Speed and velocity have no meaning without something to reference. If I said we are moving at 230 000
m/s,
your first question should be, "relative to what?". A plane? The Earth? The Sun?

We are moving at 230 000 m/s relative to our galaxy, the Milky Way.

Velocity must be relative to a reference frame. A
reference frame is a point of view from which events are observed.

A train is moving at 40 m/s relative to the train track.

The same train is stationary relative to a passenger on the train.

Each observer only sees motion in others. They see themselves at rest.
Move the mouse vertically to change observers in the animation above.
(note: special relativity isn't included yet in this animation.)

Question: Imagine two cars. One is moving at 15 m/s relative to the Earth and the other at
20 m/s relative to the Earth. How fast are they moving relative to each other?
solution
$$v = 20 \, \mathrm{\tfrac{m}{s}}-15 \, \mathrm{\tfrac{m}{s}}$$
$$v = 5 \, \mathrm{\tfrac{m}{s}}$$

Question: Imagine a boat traveling up a river. The current in the river is 5 m/s
downstream. The boat is moving upstream at 15 m/s relative to the water in the river. How fast is the boat
moving relative to the land?
solution
$$v = 15 \, \mathrm{\tfrac{m}{s}}-5 \, \mathrm{\tfrac{m}{s}}$$
$$v = 10 \, \mathrm{\tfrac{m}{s}}$$

Question: A train moving at 20 m/s makes a sound with its steam whistle.
Sound moves through air at around 343 m/s relative to the air.
How fast would each observer measure the speed of sound?

Observer 1: A person at the train station.

Observer 2: A person at the back of the train.

answer

Observer 1:343 m/s.

The person on the ground measures the speed of sound as normal because they are at rest
relative to the air.

Observer 2:343 m/s + 20 m/s = 363 m/s

The person on the train is moving relative to the air so they will measure the speed of
sound as either higher or lower.

Thought Experiment: Imagine a train moving at half the speed of sound.
Whistles at the front and the back of the train blow at the same time.

Where on the train would a passenger hear the whistles simultaneously?

Where on the ground would an observer hear the whistles simultaneously?

results

A train passenger measures the sound from the front of the train as moving faster, and the sound
from the back as moving slower.

An observer on the ground measures both sound waves moving at the same speed, but the train is
moving to the right.

Both frames of reference agree that the sound waves meet towards the back of the train.

A Constant Speed of Light

Waves are a disruption that propagates through a medium. The speed of a wave is constant and determined by
the medium.
Sound's medium is atoms. Light's medium is electric and magnetic fields.

Light is different from other waves.
It moves faster than any known object, and it is able to propagate through the vacuum of space.
How can a wave exist in seemingly empty space?
Is space filled with a medium? What is the velocity of that medium relative to Earth?

In 1887, scientists Albert A. Michelson and Edward W. Morley developed an experiment
to learn about the relative velocity between the Earth and light's medium, electromagnetic fields.

Michelson and Morley split
a beam of light into two perpendicular paths. These separate beams reflected off mirrors to recombine again
at the splitter.
By looking at the interference pattern of the combined beams, they could tell with a high accuracy if either
path took less time.

They tested at different times of day and year to measure the effect of Earth's relative velocity on the
speed of light.
They always measured a constant speed of light in every direction. Earth's motion had no effect.

$$c = 3 \times 10^8 \, \mathrm{\tfrac{m}{s}} $$

All observers measure the speed of light as the same value even when moving at a relative velocity.

It seems like a constant speed of light for all observers leads to a paradox.
How can two observers moving relative to each other both see the speed of something as the same?

Thought Experiment:
Imagine a train moving at half the speed of light.
Imagine lights on the front and back of the train flash simultaneously for both observers.

Where would a passenger on the train see the lights flash at the same time?

Where would a ground based observer see the lights flash at the same time?

results

The train isn't moving from the passenger's frame of reference. This means they see the light
meet in the middle of the train.

A frame of reference on the ground sees the train moving to the right.
They see the light waves meet closer to the back of the train.

The frames of reference don't agree on the location and timing of events.
This happens when two frames of reference have a relative velocity between them.
These contradictory results indicate there is a problem with our model of physics.

