Q: What's the Difference Between a "Gravitational Wave" and a "Gravity Wave"?

The things that LIGO looks for are called gravitational waves (which are discussed in depth here on my blog and on the LIGO website).  That can be a mouthful, especially when having a conversation about them.  People, including us professionals, realize this and often take the shortcut of calling them "gravity waves".  It sounds so similar that this must mean the same thing, right?  Well, no!


GRAVITY WAVES ARE NOT GRAVITATIONAL WAVES

The proper technical use of gravity wave refers to waves on the interface of two fluids, which can be liquid and/or gas.  Where this boundary is disturbed, gravity will pull it down and buoyancy will push it up.  This combination of opposite push and pull creates a wave that moves out over the surface.  You can make your own interface of two fluids by filling a glass with some water and oil:

A glass containing oil and water.  Oil settles at the top because it is less dense (more buoyant).  [Source: Wikipedia]

Water and oil will separate if left alone.  This separation creates a boundary between the oil and water with the oil on top since it is less dense.  Now imagine gently tapping on the side of the glass.  The vibration from your tap will transfer into the separated oil and water which will produce a gravity wave on their boundary.  If you actually do this carefully enough, you can produce a gravity wave ONLY on the oil/water boundary and not on the surface of the oil (though a surface wave on the oil is technically a gravity wave too since that is a liquid/gas fluid boundary).

While the oil and water example technically illustrates a gravity wave, the term is usually applied to gravity waves that occur in nature.  Examples include:

• The waves on water caused by wind from large ocean waves to ripples in a puddle; these are examples of gravity waves on an gas/liquid boundary.  
• Waves of different density waters under the oceans' surface (like warm/cool water, or fresh/salt water); these are examples of a liquid/liquid boundary.
• The rippling of clouds, like in the movie below; this is an example of a gravity wave on a gas/gas boundary.

CAN A GRAVITATIONAL WAVE DETECTOR DETECT GRAVITY WAVES TOO?

We've now established that a gravity wave is very different from the gravitational waves that LIGO is looking for.  But can LIGO detect them anyway?  Indirectly, yes!  Almost three-quarters of the Earth is covered by oceans.  These oceans are roiling with gravity waves both within the water and on top of it.  When these waves encounter solid earth, much of the wave is reflected but some of the energy is absorbed.  This absorbed energy can then create surface waves on the remaining part of the Earth's surface that is solid.  These ground vibrations are called microseism.

Since LIGO lives on the Earth's surface (many people think that LIGO is underground but it really is built above ground), these vibrations shake the detector and contribute to the measured detector noise.  So much so that, compared to the gravitational waves we seek, we don't expect to be able to detect low frequency (less than about 10 Hz or so) gravitational waves.  And it doesn't matter that both LIGO detectors are near shores since the microseism shakes the entire Earth - we could have built LIGO in the middle of Nebraska and the microseism would still negatively affect us. 

In order to detect low frequency gravitational waves, we need to get away from the microseism.  The proposed gravitational wave detector that can do this is the space-based eLISA satellites.  (I've also discussed eLISA and associated drama on this blog previously.)  eLISA would be exclusively sensitive to low frequency gravitational wave and would compliment LIGO well: there are many young systems producing low frequency gravitational waves all the time while there are few producing the high frequency death throes that LIGO can detect.  Together, LIGO and eLISA will provide a more complete gravitational-wave picture of the life cycle of some of the most energetic, violent objects in the Universe.


CONCLUSION

"Gravitational waves" and "gravity waves" are very different entities.  However, you may hear us refer to a gravitational wave as a "gravity wave".  This is a personal pet peeve of mine (can't you tell?).  While I work hard to use the term "gravitational wave" correctly, I am often hesitant to say anything to colleagues I hear using "gravity wave" instead.  Watch the NSF documentary Einstein's Messengers (also on the "Viewing Fun" page on this blog) and you will see some highly respected LIGO scientists refer to "gravity waves"; it makes me cringe a little every time but I'm not one to gainsay my betters.  Now that you've read this, you'll know what we really mean ;)


Read more:

• Another explanation of the difference between gravitational waves and gravity waves (this is correct but a little outdated on its discussion of gravitational waves)

Q: If Light is Stretched/Compressed by a GW, Why Use Light Inside LIGO?

