This note has a closer look at the relation between conservation laws and symmetries. As an example it derives the law of conservation of angular momentum directly from the rotational symmetry of physics. It then briefly explains how the arguments carry over to other conservation laws like linear momentum and parity. A simple example of a local gauge symmetry is also given. The final subsection has a few remarks about the symmetry of physics with respect to time shifts.
The mathematician Weyl gave a simple definition of a symmetry. A symmetry exists if you do something and it does not make a difference. A circular cylinder is an axially symmetric object because if you rotate it around its axis over some arbitrary angle, it still looks exactly the same. However, this note is not concerned with symmetries of objects, but of physics. That are symmetries where you do something, like place a system of particles at a different position or angle, and the physics stays the same. The system of particles itself does not necessarily need to be symmetric here.
As an example, this subsection and the next ones will explore one particular symmetry and its conservation law. The symmetry is that the physics is the same if a system of particles is placed under a different angle in otherwise empty space. There are no preferred directions in empty space. The angle that you place a system under does not make a difference. The corresponding conservation law will turn out to be conservation of angular momentum.
First a couple of clarifications. Empty space should really be understood to mean that there are no external effects on the system. A hydrogen atom in a vacuum container on earth is effectively in empty space. Or at least it is as far as its electronic structure is concerned. The energies associated with the gravity of earth and with collisions with the walls of the vacuum container are negligible. Atomic nuclei are normally effectively in empty space because the energies to excite them are so large compared to electronic energies. As a macroscopic example, to study the internal motion of the solar system the rest of the galaxy can presumably safely be ignored. Then the solar system too can be considered to be in empty space.
Further, placing a system under a different angle may be somewhat awkward. Don’t burn your fingers on that hot sun when placing the solar system under a different angle. And there always seems to be a vague suspicion that you will change something nontrivially by placing the system under a different angle.
There is a different, better, way. Note that you will always need a coordinate system to describe the evolution of the system of particles mathematically. Instead of putting the system of particles under an different angle, you can put that coordinate system under a different angle. It has the same effect. In empty space there is no reference direction to say which one got rotated, the particle system or the coordinate system. And rotating the coordinate system leaves the system truly untouched. That is why the view that the coordinate system gets rotated is called the “passive view.” The view that the system itself gets rotated is called the “active view.”
![]() |
Figure A.7 shows graphically what happens to the
position coordinates of a particle if the coordinate system gets
rotated. The original coordinate system is indicated by primes. The
-
produces a
new coordinate system indicated without primes. In terms of spherical
coordinates, the radial position
of the particle does not change.
And neither does the “polar” angle
.
does change. As the figure
shows, the relation between the azimuthal angles is
However, it must still be applied to the description of the physics.
And in quantum mechanics, the physics is described by a wave function
that depends on the position coordinates of the particles;
Physically absolutely nothing changes if the coordinate system is
rotated. So the values
of the wave function in the
rotated coordinate system are exactly the same as the values
in the original coordinate system. But the particle coordinates
corresponding to these values do change:
Mathematically, changes in functions are most conveniently written in
terms of an appropriate operator, chapter 2.4. The
operator here is called the “generator of rotations around the
-
.
to
the azimuthal angles of the function. By definition:
So far, this is all mathematics. The above expression applies whether
or not there is symmetry with respect to rotations. It even applies
whether or not
is a wave function.
The next question is what it means in terms of physics that empty
space has no preferred directions. According to quantum mechanics,
the Schrödinger equation describes the physics. It says that the
time derivative of the wave function can be found as
In particular, consider the two coordinate systems of the previous
subsection. The second system differed from the first by a rotation
over an arbitrary angle
around the
-
A couple of very basic examples can make this more concrete. Consider
the electronic structure of the hydrogen atom as analyzed in chapter
4.3. The electron was not in empty space in that
analysis. It was around a proton, which was assumed to be at rest at
the origin. However, the electric field of the proton has no
preferred direction either. (Proton spin was ignored). Therefore the
current analysis does apply to the electron of the hydrogen
atom. In terms of Cartesian coordinates, the Hamiltonian in the
original
coordinate system is
As a second example, consider the analysis of the complete hydrogen
atom as described in addendum {A.5}. The complete
atom was assumed to be in empty space; there were no external effects
on the atom included. The analysis still ignored all relativistic
effects, including the electron and proton spins. However, it did
include the motion of the proton. That meant that the kinetic energy
of the proton had to be added to the Hamiltonian. But that too is a
Laplacian, now in terms of the proton coordinates
.