Special Relativity

The Michelson–Morley experiment and a few other experiments indicated that there was a problem with our
understanding of relative velocity and light.

In 1905 Albert Einstein published his answer to the problem. He suggested special relativity as a
modification of the laws of physics to take into account a constant speed of light. Special relativity
suggests that space and time change for different observers in a way that keeps the speed of light constant.

Special relativity is based on two postulates:
1. The laws of physics are the same in all reference frames.
2. Light moves at the same speed for all observers.

Special relativity predicts that observers moving at a relative velocity to each other don't agree on the:

order of events (simultaneity)

passage of time (time dilation)

length of objects (length contraction)

mass of objects (mass–energy equivalence)

Because of the high speeds needed, special relativity is difficult to observe, but so far all tests support the theory to a high
degree of precision.

Here is a relative velocity simulation with time dilation and length contraction. Move the mouse vertically
to change observers.

The doppler effect and a few other quirks of relativity aren't part of this simulation. Try this game or this video for a more accurate experience.

Question: Are the predictions of special relativity 'real' or an 'illusion' that only
affects how an observer sees things?
solution

Effects like time dilation and length contraction have real consequences that all observers can
agree on. Time dilation can produce real differences in the ages of objects. (see twin paradox)

Question: Does special relativity mean time travel might be possible one day?
answer

YES! and no

You can already go forwards in time by just waiting, but you will get old.

If you have a velocity near the speed of light relative to the Earth, you will age slow as the Earth
ages fast. You could use this to see the far future, but right now we don't have a safe way to get a
person up to relativistic speeds.

It is probably impossible to go backwards in time, but the equations don't
completely rule it out.

Thought Experiment: Remember the train paradox?
The ground based frame of reference and the train based frame of reference disagreed on where the
flashes of light met.
Special relativity removes this inconsistency by not letting different frames agree on simultaneity.

It is only possible for the light flashes to be simultaneous for one of the observers.
If the flashes occur at the same time for the train observer, the ground observer will see the flashes
at different times.

Question: What relativistic effects can you observe in the simulation?
answer

simultaneity and length contraction

The trees are narrow from the train's reference frame.
The train is shorter from the ground's reference frame.

Time dilation should also be present, but there isn't a way to see it in the simulation.

Lorentz factor

These equations predict how observers in two non-accelerating reference frames can disagree on space and
time if they have a relative velocity.

$$ \Delta t = \gamma \Delta t_0 \quad \quad \quad \quad L = \frac{L_0}{\gamma}$$

Before we can solve these equations, we need to calculate the Lorentz factor, written as Ɣ
(gamma).
The Lorentz factor is used in special relativity equations to scale how different reference frames measure
space and time.

As the relative velocity approaches the speed of light, extreme effects like: time dilation, mass
increase, and length contraction hinder acceleration. This means that the speed of light is also the
maximum relative speed for any object.

At a low relative velocity, the effects of special relativity aren't noticeable because the Lorentz factor is
one. As the relative speed approaches the speed of light, the Lorentz factor increases towards infinity.

Time Dilation

Time dilation is amazing because it disagrees with our natural intuition. Be careful when solving these
problems. Keep a clear idea of the observer and their velocity relative to the events.

derivation of time dilation

To understand where the time dilation equation comes from we will explore a hypothetical
situation. Imagine light
clocks that work by firing light at a mirror and measuring the time for the light to return.
Each light clock's path is marked in blue.

On the left, a light clock is not moving relative to the observer.

\( \Delta t_0 \) is the time for one tick of the light clock at rest.

On the right, a light clock is moving at v relative to the observer.

\( \Delta t \) is the time for one tick of the light clock at velocity v.

First we apply \( v= \frac{\Delta x}{\Delta t}\) to each side of the triangle highlighted in red.

$$ c = \frac{2D}{\Delta t } \quad \quad c = \frac{2L}{\Delta t_0 } \quad \quad v = \frac{2W}{\Delta t}$$
$$D = \tfrac{1}{2} c \Delta t \quad L = \tfrac{1}{2} c \Delta t_0 \quad W = \tfrac{1}{2} v \Delta t $$

\(\Delta t\) = elapsed time for an observer in a frame of reference where the events occur in
different locations

\(\Delta t_0\) = elapsed time for an observer in a frame of reference where the events occur in
the same location, proper time

\( \gamma \) = Lorentz factor, gamma [no units]

Gamma must be greater than one. This means that \(\Delta t> \Delta t_0\).

