シャドーイング練習: The Biggest Misconception in Physics - 動画で英語スピーキングを学ぶ

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Imagine you're an astronaut out drifting in deep space.

When you throw a rock as hard as you can, what's gonna happen to that rock?

Well, you would think that it would continue with constant velocity in a straight line.

That's just Newton's first law.

But what actually happens is it eventually slows down and stops.

So why does this happen?

Where did all the rock's energy go?

At the turn of the 20th century, the problem of energy conservation baffled some of the greatest minds, including Albert Einstein.

Einstein came up with a possible solution.

But then a little -known unpaid mathematician named Emmy Noether proved he was wrong.

And in doing so, she created a whole new paradigm for physics, one that underlies all of particle physics and explains why anything is conserved.

It all started in 1915 at the University of Göttingen, where Einstein was giving six lectures on his new theory of gravity,

what would become the general theory of relativity.

The lectures were well received, but Einstein hadn't yet settled on the final form of the field equations.

One problem he was facing was how to show that total energy was conserved in his new theory.

This is the whole beginning of this story, right?

Classically, they thought they had this understanding of what the energy of a gravitational field was.

All of a sudden, with these new equations, they go, where is it?

You know, is it in the curvature?

You know, is it in the stress -energy tension?

Where's the term that we're looking for?

Einstein suggested that the principle of conservation of energy, long established as a bedrock of physics,

might hold the key to working out the correct field equations.

In the audience, legendary mathematician David Hilbert was intrigued.

So he started to look for the energy conservation equations in Einstein's new theory.

But the best he could find was a set of equations known as the Bianchi identities.

They showed that energy was conserved, but only in a completely empty universe.

So for one like ours, filled with stuff, they seemed useless.

Hilbert was stumped.

Fortunately, he knew just the person for the job

His new assistant, Emmy Nutter From an early age,

Nutter had dreamed of following the footsteps of her father A mathematics professor at the University of Erlingen

She got special permission to attend lectures at the university

But they refused to admit her as an official student

The Erlingen Academic Senate held that the admission of women would overthrow all academic order

So, in 1903, she spent a semester at Göttingen instead.

There, she learned about a new way to approach geometry.

Using symmetry.

Symmetry is one of those ideas that's easy to recognize, but harder to describe.

If I align a mirror on this triangle like so, then it looks the same as without the mirror.

And that's because this is an axis of symmetry.

Reflections about this axis leave the triangle unchanged.

And the same thing happens if I put the mirror like this or if I orient the mirror like this.

So this triangle has three axes of symmetry.

Now mathematicians generalize the idea of symmetry further to be any action you can take that leaves an object unchanged.

So something else I could do is I could rotate this triangle by 120 degrees

or by 240 degrees or by 360 degrees.

Together, these six actions capture all the symmetries of the equilateral triangle.

But you can also have more abstract symmetries, for example with a mathematical function.

If I shift this function up or down by some constant amount, call it a, then all of its y values will change.

But if I differentiate that function, I get the slope and that remains unchanged regardless of whatever constant is added.

So you can add any constant to this function and its derivative always stays the same.

So there's a kind of translation symmetry.

And unlike the symmetries of the triangle, this is a continuous symmetry, meaning you can shift it by any amount you like.

Over the next 12 years, Noether became a leading expert on symmetry.

She became only the second woman in Germany to earn a PhD in mathematics,

and she used this expertise to help Hilbert and Einstein with their problem of energy conservation.

The issue had bothered Einstein so much that he proposed a new conservation equation.

It said that if we add together the energy of matter and the energy of the gravitational field, then that total remains constant.

Its change over time and space is zero.

But when Noether saw this,

she was convinced Einstein had made a fundamental mistake because this equation disregards the foundational principle that general relativity is built on.

Ten years earlier, in 1905, Einstein had introduced his special theory of relativity,

and it was built on the idea that the laws of physics were independent of your frame of reference.

But so far, Einstein had only applied this principle to inertial frames of reference.

Those are frames that move at a constant speed.

He began wondering what would it take to generalize that, to consider more general states of motion.

After all, trains on the platform, he loved trains.

Trains would speed up or slow down.

People, you know, moving around the world don't only move at a single constant speed forever.

In 1907, he wrote, is it conceivable

that the principle of relativity also applies to systems that are accelerated relative to each other?