The equality of the Hamiltonians in the original and rotated
coordinate systems has a consequence. It leads to a mathematical
requirement for the operator
of the previous subsection
that describes the effect of a coordinate system rotation on wave
functions. This operator must commute with the Hamiltonian:
This observation can be inverted to define a symmetry of physics in general:
A symmetry of physics is described by a unitary operator that commutes with the Hamiltonian.If an operator commutes with the Hamiltonian, then the same Hamiltonian applies in the changed coordinate system. So there is no physical difference in how systems evolve between the two coordinate systems.
The qualification “unitary” means that the operator should not change the magnitude of the wave function. The wave function should remain normalized. It does for the transformations of interest in this note, like rotations of the coordinate system, shifts of the coordinate system, time shifts, and spatial coordinate inversions. All of these transformations are unitary. Like Hermitian operators, unitary operators have a complete set of orthonormal eigenfunctions. However, the eigenvalues are normally not real numbers.
For those who wonder, time reversal is somewhat of a special case. To
understand the difficulty, consider first the operation “take
the complex conjugate of the wave function.” This operator
preserves the magnitude of the wave function. And it commutes with
the Hamiltonian, assuming a basic real Hamiltonian. But taking
complex conjugate is not a linear operator. For a linear operator
.
![]()
.
and
.
and
). However, taking complex conjugate changes inner
products into their complex conjugates. Operators that do that are
called “antiunitary.” So taking complex conjugate is both antilinear
and antiunitary. (Of course, in normal language it is neither. The
appropriate terms would have been conjugate-linear and
conjugate-unitary. But if you got this far in this book, you know how
much chance appropriate terms have of being used in physics.)
Now the effect of time-reversal on wave functions turns out to be
antilinear and antiunitary too, [47, p. 76]. One simple
way to think about it is that a straightforward time reversal would
change
into
.
The definition of a symmetry as an operator that commutes with the
Hamiltonian may seem abstract. But it has a less abstract
consequence. It implies that the eigenfunctions of the symmetry
operation can be taken to be also eigenfunctions of the Hamiltonian,
{D.18}. And, as chapter 7.1.4 discussed, the
eigenfunctions of the Hamiltonian are stationary. They change in time
by a mere scalar factor
of magnitude 1 that does
not change their physical properties.
The fact that the eigenfunctions do not change is responsible for the
conservation law. Consider what a conservation law really means. It
means that there is some number that does not change in time. For
example, conservation of angular momentum in the
-
-
And if the system of particles is described by an eigenfunction of the
symmetry operator, then there is indeed a number that does not change:
the eigenvalue of that eigenfunction. The scalar factor
changes the eigenfunction, but not the eigenvalue
that would be produced by applying the symmetry operator at different
times. The eigenvalue can therefore be looked upon as a specific
value of some conserved quantity. In those terms, if the state of the
system is given by a different eigenfunction, with a different
eigenvalue, it has a different value for the conserved quantity.
The eigenvalues of a symmetry of physics describe the possible values of a conserved quantity.
Of course, the system of particles might not be described by a single eigenfunction of the symmetry operator. It might be a mixture of eigenfunctions, with different eigenvalues. But that merely means that there is quantum mechanical uncertainty in the conserved quantity. That is just like there may be uncertainty in energy. Even if there is uncertainty, still the mixture of eigenvalues does not change with time. Each eigenfunction is still stationary. Therefore the probability of getting a given value for the conserved quantity does not change with time. In particular, neither the expectation value of the conserved quantity, nor the amount of uncertainty in it changes with time.
The eigenvalues of a symmetry operator may require some cleaning up.
They may not directly give the conserved quantity in the desired form.
Consider for example the eigenvalues of the rotation operator
discussed in the previous subsections. You would surely
expect a conserved quantity of a system to be a real quantity. But
the eigenvalues of
are in general complex numbers.
The one thing that can be said about the eigenvalues is that they are
always of magnitude 1. Otherwise an eigenfunction would change in
magnitude during the rotation. But a function does not change in
magnitude if it is merely viewed under a different angle. And if the
eigenvalues are of magnitude 1, then the Euler formula
(2.5) implies that they can always be written in the form
But although
is real and conserved, still it is not the
desired conserved quantity. Consider the possibility that you perform
another rotation of the axis system. Each rotation multiplies the
eigenfunction by a factor
for a total of
.