Wow!  It's been a while since I've posted...  After the start of a new semester (I have 150 students in the class I am teaching at LSU) and Hurricane Isaac (which shut LIGO Livingston down for almost a week, LSU for 3 days, and left me without power for a while), I am just getting my life back to a somewhat normal routine.  I love even the hectic parts of my life, but I've missed writing about gravitational waves here on Living LIGO!


Q: IF LIGHT IS STRETCHED/COMPRESSED BY A GRAVITATIONAL WAVE, WHY USE LIGHT INSIDE LIGO?

Today I am addressing a question that many professional physicists fully don't understand!  I wrote a little while ago about how light and gravitational waves will stretch out as the Universe expands (this is called redshift).  If an object is coming towards us, its light is compressed (and this is called blueshift).  Basically, if objects are moving, light and gravitational waves will experience a Doppler effect.  I have also written about how a passing gravitational wave will stretch and compress space in perpendicular directions.  When you put these two facts together, you come to the conclusion that the light inside the arms of LIGO is also be stretched and compressed by a gravitational wave.  So, how can we use this light to measure gravitational waves when the light itself is affected by the gravitational wave?

Like I suggested earlier, this is not obvious upon first inspection.  The apparent paradox arises from thinking of laser light as a ruler.  When you think of light, you usually think of it as a wave (which it is, but light is also a particle - however that isn't relevant to this discussion).  Waves have a wavelength -- the distance between each successive wave:

Illustration of wavelength (represented by λ) measured from various parts of a wave. [Source: Wikipedia]

A passing gravitational wave will expand and compress space-time and the wavelength of the light we are using to measure gravitational waves is itself affected by the gravitational wave.  Since LIGO and detectors like it effectively measure the length of its arms and compares them to each other,  how can we rely on light to measure any length changes from a passing gravitational wave?

The solution begins to become clear when you start thinking of the laser light as a clock instead of a ruler.  When the light comes out of the laser, there is a fixed time between each crest of the wave (this is called the period of the wave).  Let's label each crest as 'tick' (like a clock).  Our laser (labeled 'Laser' in the image below) is very stable in that it produces a very consistent wavelength of 1064 nm (near-infrared light).  Because the speed of light is constant no matter how you measure it, that means that there are almost 282 trillion (2.817 x 10¹⁴) 'ticks' every second.  This light is then split into two equal parts (at the 'Beam Splitter' in the image below), one for each arm.

Basic diagram of the LIGO detectors.

Since different things can happen to the light once it is in the arms, let's reference the beam splitter for making length measurements (i.e., let the beam splitter stay in the same place while the gravitational wave alternates squishing and stretching the arms).  A real gravitational wave will cause one arm to shorten and the other to lengthen.  This will also cause the laser wavelength in the shortened arm to decrease (blueshift) and the wavelength in the lengthened arm to increase (redshift).  But there is nothing in the detector that measures wavelength.  What it really measures is the shift in the arrival time of each 'tick' of the wavelength crests.  If the arms stay the same length (no gravitational wave), then the 'ticks' of the laser light come back to the beam splitter at the same time and produces destructive interference where we measure the light (labeled 'Photodetector' in the image above).  If a gravitational wave causes the length of the arms to change and shifts where the 'ticks' of the laser light occur, the two light beams will no longer return to the beam splitter at the same time.  It is this "out of sync" arrival time of the crests of the laser light that produces the interference patter we utilize to detect gravitational waves - we couldn't care less about the actual wavelength of the light (other than it was consistent going into the detector).


READ MORE FROM OTHER LIGO SCIENTISTS:

A wonderful, concise summary on why light can be used in gravitational wave detectors like LIGO has been published in American Scientist here.  The author, Peter Shawhan, is an associate professor at the University of Maryland, College Park.

There is also an article in the American Journal of Physics (vol. 65, issue 6, pp. 501-505) titled "If light waves are stretched by gravitational waves, how can we use light as a ruler to detect gravitational waves?"  This is a more technical article by Peter Saulson who is a professor at Syracuse University.

The Journey of a Gravitational Wave III: GWs Stretch Out

What happens to a gravitational wave between when it is produced and when LIGO can detect it?  It turns out not much, which makes it a key new medium in which to observe the Universe!