\(\Delta t\) represents the time passed for an observer watching events that are
moving relative to the observer.

This is the point of view where there is a relative velocity between events and
observer.

For example, if you watch an airplane fly past, events on the plane occur in different
locations because the airplane is moving.

\(\Delta t_0\) represents the time passed for an observer while watching events that are at
rest relative to the observer.

This is the point of view where there is no relative velocity between events
and observer.

For example, if you are flying in an airplane, the events on the plane occur in the same
location, because there is no relative motion.

Thought Experiment: You are on Earth, and a spaceship zooms past near the speed of light.
When the ship is overhead, will you see the ship in slow motion or fast forward?
results You will see them in slow motion. Observers always see moving objects in slow motion.

Although, this gets more complicated when an object is moving towards or away from you because of
the Doppler effect. The doppler effect makes it so that when something is moving towards you they will
seem to you to be in fast forward, and when they move
away from you they seem to be in slow motion.

What does the spaceship see?
Are you in fast forward, slow motion, or normal?
results

From the ship's point of view you are in slow motion! This is similar to how two people at a
distance will see each other as smaller.

Example: A spaceship is moving at 0.9c relative to Earth. A person on the spaceship cooks a
burrito for 90 seconds. How long does an Earth based observer have to watch the spaceship while the burrito
heats up?
disclaimer

These problems about spaceships are all science fiction.

Current spaceships can't travel near the speed of light. As of 2018, the fastest manmade object is
the Juno space probe at 73,800 m/s
relative to Earth.

hint What is the event? (the 90s on the ship)
Who sees the event at rest? (the ship observer)
Who sees the event as moving? (the Earth observer)

Example: A spaceship is moving at 0.9c relative to Earth. A person on the ship can see a
live Earth broadcast of an episode of Star Trek, but the episode lasts 100.9 minutes. How long is the
episode when viewed at rest on Earth?
solution
$$\gamma = 2.29$$
$$ \Delta t = \gamma \Delta t_0 $$
$$ 100.9 \, \mathrm{ min} = (2.29) \Delta t_0 $$
$$ \Delta t_0 = 44 \, \mathrm{ min} $$

Example: What fraction of the speed of light is \( \small 2\times 10 ^{8} \tfrac{m}{s} \)?
solution
$$ 2\times 10 ^{8} \, \mathrm{\tfrac{m}{s}} \left( \frac{c}{3 \times 10^8 \tfrac{m}{s}} \right) =
\tfrac{2}{3} c = 0.\overline{6}c$$

Example: A spaceship is moving at \( \small 2\times 10 ^{8} \tfrac{m}{s} \) relative to the
Earth. A person on the spaceship watches a 74 minute episode of the show Black Mirror at normal speed. How
long would an Earth observer spying on the spaceship have to wait for the episode to be over?
solution
$$ 2\times 10 ^{8} \, \mathrm{\tfrac{m}{s}} \left( \frac{c}{3 \times 10^8 \, \mathrm{\tfrac{m}{s}}}
\right) = \tfrac{2}{3} c$$
$$\gamma = 1.34$$
$$ \Delta t = \gamma \Delta t_0 $$
$$ \Delta t = (1.34) (74 \, \mathrm{min}) $$
$$ \Delta t = 99.16 \, \mathrm{min} $$

Muons are elementary particles similar to
electrons, but more massive.
Muons are produced in Earth's upper atmosphere by cosmic rays, but they have a half-life of 1.5
microseconds at rest.
This means after 0.0000015 seconds half of a population of muons will decay into other particles.

Example: As muons enter the Earth's atmosphere, they typically have a speed of 0.98c.
How long would the half life of these high speed muons look to an observer on Earth?
solution
$$\gamma = 5.0$$
$$ \Delta t = \gamma \Delta t_0 $$
$$ \Delta t = (5) (1.5 \,\mu\mathrm{s}) $$
$$ \Delta t = 7.5 \,\mu\mathrm{s}$$

Example: Find the relative velocity of a clock that runs at one-half the rate of a clock at
rest.
strategy Use the time dilation equation to solve for the Lorentz factor.
Use the Lorentz factor to find the velocity.