,
.
and
are
conserved. If
is conserved, then so is
;
is proportional to
,
The constant
is the desired conserved quantity. For historical
reasons it is called the “magnetic quantum number.”
Unfortunately, long before quantum mechanics, classical physics had
already figured out that something was preserved. It called that
quantity the “angular momentum”
.
But the magnetic quantum number is more fundamental. Its possible
values are pure integers, unlike those of angular momentum. To see
why, note that in terms of
,
are of the form
It may be interesting to see how all this works out for the two
examples mentioned in the previous subsection. The first example was the
electron in a hydrogen atom where the proton is assumed to be at rest
at the origin. Chapter 4.3 found the electron energy
eigenfunctions in the form
The second example was the complete hydrogen atom in empty space. In
addendum {A.5}, the energy eigenfunctions were found in
the form
As a final step, it is desirable to formulate a nicer operator for
angular momentum. The rotation operators
are far from
perfect. One problem is that there are infinitely many of them, one
for every angle
.
being the same as two rotations over an angle
.
If you define a rotation operator over a very small angle, call it
,
by just applying
sufficiently many
times. To make this approximation exact, you need to make
infinitesimally small. But when
becomes
zero,
would become just 1. You have lost the
nicer operator that you want by going to the extreme. The trick to
avoid this is to subtract the limiting operator 1, and in addition, to
avoid that the resulting operator then becomes zero, you must also
divide by
.
Now consider what this operator really means for a single particle
with no spin:
You can go one better still, because the eigenvalues of the operator
just defined are
The angular momentum operator of a general system can be defined
using the same scale factor:
Consider now what happens if the angular operator
as defined
above is applied to the wave function of a system of multiple
particles, still without spin. It produces
Of course, even if the complete system has definite angular
momentum, the individual particles may not. A particle numbered
has definite angular momentum
if
Now that the angular momentum operator has been defined, the generator
of rotations
can be identified in terms of it. It turns
out to be
![]() |
(A.77) |
Now consider the generator of rotations in terms of the individual
particles. Since
is the sum of the angular momenta of the
individual particles,
How about spin? The normal angular momentum discussed so far suggests
its true meaning. If a particle
has definite spin angular
momentum in the
-
,
when you rotate the axis system over an angle
.
But there is something curious here. If the axis system is rotated
over an angle
,
1 as long
as
is an integer, (2.5). But for fermions the spin
angular momentum
in a given direction is half-integer, and
1
and is
back in its original position. That is true even if there is
uncertainty in the spin angular momentum. For example, the wave
function of a fermion with spin
can be written as, chapter
5.5.1,
Now the sign of the wave function does not make a difference for the
observed physics. But it is still somewhat unsettling to see that on
the level of the wave function, nature is only the same when the
coordinate system is rotated over
instead of
.
(Some books now raise the question why the orbital angular momentum functions could not do the same thing. Why could the quantum number of orbital angular momentum not be half-integer too? But of course, it is easy to see why not. If the spatial wave function would be multiple valued, then the momentum operators would produce infinite momentum. You would have to postulate arbitrarily that the derivatives of the wave function at a point only involve wave function values of a single branch. Half-integer spin does not have the same problem; for a given orientation of the coordinate system, the opposite wave function is not accessible by merely changing position.)
The previous subsections derived conservation of angular momentum from the symmetry of physics with respect to rotations. Similar arguments may be used to derive other conservation laws. This subsection briefly outlines how.
Conservation of linear momentum can be derived from the symmetry of
physics with respect to translations. The derivation is completely
analogous to the angular momentum case. The translation operator
shifts the coordinate system over a distance
in
the
-
It may again be interesting to see how that works out for the two
example systems introduced earlier. The first example was the
electron in a hydrogen atom. In that example it is assumed that
the proton is fixed at the origin. The energy eigenfunctions for
the electron then were of the form
However, the physics of the complete hydrogen atom as described in
addendum {A.5} is independent of coordinate shifts. A
suitable choice of energy eigenfunctions in this context is
The derivation of linear momentum can be extended to conduction
electrons in crystalline solids. In that case, the physics of the
conduction electrons is unchanged if the coordinate system is
translated over a crystal period
.