This made him wonder.

Perhaps his principle could also be applied to accelerating and rotating frames, frames that move in any way in general.

That's the general in general relativity.

So Einstein got to work on this largely intellectual pursuit.

But then, as he was daydreaming in the patent office, he had what he called the happiest thought of his life.

He imagined the window cleaner at the top of the opposite building falling off.

And Einstein realized that while the man was falling, he wouldn't feel his own weight.

He would be weightless, and anything he dropped on his way down would remain stationary relative to him.

It would be just as if he was floating in outer space.

It's ironic.

We would have sat down with being pulled down to the ground because the gravity of the earth is exerting a force.

But Einstein said while that person is in motion, what we call freefall motion, they'll actually feel no gravity at all.

There must be some equivalence between accelerated motion and the action of gravity.

So Einstein arrived at what he called the equivalence principle.

If you were stuck in a rocket in outer space accelerating at 9 .8 meters per second squared,

then it would be the exact same as if you were standing on the surface of Earth.

and this was huge because it meant that

if Einstein could figure out how to understand accelerating frames

then he didn't just get a more general theory he would also have a new theory of gravity

but to achieve this Einstein needed to make sure the laws

of gravity had the same form in every frame of reference this is the idea of general covariance

and it's one of the core tenets of general relativity to satisfy

it Einstein knew he had to use special mathematical objects called tensors.

A simple kind of tensor is a vector.

You can write a vector as a set of components multiplied by their basis vectors.

For example, this vector can be written as 3x hat plus 2y hat.

But I can also write this using a different coordinate system.

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And with these new basis vectors, the original vector is now written as 2a plus 1b.

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So the components, the numbers in this list changed, but the vector didn't.

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It stayed the same.

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And that's because when the basis vectors change, the components adjust in a complementary way to keep the vector the same.

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The vector itself is independent of which coordinate system you use.

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And the same is true for tensors.

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Only now, instead of having just two components, a general tensor can have any number of them in the form of a matrix.

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And just like with vectors, you can change a tensor from one coordinate system to another, and the tensor stays the same.

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So that's why Einstein had to use them to build his new theory.

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And that was exactly the problem that Knüter found, because when she looked at Einstein's proposed energy conservation equation, it contained a pseudotensor.

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And as the name implies, that isn't quite a tensor.

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When you try to transform it from one frame of reference to another, it doesn't remain the same quantity in different frames.

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The gravitational energy you might observe in one frame completely disappears in another.

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And Einstein, he had some strange thoughts about this.

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I mean, people were trying to stamp conservation of energy into relativity by bending the rules of mathematics.

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So, Nutter knew that Einstein's proposed solution couldn't be the answer.

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And that made her think.

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What if general covariance and energy conservation are simply incompatible?

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And if that's the case, then why?

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General covariance says that laws of physics must stay the same when you change reference frames.

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So that is a kind of symmetry, exactly what Noether had spent her career studying.

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So she started thinking about the symmetries of the universe, beginning with the simplest possible case, an empty static universe.

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Imagine you're an astronaut in this universe.

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Since it's empty, there is nothing special about any particular point.

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I mean, it doesn't matter if you're over here or over there.

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The universe is completely symmetric under translations in space.

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So suppose you throw a ball.

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Well, it'll travel at a given speed, and after a short amount of time, it will have traveled some distance.

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But since the laws of physics are the same here as just before,

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Or, we can shift the whole universe and we're back to the situation we started with.

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And we can keep doing this over and over, and this shows us that the object will continue with that same speed indefinitely.

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So what we've discovered is

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that the principle of conservation of momentum is a direct result of the fact that there's a translation symmetry in the universe,

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that an experiment done in one spot will give identical results to that same experiment done somewhere else.

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You could move everything from one place to another, and the physics won't change.

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Similarly, the laws of physics don't depend on whether you perform an experiment like this, or rotate everything by 90 degrees.

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This universe is symmetric under rotations.

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So imagine we take a metal rod and spin it.

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If we let it rotate for a minute, then it will have moved through a small angle.

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But we can rotate the whole universe back by that same angle, and now we're at the starting position again.

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And we can keep doing this so that each instant looks exactly the same as the one before,

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which means the object will keep rotating this way indefinitely.

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So the law of conservation of angular momentum comes from the rotational symmetry of the universe.