Today I will be discussing how a gravitational wave can get stretched during its journey to Earth.  Previously, we have discussed how gravitational waves can be bent away from a straight path and how things cannot absorb or reflect a gravitational wave.


THE DOPPLER EFFECT

If you have ever been passed by an ambulance or police car with its sirens on, then you likely noticed that as the sound from the siren approached you, the tone was higher than when the siren passed you.  This is due to something called the Doppler effect.  As the source of a sound is moving toward toward you, the distance between the sound wave's crests (wavelength) are compressed, resulting in a higher frequency.  We hear higher frequencies as higher tones.  Conversely, when the source of a sound is moving away from you, the sounds wave's crests are stretched apart resulting in a lower frequency and a lower tone.  Consider the following animated example:

Animated example of the Doppler effect: how motion and cause the wavelength of sound to be affected.
[Image from Wikipedia]

In the beginning of this animation, the car is not moving and the sound waves have the same wavelength both in front and behind the car.  Once it starts moving forward (to the left), the sound waves in front of the car are closer together and the sound waves behind the car are farther apart.  This results in us hearing a higher tone when you are in front of the car and a lower tone when you are behind the car.


COSMOLOGICAL REDSHIFT

This Doppler effect can also affect the wavelength of light and of a gravitational wave depending on the motion of the object creating the waves.  First, let's think about what happens to light.  As the source moves toward you, the wavelength of the light will get shorter.  Since we can't hear light, instead of hearing a higher tone, we will see the light to be shifted toward the blue end of the spectrum (where the shortest wavelengths we can see are).  This is called blueshift.  For a source moving away from us, the wavelengths would be longer and we would see the light shifted toward the red end of the spectrum (where the longest wavelengths we can see are).  This is called redshift.

We can measure this cosmological Doppler effect by measuring the spectral signatures of stars.  Below is an example of such a spectral signature.  Stars give off almost every color of light, but there are particular colors that get absorbed by different elements before that light can make it to Earth.  Those absorbed colors show up as dark lines in an otherwise complete spectrum of colors:

The optical spectrum from our Sun (left) compared to the optical spectrum of a supercluster of galaxies (right).  Note that there are similar dark lines (from absorption of those wavelengths by different chemical elements), but the lines on the right are shifted toward the red end of the spectrum.  This phenomena is called "redshift" because of this.  [Source: Wikipedia]

The spectrum to the left is what we observe from our local star, the Sun.  The spectrum on the right is from a distant cluster of galaxies (containing many stars).  Note that the spacing of the dark lines is essentially the same, just shifted toward the red end of the spectrum (this is highlighted by the arrows).  That means that this cluster of galaxies is moving away from us.  Just about everything (but not quite) in the Universe shows this redshift which implies that the Universe is expanding!  (There is more than one cause of redshift, but we will only be discussing the redshift due to the expanding Universe in this blog post.)

Redshift is measured by the change in wavelength of light (or a gravitational wave) divided by the wavelength of light if the source wasn't moving.  For the spectrum example here, this would be the amount the color of the light changed (the difference between the right and the left side) divided by its original color (the left side).  The redshift is a result of the Doppler effect; it can also be used to measure an object's velocity.  To do that, we need to determine the proportionality constant between redshift and velocity.  This constant is known as the Hubble constant, H (named after Edwin Hubble who first determined this relationship).  The best estimate of this constant is currently:

H = 71.0 ± 2.5 km/s/Mpc
        67.2 ± 1.2 km/s/Mpc
(revised on 20 March 2013 with the parameters released by Planck)

This means that for every light-year away an object is, its velocity away from us increases by about 257 feet/hour.  (This may not sound like much, but a light-year is really a very small distance in the Universe; our own galaxy is about 110,000 light-years across!)  This expansion is believed to have originated with the Big Bang.  So, will the Universe expand forever?  Will it slow to a stop?  Will it stop expanding and start shrinking until everything is a compact ball again (this is called the Big Crunch)?  From current observations, the ultimate fate of the Universe appears to be an eternal slowing expansion which will cause all of the energy to be evenly distributed throughout this even larger Universe (compared to now).  That means that there won't be enough energy in any one place to make anything happen (all events in the Universe need an imbalance in energy).  This is called the Big Freeze or the heat death of the Universe.  However, more observations (especially of things like dark matter and dark energy) of our Universe are needed before we can be sure of the Universe's future.