-
.
must be the crystal period, or an integer multiple of
it. Therefore, the operator
is not useful; the symmetry does
not continue to apply in the limit
.
The conserved quantity in this case is just the
eigenvalue of
.
and the
corresponding crystal momentum
.
that differ by a whole multiple of ![]()
![]()
produce the same
eigenvalue. But Bloch waves have the same indeterminacy in their
value of
anyway. In fact, Bloch waves are eigenfunctions of
as well as energy eigenfunctions.
One consequence of the indeterminacy in
is an increased number
of possible electromagnetic transitions. Typical electromagnetic
radiation has a wave length that is large compared to the atomic
spacing. Essentially the electromagnetic field is the same from one
atom to the next. That means that it has negligible crystal momentum,
using the smallest of the possible values of
as measure.
Therefore the radiation cannot change the conserved eigenvalue
.
values
in some “extended zone scheme,” chapter 6.22.4.
As long as the two
values differ by a whole multiple of
![]()
![]()
,
does not
change. In that case there is no violation of the conservation law in
the transition. The ambiguity in
values may be eliminated by
switching to a “reduced zone scheme” description,
chapter 6.22.4.
The time shift operator
shifts the time coordinate over an
interval
.
| (A.79) |
Usually, nature is not just symmetric under rotating or translating
it, but also under mirroring it. A transformation that creates a
mirror image of a given system is called a parity transformation. The
mathematically cleanest way to do it is to invert the direction of
each of the three Cartesian axes. That is called spatial inversion.
Physically it is equivalent to mirroring the system using some mirror
passing through the origin, and then rotating the system
![]()
(In a strictly two-dimensional system, spatial inversion does not work,
since the rotation would take the system into the third dimension. In
that case, mirroring can be achieved by replacing just
by ![]()
![]()
-
by ![]()
![]()
by ![]()
![]()
The analysis of the conservation law corresponding to spatial
inversion proceeds much like the one for angular momentum. One
difference is that applying the spatial inversion operator a second
time turns ![]()
![]()
.
1
| (A.80) |
In a system, the
parity eigenvalues of the individual particles
multiply together. That is just like how the eigenvalues of the
generator of rotation
multiply together for angular
momentum. Any particle with even parity has no effect on the system
parity; it multiples the total eigenvalue by 1. On the other hand,
each particle with odd parity flips over the total parity from odd to
even or vice-versa; it multiplies the total eigenvalue by
1
Modern quantum theories are build upon so-called “gauge symmetries.” This subsection gives a simple introduction to some of the ideas.
Consider classical electrostatics. The force on charged particles is
the product of the charge of the particle times the so-called electric
field
.
.
is commonly known as the “voltage” in
electrical applications. Now it too has a symmetry: adding some
arbitrary constant, call it
,
does not make a
difference. Only differences in voltage can be observed
physically. That is a very simple example of a gauge symmetry, a
symmetry in an unobservable field, here the potential
.
Note that this symmetry does not involve the gauges used to measure voltages in any way. Instead it is a reference point symmetry; it does not make a difference what voltage you want to declare to be zero. It is conventional to take the earth as the reference voltage, but that is a completely arbitrary choice. So the term “gauge symmetry” is misleading, like many other terms in physics. A symmetry in a unobservable quantity should of course simply have been called an unobservable symmetry.
There is a relationship between this gauge symmetry in
and
charge conservation. Suppose that, say, a few photons create an
electron and an antineutrino. That can satisfy conservation of
angular momentum and of lepton number, but it would violate charge
conservation. Photons have no charge, and neither have neutrinos. So
the negative charge ![]()
![]()
The problem is that in electrostatics an electron has an electrostatic
energy
.
.
at the point of pair creation has been determined. Not just
a difference in
values between different points. And that
would mean that the value of the constant
would be fixed. So
nature would not really have the gauge symmetry that a constant in the
potential is arbitrary.
Conversely, if the gauge symmetry of the potential is fundamental to
nature, creation of lone charges must be impossible. Each negatively
charged electron that is created must be accompanied by a positively
charged particle so that the net charge that is created is zero. In
electron-positron pair creation, the positive charge
of the
positron makes the net charge that is created zero. Similarly, in
beta decay, an uncharged neutron creates an electron-antineutrino pair
with charge ![]()
,
.