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Now, another important symmetry of this universe is time symmetry.

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The laws of physics don't change over time.

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If you do an experiment today or tomorrow, you will get the same result.

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So what does this symmetry lead to?

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Well, to understand this, we're gonna dig into some math

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and a different way of doing mechanics using the principle of least action.

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Previously on Veritasium, we learned that everything always follows the path that minimizes a quantity known as the action.

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This is equivalent to the integral of the Lagrangian L over time.

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In the simplest case, that's just the kinetic minus potential energy.

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Euler and Lagrange found that the principle of least action is obeyed so long as this set of differential equations is satisfied.

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So Noether used action to see how physics was affected by different symmetries.

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So suppose we do an experiment where the result is the same now as some tiny time interval epsilon later.

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Then how does this affect the action?

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Well, the time is going to change from just t to t plus epsilon.

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And as a result, the Lagrangian is also going to change.

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So the new Lagrangian will be L prime, which is equal to the old Lagrangian, plus how much the Lagrangian changes over time,

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that's just dl by dt, multiplied by how long that change lasts, so multiplied by epsilon.

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But now also remember that the result is going to be the exact same now as a little while later,

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which means that whatever this term is the dl over dt doesn't affect the equations of motion

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and it's from this symmetry in the action

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that we're going to be able to find the conserved quantity

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so let's take dl dt and rewrite it using the chain rule

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that gives us the partial derivative of L with respect to

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X times dx over dt plus the partial derivative of L with respect to V times dv over dt

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but we can sub in the partial derivative of L with respect to x with this term from the Euler -Lagrange equation.

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And we can simplify this further by writing dx over dt as V and that gives us this expression.

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And now notice what we've got right here.

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We've got the time derivative of some function dL over dV times another function plus

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that first function times the time derivative of the second function.

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So we can use the reverse of the product rule to simplify

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this to the time derivative of dl over the v times v

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then as a final step we can bring dl over the t to the right

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so what we found is that

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if you take the time derivative of this quantity it's equal to zero

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which means that whatever this is has to be a constant

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so what is it well remember

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that in the simplest case the lagrangian is just equal to the kinetic minus potential energy

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which we can write as 1 half mv squared minus v. So

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if we take the partial derivative of the Lagrangian with respect to v

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we're just going to get d over dt m times v multiplied by v

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so this is going to become mv squared

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and then we can sub in the Lagrangian

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so this becomes minus 1 half mv squared minus v

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but also a minus here so this becomes plus v and all of that's equal to zero

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which we can simplify to just one -half mv squared plus v is equal to zero.

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But wait a second, because this is just the total energy.

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So what we've discovered is that time translation symmetry is equivalent to saying that energy is conserved.

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The principle of conservation of energy is a direct consequence of time translation symmetry.

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In a theorem, Noether proved that all of these examples are no coincidence.

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For centuries, people had no idea where conservation laws came from.

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But now, Noether had discovered the origin of all of them.

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She proved that any time you have a continuous symmetry, you get a corresponding conservation law.

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Translational symmetry gives you conservation of momentum.

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Rotational symmetry gives you conservation of angular momentum and time translation symmetry gives you conservation of energy.

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But these are all symmetries of a static, empty universe.

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The universe we live in is very different.

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In the 1920s, astronomers measured the velocities of distant galaxies, and they realized all of them are moving away from us.

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The farther away they are, the faster they're moving.

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The implication was clear.

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In the distant past, everything must have been much closer together.

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In the 1990s, precise measurements of supernovae revealed that not only was the universe expanding, but that expansion was speeding up.

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This means over large timescales, our universe is not symmetric in time.

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It was very different 13 billion years ago, and it'll be different billions of years from now.

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Since we don't have time symmetry, that also means energy as we usually think of it isn't conserved.

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There's no reason for energy to be conserved anymore because you don't have that symmetry.

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Think about a photon of visible light emitted 380 ,000 years after the Big Bang.

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It travels through the universe unimpeded to arrive at our telescopes, not as visible light, but as a microwave.

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It has lost 99 .9 % of its energy.

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Where did the energy go?

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It doesn't go anywhere.

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Energy is not conserved.

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And this is exactly what's happening to the rock as well.

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It starts off with energy, but as it travels through the expanding universe, it slows down and stops.

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The energy doesn't really go anywhere.

