counterclockwise in the northern hemisphere so that from Baja California to Alaska and from France to Ireland the M2 tide propagates northward. In the southern hemisphere this direction is clockwise. On the other hand M2 tide propagates counterclockwise around New Zealand, but this is because the islands act as a dam and permit the tides to have different heights on the islands' opposite sides. (The tides do propagate northward on the east side and southward on the west coast, as predicted by theory.)
The exception is at Cook Strait where the tidal currents periodically
link high to low water. This is because cotidal lines 180° around
the amphidromes are in opposite phase, for example high water across
from low water at each end of Cook Strait. Each tidal constituent has
a different pattern of amplitudes, phases, and amphidromic points, so
the M2 patterns cannot be used for other tide components.
Figure 9 shows the common pattern of two daily tidal peaks (the precise cycle time is 12.4206 hours). The two peaks are not equal: the twin tidal bulges beneath the Moon and on the opposite side of the Earth align with the Moon. Bridgeport is north of the equator, so when the Moon is north of the equator also and shining upon Bridgeport, Bridgeport is closer to its maximum tide than approximately twelve hours later when Bridgeport is on the opposite side of the Earth from the Moon and the high tide bulge at Bridgeport's longitude has its maximum south of the equator. Thus the two high tides a day alternate in maximum heights: lower high (just under three feet), higher high (just over three feet), and again. Likewise for the low tides.
Figure 10 shows the spring tide/neap tide cycle in tidal amplitudes as the Moon orbits the Earth from being in line (Sun–Earth–Moon, or Sun–Moon–Earth) when the two main influences combine to give the spring tides, to when the two forces are opposing each other as when the angle Moon–Earth–Sun is close to ninety degrees, producing the neap tides. As the Moon moves around its orbit it changes from north of the equator to south of the equator. The alternation in high tide heights becomes smaller, until they are the same (at the lunar equinox, the Moon is above the equator), then redevelops but with the other polarity, waxing to a maximum difference and then waning again.
Figure 11 shows just over a year's worth of tidal height calculations.
The Sun also cycles from north to south of the equator, while the Earth–Sun
and Earth–Moon distances change on their own cycles. None of the
various cycle periods are commensurate.
The tides' influence on current flow is much more difficult to analyse, and data is much more difficult to collect. A tidal height is a simple number which applies to a wide region simultaneously. A flow has both a magnitude and a direction, both of which can vary substantially with depth and over short distances due to local bathymetry. Also, although a water channel's center is the most useful measuring site, mariners object when current-measuring equipment obstructs waterways. A flow proceeding up a curved channel is the same flow, even though its direction varies continuously along the channel. Surprisingly, flood and ebb flows are often not in opposite directions. Flow direction is determined by the upstream channel's shape, not the downstream channel's shape. Likewise, eddies may form in only one flow direction.
Nevertheless, current analysis is similar to tidal analysis: in the simple case, at a given location the flood flow is in mostly one direction, and the ebb flow in another direction. Flood velocities are given positive sign, and ebb velocities negative sign. Analysis proceeds as though these are tide heights.
In more complex situations, the main ebb and flood flows do not dominate. Instead, the flow direction and magnitude trace an ellipse over a tidal cycle (on a polar plot) instead of along the ebb and flood lines. In this case, analysis might proceed along pairs of directions, with the primary and secondary directions at right angles. An alternative is to treat the tidal flows as complex numbers, as each value has both a magnitude and a direction.
Tide flow information is most commonly seen on nautical charts, presented as a table of flow speeds and bearings at hourly intervals, with separate tables for spring and neap tides. The timing is relative to high water at some harbour where the tidal behaviour is similar in pattern, though it may be far away.
As with tide height predictions, tide flow predictions based only on astronomical factors do not incorporate weather conditions, which can completely change the outcome.
The tidal flow through Cook Strait between the two main islands of New Zealand is particularly interesting, as the tides on each side of the strait are almost exactly out of phase, so that one side's high water is simultaneous with the other's low water. Strong currents result, with almost zero tidal height change in the strait's center. Yet, although the tidal surge normally flows in one direction for six hours and in the reverse direction for six hours, a particular surge might last eight or ten hours with the reverse surge enfeebled. In especially boisterous weather conditions, the reverse surge might be entirely overcome so that the flow continues in the same direction through three or more surge periods.
