04.06 – Supermassive Black Holes

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En provenance du cours de University of Alberta

Astro 101: Black Holes

122 notes

University of Alberta

Astro 101: Black Holes

122 notes

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.

À partir de la leçon

Sizing Up Black Holes

So far discussion has focussed on either the general case for black holes, of the stellar mass variety (endpoint of a star's life). In this module students will explore the various sizes of black holes and their measurable properties. Students will learn that there are four major types of astrophysical black holes (primordial/mini black hole’s, stellar mass, intermediate mass and supermassive black holes), and discover current theories on their formation, and what might feed them. Students will also gain an knowledge of ‘no-hair’ theorem and gravitational lensing. We will also explore the formation of supermassive black holes, intermediate mass black holes, and mini black holes in particle accelerators.

04.01 – Introduction1:07

04.02 – May the Schwarz(schild) Be With You6:34

04.03 – Dancing With the Stars12:57

04.04 – Weight Training5:30

04.05 – Stellar Mass Black Holes3:12

04.06 – Supermassive Black Holes10:53

04.07 – Intermediate Mass Black Holes8:27

04.08 – Super Tiny Black Holes2:43

04.09 – Summary: Preparing to Explore1:10

Interviews with experts - How do supermassive black holes form?3:11

Rencontrer les enseignants

Sharon Morsink
Associate Professor
Department of Physics, University of Alberta

Supermassive black holes are

the largest mass black holes and are found at the centers of galaxies.

Galaxies are large collections of stars ranging from

small galaxies consisting of hundreds of millions of stars,

up to the largest galaxies which can have upwards of 1 trillion stars.

Galaxies fall into several categories developed by astronomers based on their shapes.

Like spiral galaxies and elliptical galaxies.

There are also galaxies that don't fit into the standard classifications.

Our classification system has really become a zoo of galaxy types.

Among the unusual creatures in the galactic zoo,

active galaxies are those which are thought to host

a supermassive black hole at their center. Let's visit the zoo.

The galaxy NGC 7742 is an example of a Seyfert galaxy.

Seyfert galaxies are spiral galaxies,

with unusually bright central regions.

The properties of the light emitted from

the bright cores is not typical of regular star light.

Normally the light from a galaxy is mainly blackbody emission from the stars,

as we learned about earlier.

But the central regions of Seyfert galaxies also have

a bright emission spectrum which indicates extremely hot gas.

We will learn what an emission spectrum is in a later module.

The first Quasar discovered in 1963,

is called 3C 273.

In the first pictures taken of the quasar,

its features could not be resolved and it looked much like a star.

However, the properties of this star seemed very peculiar.

So it was called a quasi-stellar object.

This name was later shortened to QSO or quasar.

Modern images show that the quasar isn't a star but the ultra bright nucleus of a galaxy.

In the left picture,

the quasar is the very bright point of light in the middle of the box.

The spikes that are visible are artifacts of how the light is collected by the telescope.

You might be able to see faint light from the galaxy surrounding the bright quasar.

There is a jet of gas poking down into the right. In order to take a photo on the right,

the Hubble Space telescope placed a shield

over the bright light which allowed it to take a picture of the galaxy.

In 1929, astronomers observed a star-like object that they called

BL Lacertae or BL Lac for short.This thing also looked like a star through a telescope.

But its brightness varied so wildly that it could sometimes

be 15 times brighter than it was during the previous month.

At the time it was classified as a variable star.

But when better telescopes observed BL Lac,

evidence for a galaxy could be seen surrounding the bright point of light.

Other similar galaxies have since been discovered and they've been called BL Lac objects.

Since they seem very similar to the original.

More recently, astronomers have been calling these galaxies BLAZARS.

When Blazars are imaged,

we find them at the center of elliptical galaxies.

Galaxies are made up of lots of stars.

So we expect the light from a galaxy to look like the light from stars.

Stars emit most of their light in

the ultraviolet, visible, and infrared parts of the electromagnetic spectrum.

One thing that stars do not emit significant amounts of are radio waves.

That means that normally we would not detect much radio wave emission from galaxies.

However, a small fraction of galaxies emit lots of radio waves.

We call these galaxies radio galaxies.

Most radio galaxies are also giant elliptical galaxies.

Active galaxies that are part of this zoo,

share many similar properties.

Typically they have a bright central object called an Active Galactic Nucleus or AGN,

which is surrounded by the fainter stars that make up the spiral or elliptical galaxy.