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It just disappears years, it ends up coming to rest with regards to the other particles in the universe.

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This doesn't violate any laws of physics because energy and momentum aren't conserved if there is no time or spatial symmetry.

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So once you know that symmetries give you conservation laws, and so once those symmetries are gone,

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you don't have to worry about those conservation laws anymore, then you can start drop in these concepts of trying to force something

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that you want to say is fundamental into the theory and you just deal with what the theory gives you.

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But if energy isn't conserved in our universe then why does it usually seem like it is?

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That's because when you're looking at the short timescales that we're used to, time translation symmetry pretty much holds.

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An experiment done today will give the same results as the same experiment done tomorrow.

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So that That means, for all intents and purposes, energy is conserved.

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But over large timescales, on the order of millions of years, well then, the expansion of the universe can't be neglected, and the symmetry is broken.

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So only when you look at timescales that big do you notice that energy isn't conserved.

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Noether's first theorem explains why a rock or a photon loses energy.

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But it didn't fully solve the problem of energy conservation in general relativity.

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See, so far, Nutter had only dealt with an empty universe,

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where you could shift the whole universe and the laws of physics would stay the same.

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But this doesn't work in general relativity, where the curvature can change from one point to another.

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Now, if you shift the whole universe, rotate it, or let it evolve in time, things don't stay exactly the same,

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so you no longer have these global symmetries.

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But Nutter realized there are still other symmetries left.

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See, no matter how you're moving, the laws of physics always look the same.

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That's general covariance.

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And it is a kind of symmetry that holds everywhere.

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It means that in any small region, we can always change our frame of reference.

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We can transform the points of space around as much as we like.

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And since these transformations aren't global, but local, these are called local symmetries.

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In a second theorem, Nutter proved that for these local symmetries, you no longer get proper conservation laws like we're used to in classical physics.

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Instead, you get something that only works locally, a continuity equation.

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One example of a continuity equation describes the flow of water through a pipe.

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This first term tells you how the amount of water changes in a section of the pipe,

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and the second tells you the difference between how much water is flowing out and how much is flowing in.

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In this case, the first term is positive because the water level in this pipe section is increasing,

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and the second term will be negative because less water is flowing out of the section than in.

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Together, the two terms cancel to give zero, which guarantees that no water is created or destroyed.

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If the total amount of water changes in a section, there must either be excess water flowing in or out.

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In the case of general relativity, Noether found a similar continuity equation, but with an important difference.

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Imagine that now our pipes are little patches of space -time, and the water is energy flowing from one patch to another.

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In any individual section, the continuity equation looks exactly the same as before, so that in any small region spacetime, energy is conserved.

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But when we link these sections together, we need to take into account the curvature of spacetime.

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And this changes the equation.

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Now it's as if there are little cracks appearing between different sections of pipe, between the local patches of spacetime.

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And through those cracks, energy can leak out.

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In special relativity, the pipe is imperturbable because the pipe is fixed and in general activity, you know, we have to account for the energy

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that goes into other kinds of change over time and that gets correspondingly more tricky.

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Now that we have this new equation, we can see how it works by expanding it as a sum of different terms.

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This first term is analogous to the continuity equation from before, the one which conserves energy within a local patch of spacetime.

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But now we have all these extra terms.

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These describe the curvature of spacetime.

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So as energy decreases in the first term, these curvature terms increase.

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The energy that you lose from the system you're tracking, we now start attributing it to things like the gravitational field,

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which has changed because the whole universe is stretched.

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We should account for the energy that we attribute to the action of the gravitational field as well, because space and time themselves aren't sitting still.

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And all of this can be described by the continuity equation Noether had found.

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But when she looked at it, she realized something.

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It was exactly equivalent to the Bianchi identities, the half solution Hilbert had found.

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He had dismissed it because it only gave you proper energy conservation in an empty universe.

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But now Noether proved that it was the best you could do in general relativity.

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With one paper, she had uncovered the source of all conservation laws, and she had solved the problem in general relativity that eluded Hilbert and Einstein.

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She was so amazing.

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I mean, I would go out on a limb

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and I would say these two theorems are probably the most important theorems for physics of the 20th century.

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In the following years, the University of Göttingen took steps to make Noether's position more official, allowing her to do what she loved most, to teach.

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They made her a professor and she even got a small salary starting in 1923.