BLUESHIFT

There are a few things in our Universe that are moving towards us and therefore have a blueshift.  Of most note is the Andromeda Galaxy which is moving towards us at about 300,000 meters/s (671,801 mph).  This is because our Milky Way Galaxy and the Andromeda Galaxy are gravitationally bound to each other; this means that the gravitational attractions between these two galaxies are greater than the expansion of the Universe.  In the future, our two galaxies will collide, but not for an estimated 4.5 billion years.  This is also about the time the that our Sun will become a red giant and all life on Earth will be extinct by then anyway!  I wouldn't stress about it if I were you :P

Also, portions of rotating galaxies can be blueshifted.  In this case, the side that is rotating toward us will be blueshifted and the part that is rotating away from us will be redshifted.


GRAVITATIONAL WAVES AND REDSHIFT

Just like redshift stretches out the wavelength of light, the expansion of the Universe will also stretch out the wavelength of a gravitational wave during its journey to Earth.  In a previous post, I discussed what gravitational waves would sound like if you put their signal through a speaker (remember: gravitational waves don't make sound!).  So, I decided I wanted to hear what the change in the sound of a gravitational wave is due to different amounts of redshift.  I did the calculations, generated the sounds, and assembled them into the video below for your viewing pleasure:

So, how can we make use of the redshifting of a gravitational wave to learn more about our Universe?  Well, most astronomers and physicists don't believe that the rate of expansion of the Universe (the Hubble constant, H, above) has been the same since the Big Bang.  Particularly, there is a period believed to have existed in the past history of the Universe called inflation which is a time of rapid expansion.  From a certain kind gravitational wave source, we will be able to measure the Hubble constant around the neighborhood of the source.  This will be a direct probe of how the expansion of the Universe (the Hubble constant) has changed through the history of the Universe because observing objects in the distance is the same as observing them as they were in the past (e.g. observing an object 1 light-year away is the same as observing it as it was a year ago since light and gravitational waves travel at the speed of light - at least gravitational waves are expected to travel at the speed of light!).

The Journey of a Gravitational Wave II: GWs Get Bent

What happens to a gravitational wave between when it is produced and when LIGO can detect it?  It turns out not much, which makes it a key new medium in which to observe the Universe!

Last week, I began discussing what happens to a gravitational wave as it makes its way from its source to Earth; specifically that gravitational wave can travel through matter and come out the other side unchanged!  Today's post talks about how the gravitational effects of other masses in the Universe can deflect the gravitational wave from its otherwise straight path.


GRAVITATIONAL LENSING

Let's think again about what happens to light on its way to Earth.  We know from the last post that any matter light comes into contact with will reflect or absorb at least part of the light.  There is also another effect called gravitational lensing that causes light to bend around massive objects due to the massive object's gravitational influence.  This is caused by light following its natural path on curved spacetime (or light being bent by a gravitational field since we've previously established that the curvature of spacetime is a representation of the strength of the gravitational field there).  The first thing that pops into my mind that illustrates something following its natural path on a curved surface is miniature golf:

This is hole 13 at Safari Mini Golf in Vero Beach, FL.  This image is taken from a review of this course and can be read here.

Consider the example hole in the above image.  After you get your ball past the three bumps, there is a wonderful bowl-like curved portion behind the target hole (if you look very closely, you can see the hole directly after the last bump and in the center).  If you hit your ball into this area, the ball's trajectory will change from a straight path to a curved one.  If your ball begins its path on the left side of the bowl, it will curve right; if your ball enters the bowl from the right, it will curve left.  The same thing happens for light and gravitational waves that pass by a massive enough object to cause a significant depression in spacetime (i.e. a strong gravitational field):

The bending of light from a star that is really behind the Sun but appears to be to the side of the Sun.
[Credit: Ethan Siegel of Lewis & Clark College, OR]

The the light from a star, galaxy, or other source travels through the depression in spacetime made by a nearby massive object (in the image above it is the Sun).  The path that light takes is curved just like the golf ball in the miniature golf example above.  But our brains are wired to assume that any light that enters our eyes has come to us in a straight line (which is how light usually travels) so we perceive the location of the source to be directly behind where it appears to be.  Therefore, while the star is really behind the Sun (at point A in the image above), it appears to us to be to the side of the Sun (at point B).  This bending effect is called gravitational lensing and it applies to gravitational waves just like it does to light.