Have a look at this diagram which represents

a unified model for all of these active galaxies.

The unified model for

an active galactic nucleus has a supermassive black hole at its center,

surrounded by a disc of gas that orbits the black hole and emits lots of energy.

In some cases there is a jet of gas shooting out from the central object.

We will learn more about discs and jets in a later module.

The model predicts that when you look directly down the jet you see a blazar.

If you look at the jet from an angle so that you can also see into the accretion disk,

then you see a radio loud quasar.

If you're looking at the edge of the disc

so that the inner part of the accretion disc is blocked,

you will see a radio galaxy.

If there's no jet then there will be

very little radio emission and you'll see a Seyfert galaxy.

Which is also something that could be called a radio quiet quasar.

So, the difference in the names you call

a supermassive black hole really just depend on your point of view.

One thing in common with all the active galaxies is that the supermassive black hole at

the center is consuming lots of gas enough to power their energy output.

The active galaxies are feeding their black holes,

which allows the black holes to grow.

The supermassive black holes may have started out as

large stellar mass or intermediate mass black holes

many billions of years ago and grew over time.

On the other hand, sometimes there's evidence for

supermassive black holes which aren't being fed tremendous amounts of gas,

like a supermassive black hole at the core of our own galaxy.

These black holes are quiet and much harder to detect.

So, just how massive are these supermassive black holes?

Although we can't put a black hole on a scale to figure out how much it weighs,

we can still measure its mass.

Kepler's laws of orbital motion apply to planets, stars, and black holes.

If we can find a star orbiting a black hole at the center of a galaxy,

then we can determine its mass.

The best example is the black hole known as Sagittarius A Star or SGR A star,

located at the center of our galaxy.

It is possible for astronomers to observe stars

orbiting in the region within a few light years of the center of our galaxy.

Astronomers have tracked the orbits of these stars for more than 20 years,

which can be seen in this video.

In this video, the center of our galaxy is marked with

the star symbol and the colored circles mark the position of the false coloured stars.

Over the years, the stars' paths trace out ellipses. Watch the star labelled SO2.

This star and the others moves faster

when it is closer to the black hole and slower when it is further out.

Just as required by Kepler's equal areas law.

The stars in this video orbit the invisible point at

the center of the galaxy in a manner similar to how the planets orbit our sun.

We can use Kepler's third law of motion to compute

the mass of the invisible object located at the star symbol.

The astronomers who measured the mass had to take into

account the three dimensional nature of the orbits of the stars.

The star SO2 takes 15.9 Years to make one full orbit.

When a star travels on an elliptical orbit,

the distance a, that appears in Kepler's law,

is equal to half of the length of the long axis of the ellipse. In the case

of SO2 the value of a is 1000 astronomical units.

Keplers third law for Sagittarius A Star is,

mass of SGR A Star plus massive SO2 equals A cubed divided by P

squared equals 1000 cubed divided by 15.9 squared equals 4 million solar masses.

The mass of SO2 is tiny compared to the mass of Sagittarius A Star.

So, we can approximate this as mass of SGR A star equals 4 million

solar masses.If you compare the distance

between SGR A star and the orbiting star to our own solar system,

a thousand astronomical units would be well beyond the orbit of the planets,

extending into the region where comets orbit the sun.

The closest star to us, Proxima Centauri,

is 200,000 astronomical units distant.

So, this is a gigantic mass packed into a tiny volume of space.

Whatever is located at the center of our galaxy can't be stars,

since we would be able to see them if they were there.

A black hole is the only plausible way to get such a large mass into a tiny volume.

Our galaxy's supermassive black hole is actually considered a small fry

in the heavyweight division compared to other galaxies' central massive black holes.

The giant elliptical galaxy M87 has a black hole at

its center that is approximately 7 billion solar masses.

You may have heard that galaxies have dark matter and may

be wondering whether the supermassive black holes could be the mysterious dark matter.

There are many reasons why supermassive black holes are not galactic dark matter.

The most important thing to know is that the mass of a supermassive black hole

is just a tiny fraction of the mass of the galaxy that it lives inside.

In addition, supermassive black holes are found at the center of a galaxy.

The dark matter in galaxies has a mass that is larger than the mass of all the stars in

the galaxy and is spread out throughout the whole galaxy

in a giant sphere that surrounds the galaxy.

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