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But all of that changed on the 30th of January, 1933, when Hitler became chancellor of Germany.

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The Nazis banned

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Jewish people from working at universities.

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And almost immediately, one of her former students told the authorities of her Jewish heritage, and she was suspended.

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Despite this dismissal, she continued teaching in the kitchen of her home.

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Then one day, one of her old students knocked on her door.

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Clothed in the brown shirt of the Nazi stormtroopers, Noether let him in.

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He had come to learn math and Noether was happy to teach him.

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I love what this sort of shows about Noether.

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You know, she truly deeply cared about math and she wouldn't discriminate whether someone was wearing a Nazi shirt or not.

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She taught all.

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But staying in Germany became untenable.

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Fortunately, with the help of other academics, she managed to obtain a teaching position at Bryn Maw, a women's college in America,

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where she would teach until her death.

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In an obituary for the New York Times, Einstein wrote that

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The reason that Noether's theorem is so important is that everybody just changed their state of mind.

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All of a sudden, the physicists were thinking about physics in terms of these symmetries.

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Physicists started applying these ideas to the quantum world too, realizing that charged particles like electrons also have symmetries.

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Electrons have a phase, which you can think of as an arrow pointing in some direction.

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But you can offset this phase by any arbitrary amount, so long as you do it simultaneously for all electrons.

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And that doesn't change anything physically.

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So there's another symmetry.

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So what does this offset or gauge symmetry lead to?

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Well, it leads to the conservation of electric charge.

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In the 1960s and 70s, Noether's insights led directly to the discovery of new fundamental particles like quarks and the Higgs boson.

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It taught us where the forces of nature come from, and it even helped to explain the origin of all mass in the universe.

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Noether's two theorems, although little known, are what has gotten us the closest we've ever come to a theory of everything.

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But all of this and much more will be covered in a second video,

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so make sure you're subscribed to get notified when that video comes out.

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When Emmy Noether set out to study mathematics, she was following in her father's footsteps.

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But from there, she forged her own path, and before long she was coming up with a whole theory that reshaped our understanding of the universe.

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That is the great thing about learning.

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You start by following instructions, building on what others have done before you, but then at some point, you start asking your own questions.

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You start experimenting and making discoveries.

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Without even realizing it, they were engaging with the same questioning mindset that drives real scientific discoveries.

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So who knows, maybe a simple disk launcher will inspire a young scientist who

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KiwiCo makes this easy by delivering everything you need in a single box, and they have projects for all ages designed by experts

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このレッスンの語彙とスピーキングのポイント

このスピーキングレッスンは、動画「The Biggest Misconception in Physics」を教材にしています。繰り返し出てくる語は次のとおりです：energy, symmetry, universe, conservation, Noether。この動画には、シャドーイング用の文が255文、単語が4496語あります。音声の長さは27:34です。話す速さは1分あたり約163語で、日常会話に近い自然なペースです。英語の頻出3,000語に含まれる単語は80%だけなので、語彙は難しめです。

この動画の重要語彙

動画に出てくる覚えておきたい単語15語を、発音と意味つきで紹介します。

単語	発音	意味
symmetry 名詞	/ˈsɪm.ɪ.tɹaɪ/	対称性, 対称
conservation 名詞	/ˌkɑnsə(ɹ)ˈveɪʃən/	保存
equation 名詞	/ɪˈkweɪ.ʒən/	方程式
physics 名詞	/ˈfɪz.ɪks/	物理学
vector 名詞	/ˈvɛktɚ/	ベクトル
principle 名詞	/ˈpɹɪn.sɪ.pəl/	原理, 原則
experiment 名詞	/ɪkˈspɛɹ.ə.mənt/	実験
derivative 名詞	/dɪˈɹɪvətɪv/	派生
pipe 名詞	/ˈpaɪp/	笛
theorem 名詞	/ˈθiərəm/	定理
rotate 動詞	/ˈɹoʊ.teɪt/	回る
translation 名詞	/tɹænzˈleɪʃən/	翻訳, 伝達
minus	/ˈmaɪ.nəs/	引く
triangle 名詞	/ˈtɹaɪˌæŋɡəl/	三角, 三角形
momentum 名詞	/ˌmə(ʊ)ˈmɛntəm/	運動量

動画に出てくる句動詞

単語	発音	意味
slow down 動詞		遅らせる
speed up 動詞	/spiːdˈʌp/	スピードを出す
come out 動詞	/ˌkʌm ˈaʊt/	出る
get off 動詞		降りる
try out 動詞		試す, 試してみる

繰り返し練習したい文

動画に出てくる短く完結した文です。日常会話でそのまま使えます。

What's gonna happen to that rock?
Where did all the rock's energy go?
You know, is it in the curvature?
You know, is it in the stress-energy tensor?