Length contraction only occurs in the direction of the relative velocity. Objects don't look smaller; they
look shorter.

An observer sees lengths contracted along the relative velocity.

$$ L = \frac{L_0}{\gamma}$$

\( L\) =
contracted length, as seen from a relative velocity
\( L_0\) =
rest length, as seen from its own rest frame
\( \gamma \) = Lorentz factor, gamma [no units]

The rest length is always longer. An object will look contracted from a moving reference frame.

Example: When you are holding a meter stick it looks like it is 1 meter long. How long
would the meter stick look if it was moving lengthwise at 0.5c relative to you?
solution
$$\gamma = 1.15$$
$$L = \frac{L_0}{\gamma}$$
$$ L = \frac{1 \, \mathrm{m}}{1.15} $$
$$ L = 0.87 \, \mathrm{m} $$

Example: I see myself as 1.84 m tall. If I ran past you at 0.4c how tall would I look to
you?
solution

I would still look 1.84 m tall because the length contraction is in the direction you are traveling.
I would look thinner though!

Example: You see a spaceship pass over head and you quickly record some information about
the ship. How long would the ship be if it landed on Earth?

One of the implications of special relativity is that mass is a type of energy.
Mass is not the same as energy. Mass is a type of energy, just like how kinetic and gravitational potential
are types of energy.

We originally thought that mass produced gravity and had inertia.
We now know that all types of energy have these properties,
although it does take a large amount of energy to measure them.

If you add kinetic energy to an object it will have more gravity and more inertia.
This also means that objects with no mass, like light, have inertia and gravity.

$$ E = \gamma mc^2$$

\( E\) = Energy [J]
\( \gamma \) = Lorentz factor, gamma [no units]
\( m \) = mass [kg]
\(c\) = speed of light, 3 × 10⁸ [m/s]

At rest, the Lorentz factor is one.
This gives us Einstein's famous equation for mass-energy equivalence at rest.

$$E = mc^2$$

Example: A massive object at rest still has a huge amount of energy. The book "Surely
You're Joking, Mr. Feynman!" by Richard Feynman has a mass of 0.27 kg. How much energy does the book
have at rest?
solution
$$ E = mc^2 $$
$$ E_{\text{book}} = (0.27 \, \mathrm{kg})(3 \times 10^{8} \, \mathrm{\tfrac{m}{s}})^2 $$
$$ E_{\text{book}} = 2.43 \times 10 ^{16} \, \mathrm{J}$$

Richard Feynman was part of the Manhattan Project that developed the
first nuclear bomb. The energy released by the nuclear bomb dropped on Hiroshima is 400 times less
than the energy stored in his book:

Mass is not a conserved value.
Mass can be created and destroyed when it changes into a different type of energy.
For example, the mass of a particle is converted into energy when it is annihilated.

$$ e^- + e^+ \to \gamma + \gamma $$

When a fundamental particle and its antiparticle collide they annihilate to form two photons. The photons
have the same energy as the original particles.
(The symbol gamma is used to represent a photon, not the Lorentz factor.)

Example: The antimatter version of an electron is a positron. Calculate the energy of a
photon produced by the annihilation of an electron and positron.
(Assume the electron and positron aren't moving at relativistic speeds.)Subatomic Particles Data Table

Matter antimatter annihilation converts all the mass of a particle into energy.

Calculate the energy for an electron and positron. You can look up their mass on the data table.
The electron and positron energy will equal the energy of the 2 gamma rays produced by the
annihilation.

solution
$$ m_e = 9.109 \times 10^{-31} \, \mathrm{kg} $$
$$ E = mc^2 $$
$$ E = (9.109 \times 10^{-31})(3 \times 10^{8})^2 $$
$$ E = 8.198 \times 10^{-14} \, \mathrm{J}$$
Photons produced by annihilation are typically considered gamma rays.

