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.
10.05 – Detecting Gravitational Waves with Lasers on Earth
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Из курса от партнера University of Alberta
Astro 101: Black Holes
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Riding the Gravity Wave
How do you study a black hole that has no visible companion? In this module the student will be introduced to gravitational radiation. With the 2016 LIGO discovery of gravitational waves, a whole new branch of astronomy has been opened.
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Sharon MorsinkAssociate Professor
Department of Physics, University of Alberta
Gravitational waves are extremely weak.
These waves would be felt by a human,
for example, or any other living creature for that matter.
So in order to detect gravitational waves,
scientists must use the most sensitive instruments ever invented.
What devices are suitable for measuring incredibly small changes?
Well, lasers of course,
and that means we'll also need our good friend, the Michelson-Morely interferometer.
Remember interferometers leverage the wave nature of light
to measure the difference in lengths between different beam paths.
When coherent light, light that has the same phase such as laser light,
is split between two different paths and is later recombined,
its brightness will depend on how different the two paths were.
For example, if a red laser with a wavelength of
650 nanometers is introduced into an interferometer,
it will produce a bright spot at
the end of the detector if there's no difference in the beam path.
If one of the arms differ in length by half of the red wavelength or 325 nanometers,
the interference between the two beams produces zero light.
So small changes in the length of one arm of the interferometer can be
measured by the changing brightness of the resulting pattern of light at the detector.
The original Michelson-Morely interferometer was developed to determine if the flow of
ether caused a delay in one of
the device's two arms instead of the difference in the arms' lengths.
Like a boat travelling against the current of a river,
the theory of light back then predicted that moving
ether would cause a delay in the upstream arm.
The opposite was discovered;
that there was never any delay no matter what the orientation of
the device with respect to the motion through the supposed ether.
This proved that light waves don't require
a medium like ether to travel in and as a consequence,
the speed of light is a constant.
In order to leverage the sensitivity of interferometers,
astronomers built the Laser Interferometer Gravitational-wave Observatory,
whose acronym is LIGO,
pronounced "Ligo" or sometimes "Ligo".
These are two massively improved versions of
the Michelson-Morely interferometer built
on either side of the continental United States.
One detector is in Hanford,
Washington while the other is precisely 3,002 kilometers away in Livingston, Louisiana.
They each have two arms but instead of short meter long arms,
like the original Michelson-Morely interferometer,
each of the arms of LIGO is four kilometers long.
In addition to the length,
each arm bounces light from the laser source back and forth about 280 times making
each arm of LIGO equivalent to the length of 1,120 kilometers.
Why are LIGO's arms so long?
Well, it's hunting for some of
the weakest signals that the universe has ever thrown at us.
In fact, in order for LIGO to detect the strongest gravitational waves,
it needs to be able to distinguish a change
over the four kilometer length of its detector arms,
a difference in length 1,000 times smaller than the radius of a proton.
But one LIGO isn't enough to catch a gravitational wave,
we need at least two.
There are several major gravitational wave observatories in operation around the world.
The two LIGO observatories were the first,
followed by Virgo, and a host of others in
operation and under construction around the world.
If one LIGO detector is sensitive enough to measure a change in
its arm length down to the level below the width of an atom, why make more?
Well, the first and most important reason is noise.
Yes, sounds, footsteps, earthquakes,
and cosmic gravity quakes,
all register in LIGO as a change in the length of LIGO's arms.
In order to filter out footsteps from a colliding black hole,
you need a second detector.
LIGO second detector, built in Livingston, Louisiana,
has a different set of sounds, footsteps, and earthquakes.
But presumably, the two LIGO detectors would both see
the same gravitational wave coming from an intergalactic source.
To determine whether a wiggle in one LIGO detector is the result of a gravitational wave,
scientists compare the data from the second.
If there's a wiggle at nearly the same time,
remember the detectors are separated by 3,002 kilometers,
with nearly the same shape,
scientists can be confident that they really saw
a gravitational wave and not some researcher sneezing in the control room.
But there's another important reason to have
more than one gravitational observatory; direction.
With only two LIGO detectors,
an incoming gravitational wave will not have a well-defined direction.
Just like having two ears gives a stereo hearing,
two LIGOs let us determine approximately where the sources.
Although with only two,
there's still uncertainty about which direction it came from.
In order to pin down the source of gravitational waves,
a third gravitational observatory is necessary.
In the case of the Killenova explosion resulting from
the merger of two neutron stars in 2017,
the gravitational wave signal was also detected by
a third gravitational wave observatory, Virgo, in Italy.
With all three gravity wave observatories up and running,
most major astrophysical merges will be detected.
Over the next few decades,
these types of observatories will get more and more sophisticated,
detecting dozens of compact object collisions in the universe.
But things will get really interesting once we send
these massive observatories into space.
In order to really make the most sensitive gravitational wave observatories,
scientists work hard to remove sources of error.
Just like telescopes, which are better if they're on
mountain tops but best if they're in space,
a space-based gravitational observatory wouldn't have to worry
about earthquakes or someone tripping on a banana peel near the detector.
Know the next generation of gravitational observatories will be built in space.
The Laser Interferometer Space Observatory,
whose acronym is L-I-S-A,
universally pronounce it as "LISA" but I
would argue it should be pronounced "LISA" in this case.
LISA consists of three spacecraft which will
trail behind earth in its orbit around the Sun,
flying in a triangular formation.
Each of LISA's arms extend between the three spacecrafts.
Instead of a puny 1,120 kilometer effective arm length,
LISA will have three 2.5 million kilometer long arms.
LISA will still be sensitive to
small changes in the length between the arms but we'll have
an incredible sensitivity of 20 picometers over the 2.5 million kilometer long arms.
As a result, LISA will be able to detect
much smaller and quieter collisions than LIGO but also begin
probing into the processes by which compact objects are
captured by but not collided with black holes.
Beyond LISA, which won't even launch until the early 2030's,
future gravitational wave observatories will measure
the rotation of compact objects like pulsars.
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