この動画の文法

話し手がよく使っている文型を、動画の実際の表現とともに紹介します。

文型	動画での表現
受動態 be + 過去分詞 — 誰がするかより、何が起きるかに焦点を当てる	is conserved · was conserved · was intrigued
現在完了形 have/has + 過去分詞 — 過去の出来事が今も関係している	we've discovered · has lost · has changed

注意したい発音

話し手はdoesn't, we're, don'tなど、短縮形や弱形を63回使っています。聞こえたとおりの短い形で発音しましょう。

「th」の音: theorem /ˈθiərəm/, mathematics /mæθ(.ə)ˈmæt.ɪks/, math /mæθ/, mathematical /ˌmæθ(.ə)ˈmæt.ɪ.kəl/, bother /ˈbɑðɚ/
「sh」と「zh」の音: conservation /ˌkɑnsə(ɹ)ˈveɪʃən/, equation /ɪˈkweɪ.ʒən/, translation /tɹænzˈleɪʃən/, partial /ˈpɑɹʃəl/, instruction /ɪnˈstɹʌkʃən/
長い単語（アクセントの位置に注意）: conservation /ˌkɑnsə(ɹ)ˈveɪʃən/, experiment /ɪkˈspɛɹ.ə.mənt/, derivative /dɪˈɹɪvətɪv/, continuity /ˌkɑn.tɪˈn(j)u.ə.ti/, momentum /ˌmə(ʊ)ˈmɛntəm/

日本語話者が苦手な音：

/r/ と /l/ の区別 — /l/ は舌先を歯茎につけ、/r/ はどこにもつけない: principle /ˈpɹɪn.sɪ.pəl/, translation /tɹænzˈleɪʃən/, triangle /ˈtɹaɪˌæŋɡəl/, accelerate /ɪkˈsɛl.əˌɹeɪt/, partial /ˈpɑɹʃəl/
/v/ — /b/ にならないように、上の歯を下唇に当てる: conservation /ˌkɑnsə(ɹ)ˈveɪʃən/, vector /ˈvɛktɚ/, derivative /dɪˈɹɪvətɪv/, gravity /ˈɡɹævɪti/, discovery /dɪˈskʌv.ɹi/
/f/ — 「フ」ではなく、上の歯と下唇で出す: physics /ˈfɪz.ɪks/, fundamental /ˌfʌn.dəˈmɛn.təl/, transform /tɹænsˈfɔɹm/, offset /ˈɔf.sɛt/, satisfy /ˈsætɪsfaɪ/

この動画での練習方法

まず声を出さずに動画を最後まで聞き、知らない単語をメモします。
まず0.75倍速で一文ずつシャドーイングし、慣れてきたら通常の速度に戻します。
自分の声を録音して元の音声と比べます。symmetry, conservation, equationなどの単語に特に注意しましょう。

シャドーイングとは？英語上達に効果的な理由

シャドーイング（Shadowing）は、もともとプロの通訳者養成プログラムで開発された言語学習法で、多言語習得者として知られるDr. Alexander Arguelles によって広く普及されました。方法はシンプルですが非常に効果的：ネイティブスピーカーの英語を聞きながら、1〜2秒の遅延で声に出してすぐに繰り返す——まるで「影（shadow）」のように話者を追いかけます。文法ドリルや受動的なリスニングと異なり、シャドーイングは脳と口の筋肉が同時にリアルタイムで英語を処理・再現することを強制します。研究により、発音精度、抑揚、リズム、連音、リスニング力、そして会話の流暢さが大幅に向上することが確認されています。IELTSスピーキング対策や自然な英語コミュニケーションを目指す方に特におすすめです。

シャドーイングのやり方: ステップ別の完全ガイドを読む →

シャドーイング練習: The Biggest Misconception in Physics - 動画で英語スピーキングを学ぶ

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