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.
08.04 – Advanced Illumination
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En provenance du cours de University of Alberta
Astro 101: Black Holes
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À partir de la leçon
Hunting for Black Holes
If black holes absorb all light, how do we see them? In this module, you will explore how astronomers observe real black holes, from studies of accretion discs and jets to the study of material orbiting a black hole.
Rencontrer les enseignants
Sharon MorsinkAssociate Professor
Department of Physics, University of Alberta
So to recap, we know that hot objects emit light by
producing a continuous spectrum known as a blackbody spectrum.
We know that low density clouds of hot gas emit light at specific frequencies.
We know that low density clouds of cold gas in between us and hot sources,
absorb light at specific frequencies.
Let's have a look again at a black-hole system with an accretion disk.
Can you guess what kind of light we will see from the hot dense accretion disk?
If you said that accretion disks emit black-body radiation, you'd be correct.
However, since accretion disks can become incredibly hot,
that is millions of Kelvin,
the peak wavelength according to Beams Law,
is not in the blue part of the spectrum,
it's not even the ultraviolet.
Accretion disks are so hot,
that many of them have a peak wavelength in the x-ray part of the spectrum.
We also previously learned that the black hole itself,
emits a type of radiation called hawking radiation.
Unfortunately, scientists have not yet measured any form of Hawking radiation.
Because the black-body radiation from the accretion disks of black holes
is phenomenally brighter than the light emitted through the hawking process.
In addition, the peak wavelength for hawking radiation emitted by solar mass black hole,
would be a couple of 100 kilometers long.
Which means that no radio telescope on Earth could detect it.
We previously mentioned the magnetic fields around black holes.
But we haven't done much into the physics of
their interactions with the matter and the black hole neighborhood.
The reason is that magnetic fields around black holes are poorly understood.
How they form, how they are powered,
and the effects they have on the light generated in the black hole environment.
We do suspect that magnetic fields are responsible for boosting the energy of
particles in the vicinity of a black hole by a process known as synchrotron radiation.
A magnetic field exerts a force on electrons and magnetic materials like iron filings.
We can easily see the effect of
a bar magnets magnetic field on
iron filings by bringing iron filings close to a bar magnet.
The magnetic field forces the iron filings to move.
They form a pattern that shows curves that
stretch from the north and south magnetic poles.
We call the lines that we see in this pattern,
magnetic lines of force.
An electron that moves across a magnetic field line feels a force that pushes
the electron into a circular path around the magnetic field line.
An electron that has some amount of
momentum also in the direction of the magnetic field line,
will experience the same effect.
But appear to be moving on a spiral path circulating around the magnetic field line.
Synchrotron radiation was first seen in laboratories that accelerate electrons.
These laboratory accelerators are called Synchrotrons.
So when the radiation was first observed in 1947,
it was called synchrotron radiation.
One modern synchrotron is the Canadian light source located in Saskatoon Saskatchewan,
capable of producing some of the brightest light on earth.
Synchrotron radiation is produced when electrons travel in curved paths.
Photons are emitted in the direction that the electron is traveling,
like the headlights of a car going around a curve.
I prefer to think about the screams produced on roller coasters.
They are loudest during the tightest curves.
Since spiraling electrons are moving so quickly,
they will naturally emit high energy photons due to the paths curvature.
When radiation is emitted in one direction,
we say that the radiation is beamed.
This is very different from black-body radiation,
which is equally bright in all directions.
Radiation that is equally bright in all directions is called isotropic.
Synchrotron radiation is generally associated with
the beam emission in black hole jets, which we'll discuss shortly.
The brightness of the light emitted at different wavelengths depends
on the strength of the magnetic field and the energy of the electrons.
One beautiful example of synchrotron radiation can
be seen in this true color visible light image of the Crab Nebula.
The Crab Nebula is a supernova remnant,
which has at its center,
a type of neutron star called a pulsar.
The pulsar is one of the bright white sources near the center of the image.
The faint blue light in this image is created by synchrotron emission from
electrons that have been accelerated by the neutron star strong magnetic field.
Depending on how fast the electrons are accelerated by the pulsar's magnetic field,
synchrotron radiation can also produce light in the form of radio waves,
x-rays, and even higher energy gamma rays.
But because this image is only visible light,
we can't see those forms of radiation.
The red light in the image is an emission line spectrum coming from excited hydrogen gas.
This image of the radio galaxy Cygnus A,
shows a bright point of light and two bright regions stretching out from the point
of light to about 100,000 light years in opposite directions.
The red color represents the radio emission,
showing that the central point of light is the location of a super-massive black hole.
The two bright regions are glowing due to electrons emitting synchrotron radiation.
Another process which modifies
the electromagnetic radiation present in
the environment surrounding a black hole is called Compton scattering.
When high energy photons,
like x-rays scatter off of electrons in a low density gas,
the photons can lose energy in the collision.
In Compton scattering, photons collide with electrons
like billiard balls bouncing off of one another on a pool table.
After the collision, the electron and the photon move off in different directions,
with the outgoing photon having lost energy to the electron.
The photon which has lost energy travels away
red-shifted with a longer wavelength and it started out with.
Scattering of photons off of electrons also takes place for other types of light.
Not just X-ray photons like we've seen in our description of Compton scattering.
For low energy photons,
like the light visible to the human eye,
the wavelength of the photons are much larger and quantum effects are less important.
For visible light photons,
the collision results in light changing direction but doesn't result in change of color.
A similar process to Compton scattering called inverse Compton scattering,
is well, exactly the inverse of Compton scattering.
Instead of a photon losing energy in a collision with an electron,
inverse Compton scattering describes a process which
results in an increase in photon energy.
When a photon collides with a high-energy electron,
the electron gives some of its energy to the photon.
This increases the energy of the photon resulting in wavelength being blue-shifted.
In order for inverse Compton scattering to take place,
a source of electrons which are moving close to the speed of light is required.
Regions near black holes such as the corona,
or places where inverse Compton scattering is likely to take place.
There are many more methods by which light can be emitted, absorbed, and shifted.
Some processes like synchrotron self-compton emission
are combination of the ones we just covered.
If electrons are spiraling around magnetic field lines at
relativistic speeds and emitting synchrotron radiation,
the photons emitted can then scatter off of
high energy electrons and gain even more energy.
We know our audience loves learning about changes the light but now we must
move on to determine where in a black hole system these sorts of processes dominate.
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