A further complication for Cook Strait's flow pattern is that the tide at the north side(e.g. at Nelson) follows the common bi-weekly spring–neap tide cycle (as found along the west side of the country), but the south side's tidal pattern has only one cycle per month, as on the east side: Wellington, and Napier.
Figure 12 shows separately the high water and low water height and
time, through November 2007; these are not measured values but instead
are calculated from tidal parameters derived from years-old measurements.
Cook Strait's nautical chart offers tidal current information. For instance
the January 1979 edition for 41°13·9’S 174°29·6’E
(north west of Cape Terawhiti) refers timings to Westport while the
January 2004 issue refers to Wellington. Near Cape Terawhiti in the
middle of Cook Strait the tidal height variation is almost nil while
the tidal current reaches its maximum, especially near the notorious
Karori Rip. Aside from weather effects, the actual currents through
Cook Strait are influenced by the tidal height differences between the
two ends of the strait and as can be seen, only one of the two spring
tides at the north end (Nelson) has a counterpart spring tide at the
south end (Wellington), so the resulting behaviour follows neither reference
Tidal energy can be extracted by two means: inserting a water turbine into a tidal current, or building ponds that release/admit water through a turbine. In the first case, the energy amount is entirely determined by the timing and tidal current magnitude. However, the best currents may be unavailable because the turbines would obstruct ships. In the second, the impoundment dams are expensive to construct, natural water cycles are completely disrupted, ship navigation is disrupted. However, with multiple ponds, power can be generated at chosen times. So far, there are few installed systems for tidal power generation (most famously, La Rance by Saint Malo, France) which faces many difficulties. Aside from environmental issues, simply withstanding corrosion and biological fouling pose engineering challenges.
Tidal power proponents point out that, unlike wind power systems, generation levels can be reliably predicted, save for weather effects. While some generation is possible for most of the tidal cycle, in practice turbines lose efficiency at lower operating rates. Since the power available from a flow is proportional to the cube of the flow speed, the times during which high power generation is possible are brief.
Tidal flows are important for navigation, and significant errors in position occur if they are not accommodated. Tidal heights are also important; for example many rivers and harbours have a shallow "bar" at the entrance which prevents boats with significant draft from entering at low tide.
Until the advent of automated navigation, competence in calculating tidal effects was important to naval officers. The certificate of examination for lieutenants in the Royal Navy once declared that the prospective officer was able to "shift his tides".
Tidal flow timings and velocities appear in tide charts or a tidal stream atlas. Tide charts come in sets. Each chart covers a single hour between one high water and another (they ignore the leftover 24 minutes) and show the average tidal flow for that hour. An arrow on the tidal chart indicates the direction and the average flow speed (usually in knots) for spring and neap tides. If a tide chart is not available, most nautical charts have "tidal diamonds" which relate specific points on the chart to a table giving tidal flow direction and speed.
The standard procedure to counteract tidal effects on navigation is to (1) calculate a "dead reckoning" position (or DR) from travel distance and direction, (2) mark the chart (with a vertical cross like a plus sign) and (3) draw a line from the DR in the tide's direction. The distance the tide moves the boat along this line is computed by the tidal speed, and this gives an "estimated position" or EP (traditionally marked with a dot in a triangle).
Nautical charts display the water's "charted depth" at specific locations with "soundings" and the use of bathymetric contour lines to depict the submerged surface's shape. These depths are relative to a "chart datum", which is typically the water level at the lowest possible astronomical tide (tides may be lower or higher for meteorological reasons) and are therefore the minimum possible water depth during the tidal cycle. "Drying heights" may also be shown on the chart, which are the heights of the exposed seabed at the lowest astronomical tide.
Tide tables list each day's high and low water heights and times. To calculate the actual water depth, add the charted depth to the published tide height. Depth for other times can be derived from tidal curves published for major ports. The rule of twelfths can suffice if an accurate curve is not available. This approximation presumes that the increase in depth in the six hours between low and high water is: first hour — 1/12, second — 2/12, third — 3/12, fourth — 3/12, fifth — 2/12, sixth — 1/12.