You might of course wonder whether an electrostatic energy
contribution
is really needed to create an electron. It
is because of energy conservation. Otherwise there would be a problem
if an electron-antineutrino pair was created at a location P and
disintegrated again at a different location Q. The electron would
pick up a kinetic energy
while
traveling from P to Q. Without electrostatic contributions to the
electron creation and annihilation energies, that kinetic energy would
make the photons produced by the pair annihilation more energetic than
those destroyed in the pair creation. So the complete process would
create additional photon energy out of nothing.
The gauge symmetry takes on a much more profound meaning in quantum
mechanics. One reason is that the Hamiltonian is based on the
potential, not on the electric field itself. To appreciate the full
impact, consider electrodynamics instead of just electrostatics. In
electrodynamics, a charged particle does not just experience an
electric field
but also a magnetic field
.
in addition to the scalar potential
.
The gauge property now becomes more general. The constant
that
can be added to
in electrostatics no longer needs to be
constant. Instead, it can be taken to be the time-derivative of any
arbitrary function
.
.
However, the wave function computed using the potentials
and
is different from the one computed using
and
.
| (A.81) |
To understand what a stunning result that is, recall the physical
interpretation of the wave function. According to Born, the square
magnitude of the wave function
determines the probability
per unit volume of finding the electron at a given location. But the
wave function is a complex number; it can always be written in the
form
As noted earlier, a symmetry means that you can do something and it
does not make a difference. Since
can be chosen completely
arbitrary, varying with both location and time, this is a very strong
symmetry. Zee writes, (Quantum Field Theory in a Nutshell, 2003,
p. 135): "The modern philosophy is to look at [the equations of
quantum electrodynamics] as a result of [the gauge symmetry above].
If we want to construct a gauge-invariant relativistic field theory
involving a spin
and a spin 1 field, then we are forced to
quantum electrodynamics."
Geometrically, a complex number like the wave function can be shown in
a two-dimensional complex plane in which the real and imaginary parts
of the number form the axes. Multiplying the number by a factor
corresponds to rotating it over an angle
![]()
![]()
around the origin in that plane. In those terms, the
wave function can be rotated over an arbitrary, varying, angle in the
complex plane and it still satisfies the Schrödinger equation.
For a relatively accessible derivation how the gauge invariance
produces quantum electrodynamics, see [23, pp. 358ff].
To make some sense out of it, chapter 1.2.5 gives a brief
inroduction to relativistic index notation, chapter 12.12 to
the Dirac equation and its matrices, addendum {A.1} to
Lagrangians, and {A.21} to photon wave functions. The
are derivatives of this wave function,
[23, p. 239].
It is not quite obvious that the evolution of a physical system in empty space is the same regardless of the time that it is started. It is certainly not as obvious as the assumption that changes in spatial position do not make a difference. Cosmology does not show any evidence for a fundamental difference between different locations in space. For each spatial location, others just like it seem to exist elsewhere. But different cosmological times do show a major physical distinction. They differ in how much later they are than the time of the creation of the universe as we know it. The universe is expanding. Spatial distances between galaxies are increasing. It is believed with quite a lot of confidence that the universe started out extremely concentrated and hot at a “Big Bang” about 15 billion years ago.
Consider the cosmic background radiation. It has cooled down greatly since the universe became transparent to it. The expansion stretched the wave length of the photons of the radiation. That made them less energetic. You can look upon that as a violation of energy conservation due to the expansion of the universe.
Alternatively, you could explain the discrepancy away by assuming that the missing energy goes into potential energy of expansion of the universe. However, whether this “potential energy” is anything better than a different name for “energy that got lost” is another question. Potential energy is normally energy that is lost but can be fully recovered. The potential energy of expansion of the universe cannot be recovered. At least not on a global scale. You cannot stop the expansion of the universe.
And a lack of exact energy conservation may not be such a bad thing for physical theories. Failure of energy conservation in the early universe could provide a possible way of explaining how the universe got all that energy in the first place.
In any case, for practical purposes nontrivial effects of time shifts seem to be negligible in the current universe. When astronomy looks at far-away clusters of galaxies, it sees them as they were billions of years ago. That is because the light that they emit takes billions of years to reach us. And while these galaxies look different from the current ones nearby, there is no evident difference in their basic laws of physics. Also, gravity is an extremely small effect in most other physics. And normal time variations are negligible compared to the age of the universe. Despite the Big Bang, conservation of energy remains one of the pillars on which physics is build.