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.
02.02 – The Stellar Nursery
Loading...
Do curso por University of Alberta
Astro 101: Black Holes
9 ratings
Na lição
Life and Death of a Star
Stars are the progenitors of black holes. In this module the student will learn about the lifecycle of stars, how stars produce energy, and how they radiate away energy. We will explore the death of stars, and what is produced by the death of stars, on all scales ; from the building blocks of life (carbon) to black holes.
Conheça os instrutores
Sharon MorsinkAssociate Professor
Department of Physics, University of Alberta
[MUSIC]
In order to fully understand the story of black holes,
it's important that we start at the beginning.
To know why black holes are formed,
we must first understand why the objects that form black holes are formed.
As stated in the introduction to this module,
stellar mass black holes are one of the two possible products
of violent explosions of high mass stars which occur at the end of a star's life.
These explosions, called Type-II or core-collapse supernovae
occur in stars at least eight times more massive than our sun.
When a massive star experiences a super nova event,
the amount of energy released is on the order of 10 to the 46th joules.
That's enough energy to last the sun at its present rate of
energy output 825 billion years.
For reference, our solar system, along with our sun, has existed for
just 5 billion years.
The universe has existed for a mere 13.8 billion years.
Clearly, that is a huge amount of energy.
If you're anything like me, right now you'd have a ton of questions starting
with how is it that some stars meet such violent ends?
How do stars even form in the first place?
Technically speaking, what is a star?
Let's begin by answering the simplest of those questions, what is a star?
Simply put, a star is a big ball of gas, a ball of gas which is gravitationally bound
and dense and hot enough to sustain a nuclear fusion reaction at its core.
Our sun is one such object.
It, like all of the main sequence stars,
produces energy by fusing hydrogen into helium in its core.
Most stars are spherical or if they happen to rotate quite quickly,
we call them oblate spheroidal, because they're slightly squished.
So now that we have a working definition of what a star is,
let's move on to the next question.
How do stars form?
Stars form in clouds of gas and dust which are particularly cold and dense,
at least by interstellar standards.
These regions are known as molecular clouds,
because their temperatures are low enough to allow molecules to form.
Molecular clouds are just one component of all the gas and
dust in the space between stars known as the interstellar medium or ISM.
What distinguishes molecular clouds from other gas and
dust in the ISM is the effect gravity has on them.
Molecular clouds are cold, between 10 and 30 kelvin and dense,
several hundred molecules per cubic centimeter.
Meaning there are plenty of particles in close proximity to each other,
at the same time relatively little gas pressure.
These two conditions are each very important for
star formation, as they allow the inward force of gravity to overpower the outward
force of the gas pressure.
And initiate the collapse of the cloud.
As the cloud contracts, it releases gravitational potential energy.
This energy is converted into thermal energy,
which in turn increases the pressure within the gas.
Without some way of removing thermal energy, the gas pressure would build and
eventually stop contraction of the cloud altogether prior to the formation
of a star.
What is needed then is a way to get energy out.
A way to get energy out so that gravity still has the advantage and
contraction can continue.
Thermal energy manifests itself in the random motions and
frequent collisions of molecules.
Collisions between molecules and the gas can excite the molecules,
allowing them to produce light that can escape the cloud.
And so without a buildup of thermal energy and gas pressure,
the cloud is free to continue contracting.
However, as contraction continues,
the central region within the cloud eventually becomes so
dense that light emitted by molecules and by dust grains has a hard time escaping.
More particles present in a given volume of the cloud means an increased likelihood
of absorption of the light by other molecules and
subsequent conversion of that energy back into thermal energy.
Over time, the cloud's increasing density will result in nearly
all of the radiation being trapped within the central region of the cloud.
When this radiation trapping occurs, pressure in the central region
increases to a level which slows the rate of contraction.
This is the formation of a protostar.
When observed through telescopes, protostars look much the same
as regular stars in that they have similar luminosities and surface temperatures.
The difference lies underneath, as protostars are not yet
hot enough to sustain fusion reactions.
In order to become hot enough to sustain fusion,
protostars must gather more material and squish it.
Materials surrounding the protostar feeds down unto it, and
at the same time gravity continues to slowly squish this protostellar material
into smaller and smaller regions.
As the protostar contracts and heats, the fusion rate increases.
And the heat generated by these nuclear reactions provides a pressure
force that slows the contraction caused by gravity.
When the core temperature of the protostar reaches about 1 million kelvin,
the winds generated at the protostar surface blow the surrounding gas and
dust away, ending the incretion phase.
Now without it's source of additional material, the protostar continues to
slowly contract and heat until the core temperature reaches 10 million kelvin.
At which point, fusion become stable and we have a star.
Fusion rates become stable because the forces in the interior of the star become
balanced.
Nuclear reaction rates are now high enough that they produce the necessary heat and
pressure to prevent the star from collapsing further due to gravity.
When the gravity and gas pressure forces are in balance,
we call this state hydrostatic equilibrium.
The net force on material within the star is zero.
The star can remain stable in this state for billions of years.
Our sun is currently about 5 billion years old, and
in a state of hydrostatic equilibrium.
It will remain in this stable state for another 5 billion years.
It's time again for us to confess about a lie of omission we've been telling.
Until this point,
we've been considering a scenario star formation which isn't perfectly realistic.
We've been considering a single cloud in isolation,
when in reality, individual sites of star formation are often influenced by other
nearby sites of formation and by nearby newborn stars.
In truth, large molecular clouds fragment as they contract into several smaller
cloud cores.
And from these, one or more stars form.
Often what we have is several neighboring sites potentially
each producing several stars, and then there's the matter of those additional
dynamical aspects we also forgot to mention.
More than just two forces are present in molecular clouds as they contract.
In addition to gravity and gas pressure,
magnetic fields affect molecular clouds by slowing their contraction.
Magnetic fields cause particles in a cloud to move in such a way
that they exert a friction on each other, hindering motion within the gas and
helping to prop up the cloud against gravity.
Turbulence also plays an important role.
Gas clumps moving relative to each other at large speeds act to
shear the cloud apart, rather than facilitate the cloud's contraction.
In the later stages of star formation,
materials surrounding the protostar will coalesce into a disk.
And the protostar itself will eject material from the system via large jets.
So suffice to say, star formation is very complex.
But star formation is also incredibly commonplace.
Several stars finish forming in our galaxy every year.
And in total, our galaxy contains roughly 100 billion stars.
And the key to our final question, how do some stars meet such violent ends,
lies in a variety of stars which result from the formation scenario.
Explore nosso catálogo
Registre-se gratuitamente e obtenha recomendações, atualizações e ofertas personalizadas.
O Coursera proporciona acesso universal à melhor educação do mundo fazendo parcerias com as melhores universidades e organizações para oferecer cursos on-line.
© 2018 Coursera Inc. Todos os direitos reservados.