Example: The Large Hadron
Collider can accelerate a proton to 0.999999991c.
How much energy would an observer measure for a proton at that speed?
solution
$$ \gamma = \frac{1}{\sqrt{1-\frac{v^2}{c^2} } }$$
$$ \gamma = \frac{1}{\sqrt{1-\frac{(0.999999991)^2c^2}{c^2} } }$$
$$ \gamma = \frac{1}{\sqrt{1-(0.999999991)^2 } }$$
$$ \gamma = 7453.6$$
$$m_\mathrm{p} = 1.67 \times 10^{-27}$$
$$ E = \gamma m c^2 $$
$$ E = (7453.6) (1.67 \times 10^{-27}) (3\times 10^8)^2 $$
$$E = 1.12 \times 10^{-6} \, \mathrm{J} $$

Question: If mass and energy are the same thing, why do we still use different words for
them?
Are they really the same?
answer

Mass and energy are the same thing with different units.
An accurate measurement of mass includes all energies.
I'm not sure why we continue to use separate terminology.
Maybe it's tradition, or maybe different fields need different units.

Rest mass is the energy of single particle at rest.
Most particles are actually made of several fundamental particles that are held together by a force.
When we say "mass" we typically mean the sum of rest mass and the internal energies holding groups
of particles together.

For example, a proton is made of 3 particles called quarks, but the rest mass of 3 quarks is less
than the mass of a proton.
It turns out that 99% of a proton's mass comes from the binding energy of the strong nuclear force
that holds the quarks together.

The rest mass of fundamental particles isn't where most energy is stored.
Protons, neutrons, atoms, molecules, people, planets, and stars get most of their mass from the
binding energy of the strong nuclear force.
Of course those things only make up about 5% of the total energy in the universe.
The rest of our observable universe is dark matter(27%), and dark energy(68%).
Dark matter and dark energy aren't well understood, but there is strong evidence they exist.

$$ n \to p^+ + e^- + \bar{v}_e $$

A free neutron is unstable with a half-life of about 15 minutes. It decays into a proton, an electron
and an antineutrino. This process is called beta decay.

Example: The beta decay products are measured to have a total kinetic energy of 0.78 MeV.
Show that conservation of energy holds for beta decay.
Subatomic Particles Data Table

strategy Convert the masses of each particle into energy. Conservation of energy holds if the left side of
the reaction equals the right side plus the kinetic energy.

The antineutrino has such a low mass it can be ignored

Be sure to include enough precision in the masses.

solution
$$E_0=mc^2$$
$$E_p = (1.672621 \times 10^{-27})(9 \times 10 ^{16}) = 1.5053589 \times 10^{-10} \, \mathrm{J}$$
$$E_e = (9.109383 \times 10^{-31})(9 \times 10 ^{16}) = 8.1984447 \times 10^{-14} \, \mathrm{J}$$
$$K = 0.78 \, \mathrm{MeV} \left(\frac{1.602 \times 10^{-19} \, \mathrm{J}}{ \, \mathrm{eV}}\right)
= 1.24 \times 10^{-13} \, \mathrm{J} $$
$$ E_p + E_e + K$$
$$ \small 1.5053589 \times 10^{-10} \, \mathrm{J} + 8.1984447 \times 10^{-14} \, \mathrm{J} + 1.24
\times 10^{-13} \, \mathrm{J} = $$
$$ \color{#f02} 1.507418 \times 10^{-10} \, \mathrm{J} $$
$$ E_n = (1.674927 \times 10^{-27})(9 \times 10 ^{16}) = \color{#f02} 1.5074343 \times 10^{-10} \,
\mathrm{J}$$
The energy of a neutron is very close to the total energy of its products. The small difference can
be attributed to the detail in the measurements.

Kinetic energy is the energy an object has because of its velocity. We can find a relativistic equation
for kinetic energy by finding the difference between the energy of an object at a relative velocity and
at rest.

$$K = E - E_0$$
$$K = \gamma mc^2 - mc^2 $$
$$K = (\gamma -1)mc^2$$
Example: How much kinetic energy would an observer measure for a 1 kg object moving at half
the speed of light?

\( \Delta s^2 \) is the spacetime interval. Not \( \Delta s \).

Observers at different relative velocities will disagree about ∆t and ∆x, but they will always agree on the value of ∆s².