KINDS OF GRAVITATIONAL LENSING

The example of gravitational lensing given above was one of the first observational proofs that Einstein's general relativity was correct.  Before relativity, there was already a prediction of the bending of light due to Newtonian gravity (what we use in our everyday life) but Einstein predicted the bending effect should be twice that predicted without relativity.  In 1919, there was a total eclipse of the Sun which would allow those stars that are near the Sun to become visible.  Images of the eclipse were taken and it was seen that the shift in the position of stars near the Sun was indeed twice that of the shift predicted by Newtonian gravity.

There are also kinds of lensing that produce much more dramatic effects than shifting the position of stars!  Things like large galaxies and clusters of galaxies can cause the light from objects behind them to be split up to form multiple, separate, and complete images. 

[Image from NASA]

The image above shows gravitational lensing of a quasar and a galaxy by a distant galaxy cluster SDSS J1004+4112 (SDSS indicates that it was discovered by the Sloan Digital Sky Survey).  Each image of the quasar is of the same single object; the same is true of the galaxy! 

You may notice that each of the images are a little different from each other.  This is due to the distortion that a gravitational lens can cause.  This effect is illustrated well in the simulation below of a black hole creating a gravitational lens as it passes in front of a galaxy:

[Image from Wikipedia]

Note the circular distortion of the light from the galaxy as the black hole passes by.  When the black hole is directly in front of the galaxy, there is a circular halo of lensed light around it.  This halo called an Einstein Ring can can be caused by any extremely massive object (black hole, galaxy, galaxy cluster, etc.).

[Image credited within the image and retrieved from Wikipedia.]

HOW LENSING AFFECTS THE SEARCH FOR GRAVITATIONAL WAVES

Gravitational lensing affects both light and gravitational waves.  This produces spectacular images of objects using light, but LIGO will not produce images and the sources that produce gravitational waves are more point-like (a black hole, a star exploding, etc.) than large scale objects (like galaxies which are thousands of light-years across).  The effect that will most likely be seen in gravitational waves is their focusing; the bending of gravitational waves can produce more intense gravitational waves from the lensed source (similar to a magnifying glass focusing light to a smaller point).  This paper suggests that the galactic center of the Milky Way could increase the intensity of a source in our galaxy (bur behind the galactic center) up to 4000x.  Also, if a gravitational wave is emitted from a galaxy that has multiple images from lensing, then that gravitational wave will come from each image!

However, most sources will not have appreciable lensing.  While this is something we will always need to consider while conducting gravitational-wave astronomy, it isn't something that is likely to change the information contained on the gravitational wave noticeably (and that's a good thing)!

The Journey of a Gravitational Wave I: GWs Cast No Shadows!

What happens to a gravitational wave between when it is produced and when LIGO can detect it?  It turns out not much, which makes it a key new medium in which to observe the Universe!

In order to make this information more digestible, I will address one aspect of a gravitational wave's journey through space.  Today's topic discusses how the Universe is essentially transparent to a gravitational wave.  Future editions will discuss how matter can bend gravitational waves (gravitational lensing) and how the expanding Universe can stretch out (redshift) gravitational waves.


GRAVITATIONAL WAVES CAST NO SHADOWS:

First, let's think about what happens to light.  As light travels through the Universe, any time that it encounters other matter, some of the light is absorbed by the matter or reflected away from its original path.  The opposite happens for a gravitational wave; it can pass through matter and come out the other side unchanged (although there are some negligible effects)!  That means that there is no such thing as a gravitational-wave shadow and nothing can obscure our detection of a gravitational wave!


The Spacetime Explanation:

But why is this?  In a previous post, I described a gravitational wave as a change in the gravitational field moving out into the Universe.  This change in gravitational field is often illustrated as a ripple, or wave, on spacetime (where the steepness of the curvature of spacetime represents the strength of the gravitational field, or the gravitational force a mass would feel, there).  Let's look at what the Earth sitting on space-time looks like:

This picture isn't a perfect representation since the size of the Earth will affect the shape of the depression and this has no effect on real spacetime.  Also, this is a simplified 2-dimenional representation of 3-dimensional (or a snapshot of the 4-dimensional spacetime) space.  But if you were to imagine giving a corner of this flexible grid (spacetime) a swift shake, the Earth in the middle would be affected by it but it would not impede the wave.  So, this is an example of how matter doesn't interact with gravitational waves, but I am still somewhat unsatisfied with this since you may think that the Earth will bounce after a wave passes creating more waves of its own (here is another aspect where this representation of spacetime is not perfect).

