01.06 – Doppler Shift

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Из курса от партнера University of Alberta

Astro 101: Black Holes

25 оценки

University of Alberta

Astro 101: Black Holes

25 оценки

What is a black hole? Do they really exist? How do they form? How are they related to stars? What would happen if you fell into one? How do you see a black hole if they emit no light? What’s the difference between a black hole and a really dark star? Could a particle accelerator create a black hole? Can a black hole also be a worm hole or a time machine? In Astro 101: Black Holes, you will explore the concepts behind black holes. Using the theme of black holes, you will learn the basic ideas of astronomy, relativity, and quantum physics. After completing this course, you will be able to: • Describe the essential properties of black holes. • Explain recent black hole research using plain language and appropriate analogies. • Compare black holes in popular culture to modern physics to distinguish science fact from science fiction. • Describe the application of fundamental physical concepts including gravity, special and general relativity, and quantum mechanics to reported scientific observations. • Recognize different types of stars and distinguish which stars can potentially become black holes. • Differentiate types of black holes and classify each type as observed or theoretical. • Characterize formation theories associated with each type of black hole. • Identify different ways of detecting black holes, and appropriate technologies associated with each detection method. • Summarize the puzzles facing black hole researchers in modern science.

Из урока

Introduction to Black Holes

Hello and welcome to the first module of Astro 101! In this module, you will become familiar with the basic structure of a black hole, learn the terminology used to describe them, and explore the history of black hole physics.

01.01 – Introduction to Black Holes4:28

01.02 – Black Holes in Pop Culture8:17

01.03 – Connecting Gravity and Light6:38

01.04 – Getting on the Same Wavelength11:01

01.05 – Working with Light15:03

01.06 – Doppler Shift10:23

01.07 – Newtonian Gravity16:29

01.08 – Escape Velocity11:40

01.09 – Dark Stars5:25

01.10 – What is a Black Hole?11:54

01.11 – Black Hole Basics2:39

Interviews with experts - How are black holes depicted in Japanese popular culture?4:52

Познакомьтесь с преподавателями

Sharon Morsink
Associate Professor
Department of Physics, University of Alberta

Next up on our tour of the properties of light and sometimes sound,

is an effect first explained by an Austrian mathematician and physicist,

Christian Doppler in 1842.

In a paper entitled,

On the Colored Light of Binary Stars and Some other Stars of the Heavens,

Doppler presented his theory that observed frequency of wave depends

on both the emitted light and on the relative speed of the source and the observer.

But what does this mean?

Well, if we switch back to sound waves for a moment,

we can use a real world analogy to explore this.

I'm sure many of you have been present as emergency vehicles or train pass by.

When this happens, what do you hear?

Well, yes you hear a siren,

but what happens to the siren as an ambulance drives by?

Well, if you listen closely,

you can hear that the pitch of the siren changes over time.

As the ambulance moves towards us,

you hear the siren at one pitch,

but as it passes by,

it seems to drop in pitch.

Let's listen to the sound of a passing train to

compare the sound effect from a different source.

There is a clear drop in pitch.

But what is the reason for this?

Let's take the example of trains and look at this in

more detail to explore the physics of the Doppler shift.

As the train sets off,

we begin to see things change.

The sound waves in front of the train begin to bunch up and are pushed together.

When the wave fronts of the sound waves are pushed closer together,

the wavelength that a stationary person will hear will be smaller.

Smaller wavelengths correspond to higher frequencies and higher pitch.

When a train or ambulance approaches,

you hear a higher pitched sound.

Now if we look at the waves behind the train,

we can see that as the vehicle moves forward,

the waves appear to be more spread out.

This apparent stretch results in longer wavelengths or

lower frequencies which results in a lower pitch.

As a train moves past us,

the shift raises the pitch as it moves towards us,

has no effect as it's next to us,

and lowers the pitch as it moves away from us.