Example:
What is the spacetime interval for an event 7 years in the future and 8 light-years away?
light-years

A light-year [ly] is a unit of distance. It's the distance that light travels in one year.
Light-years are a great unit for the spacetime interval because they can be used as a unit of distance or time when moving at the speed of light.

Multiplying years by the speed of light converts the units into light-year.
$$ c = \frac{\Delta x}{\Delta t} $$
$$ c \Delta t = \Delta x$$
$$ (\tfrac{\mathrm{m}}{\mathrm{s}}) (\mathrm{yrs}) = \mathrm{ly} $$
So years times the speed of light can be added to light years with out the need for conversions.

Remember, \( \Delta s^2 \) is the spacetime interval. Not \( \Delta s \). So we can stop here.

The spacetime interval's sign tells us about the possible causal relationship between two events.
In other words we can tell if two events in spacetime could communicate.

$$ \Delta s^2 = \mathrm{interval} $$
$$ \Delta s^2 = c^2 \Delta t^2 - \Delta x^2 $$
When only a single space dimension is needed we can use a shorter equation for the spacetime interval.

$$ \Delta s^2 = 0 $$ $$ c^2 \Delta t^2 = \Delta x^2 $$
A light-like interval is zero. This means that two events could be connected by a
photon of light.

$$ \Delta s^2> 0$$
$$ c^2 \Delta t^2> \Delta x^2 $$
A time-like interval is positive.
This means that there could be a causal relationship between two events.

$$ \Delta s^2 < 0$$
$$ c^2 \Delta t^2 < \Delta x^2 $$
A space-like interval is negative.
This means that there could not be a causal relationship between two events.

An event can cause another event to occur, but the speed of light puts a limit on causality.
There are places in space and time that could never interact with each other, because nothing can move fast
enough to connect them.
A light cone divides space and time into separate regions to help visualize the limits of causality.

Example:
What is the spacetime interval for an event 3 years in the future and 2 light-years away?
Is the interval space-like, time-like, or light-like?
solution
$$ \Delta s^2 = c^2 \Delta t^2 - \Delta x^2 $$
$$ \Delta s^2 = c^2 (3 \, \mathrm{yr})^2 - (2 \, \mathrm{ly})^2 $$
$$ \Delta s^2 = (3 \, \mathrm{ly})^2 - (2 \, \mathrm{ly})^2 $$
$$ \Delta s^2 = 9 \, \mathrm{ly}^2 - 4 \, \mathrm{ly}^2 $$
$$ \Delta s^2 = 5 \, \mathrm{ly}^2 $$

The interval is greater than zero, so it is time-like.
One could potentially effect events 3 years in the future and 2 light-years away.

The nearest star, not counting the Sun, is Proxima Centauri. It is 4.22 light-years away from Earth.

Example:
If the current date is January 1st 2049,
could you make it to Proxima Centauri by the year 2052?
Use the spacetime interval to prove your answer.
solution
$$\Delta t = t_f - t_i $$
$$\Delta t = 2052 \, \mathrm{yr}- 2049 \, \mathrm{yr}$$
$$\Delta t = 3 \, \mathrm{yr} $$
$$ \Delta s^2 = c^2 \Delta t^2 - \Delta x^2 $$
$$ \Delta s^2 = c^2 (3 \, \mathrm{yr})^2 - (4.22 \, \mathrm{ly})^2 $$
$$ \Delta s^2 = (3 \, \mathrm{ly})^2 - (4.22 \, \mathrm{ly})^2 $$
$$ \Delta s^2 = 9 \, \mathrm{ly}^2 - 17.8 \, \mathrm{ly}^2 $$
$$ \Delta s^2 = -8.8 \, \mathrm{ly}^2 $$

The spacetime interval between Earth in 2049 and Proxima Centauri in 2052 is negative.
The interval is space-like.

Nothing could travel between the events in that amount of time.
This means that these two locations in spacetime couldn't be casually linked.

Lorentz Transformation Solver

Relative Velocity
v = c
v = × 10^{8} m/s

Lorentz Factor
γ =

MOVING RELATIVE TO SPACESHIP time = s
energy = J
length = m

AT REST RELATIVE TO SPACESHIP proper time = s
rest energy = J
rest length = m

Frame of reference where an observer sees the spaceship in different locations.

Frame of reference where an observer sees the spaceship in the same location.