Tetas has an electronic sound device that emits a sound waves with just one pitch.

As he twells the sound emitter in circles,

we can hear the sound waves changing pitch.

Higher and lower pitches as the emitter moves towards us and away from us.

This raising and lowering of pitch is known as

the Doppler effect and as we hinted at earlier,

it also applies to light.

As light is emitted from a source,

the waves being emitted can be squashed or stretched along the direction of motion.

So, if a star is moving towards us,

the light waves moving ahead of the star can

appear to be increased in frequency or decreased in wavelength.

This translates as a shift towards the blue end of the electromagnetic spectrum.

Conventionally, as the storm moves away from us,

the waves appear to be stretched

resulting in longer wavelengths and a redder look to the star.

For light, the shifts caused by the Doppler effect are known as blueshift and redshift.

Although we should note that this is not

confined to the visible band of the electromagnetic spectrum.

Both X-rays and radiowaves can also be blue and red shifted.

The colors just speak to the direction of the shift.

While stars do not normally raise surrounding clouds,

they are all moving around in space.

Many stars that are observed in the night sky are actually in binary star systems.

In such systems, we see stars in orbit around one another.

If we view a pair of stars from the side,

it will appear as though one star is moving towards us,

while the other star is moving away from us.

This relative motion is detected as

blueshifts and redshifts that we detect from these stars.

The same is true of galaxies.

Spiral galaxies are found spinning and spiraling in space.

In fact, our own galaxy, the Milky Way,

takes about 240 million years to complete one full rotation.

When we look at other galaxies,

we can measure the light emitted at various points across

the disc to deduce the galaxy speed of rotation.

When measuring light from stars,

we see a shift in light towards shorter wavelengths from

the side of the galaxy approaching us, it's blueshifted.

If we look at the other side of the disc,

it's moving away from us,

we can see a shift of light towards longer wavelengths.

So its redshifted.

It's interesting to note that while one of our closest neighbors M31,

or the Andromeda galaxy is rotating,

we also see an overall blueshift of the whole galaxy,

implying that M31 is moving towards us.

While there are many other examples of the use of redshift and blueshift in astronomy,

the most well known Doppler shift in astronomy,

triggered the idea of the expanding universe.

In the early 1900's,

the prevailing theory was that the Milky Way,

our own galaxy, was pretty much the extent of the universe.

In the early 1920's,

an astronomer named Edwin Hubble,

was working at the Mount Wilson observatory in the USA.

He was making measurements of the distances of various Nebula,

only to find that some,

including what was then known as

the Andromeda Nebula were far too distant to be part of our own galaxy.

Instead these objects must be galaxies in their own right.

This meant that the Andromeda Nebula became known as the Andromeda galaxy,

the one just mentioned a few moments ago.

Although the idea of multiple galaxies had been proposed as early as the mid 1700's,

it is strange to think that the concept of galaxies is so new.

This idea was only conclusively proven about 100 years ago.

In 1929, Hubble continued these observations and found

a relationship between the distance and the redshift of galaxies.

Hubble found that galaxies that are outside of

our local group of galaxies have light that is red shifted.

Not only is the redshift is the light redshifted,

he also saw that the further away the galaxy is from us,

the larger the change in wavelength or the larger the redshift.

If the change in wavelength is interpreted as a Doppler shift due to the motion,

then Hubble's observations suggest that galaxies appear to move away from us.

Galaxies that are further away from us are moving away from us at a faster speed.

The modern interpretation of Hubble's observations is that the universe is expanding,

which it makes it look like galaxies are moving away from us.

The description of the expansion of the universe is called The Big Bang Theory.

The Big Bang explains the evolution of the universe after its beginning.

Thirteen point eight two billion years later,

we find ourselves here on the earth learning about Black Holes.

Speaking of which, if we are wanting to understand Black Holes,

we need to understand something about gravity.

For that, let's start with the simplest version, Newtonian gravity.

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