FYI: A better 3-dimensional representation of spacetime is shown in this clip from the American Museum of Natural History's short documentary called Gravity: Making Waves (which can be seen in its entirety on my Viewing Fun! page).  This animation shows a grid-like scaffolding filling space in which there is a depression caused by mass.  While it still isn't a perfect representation of spacetime, it is much better than the trampoline approximation above.

The Lunar Eclipse Explanation:

Recently, I thought of another more intimate example that most of us can identify with: a total lunar eclipse (which I have also blogged about).  This is a situation where the Sun, Earth, and Moon line up in that order so that the Moon is completely in the Earth's shadow:

Image from Wikipedia

When the Moon is completely in the Earth's shadow (or the umbra in the diagram above), a viewer on the Moon would not be able to see any part of the Sun.  If the gravitational field from the Sun were blocked by the Earth, then the Moon's orbit would appear to change.  Since there is no change in the Moon's orbit during a total lunar eclipse, then the Earth does not block the Sun's gravitational field.  By extension, the Earth also would not be able to block any changes in the gravitational field (which are gravitational waves).  If you are familiar with physics, this is an application of the principle of superposition.


Great!  But Why do We care?

Since mass does not absorb or reflect gravitational fields, the Universe is transparent to a gravitational wave.  This is a huge advantage when using gravitational waves to make astronomical observations since nothing can block our view of a gravitational wave!  If you have ever seen the our own Milky Way galaxy in the sky on a clear, dark night, you've seen the billions and billions of stars that live in our "backyard": 

Fish-eye mosaic of the Milky Way galaxy as seen from Chile.  [Image from Wikipedia]

While this is beautiful, it also it almost impossible to see past all the stars and dust there to observe what is behind our "backyard".  We will be able to see right through the Milky Way with gravitational waves! 

P.S.  We can also detect gravitational waves from the other side of the Earth with LIGO since gravitational waves can travel through matter.  Read more about this in this previous post (under the subheading of "Why are there 2 LIGOs?")!

What Is a Higgs Boson?, What Did CERN See?, and Why It's a Big Deal!

This is my disclaimer - I AM NOT A PARTICLE PHYSICIST!  Therefore, this subject does not fall into my realm of expertise.  However, I do have a very basic training in the physics behind all of this so I would like to share with you a little bit about why all of us physicists have been so excited of late...


WHAT IS A HIGGS BOSON?

The Higgs boson (regular Wikipedia entry, Simple English Wikipedia entry) is the elementary particle that gives matter mass.  Many of us have probably heard about Einstein's famous equation:

This image is taken from Wikipedia.

While this equation is famous, the true meaning behind what it means is often not fully appreciated (I used to see it and simply think "Einstein!").  It means that mass can be converted to energy and energy can be converted to mass, also known as the mass-energy equivalence.  The energy, E, from an amount of mass, m, is equal to the mass multiplied by the speed of light, c, squared (c² = c*c, c is about 670,616,629 miles/hour).  If you were to convert 1 oz of matter into energy, you would have about 2,500,000,000,000,000 Joules of energy and this would keep a 100 W light bulb lit for over 807,389 years!  So, a little bit of matter can be converted into an immense amount of energy!  It is this conversion of mass to energy that makes nuclear weapons so destructive.

But, if we convert energy into mass, where does this mass come from?  The Standard Model, which is the working description of how the fundamental particles interact (I talked about this in my post discussing gravitons), says it comes from the Higgs field.  This is a field similar to the electric field and the magnetic field (more on fields in general here).  At the instant after the Big Bang, all particles moved at the speed of light (c from above) since none of them had mass because there was no Higgs field.  In the next instant (about a trillionth of a second later), the Higgs field came into existence and produced a resistance to particles based on what they were made of.  This resistance manifests itself as mass: the slower a particle moves through the Higgs field, the more massive it is.  The Standard Model also allows fields to manifest themselves as particles (the photon is the particle associated with the electric and magnetic fields).  Therefore, this Higgs field should also manifest itself as a particle and we call it the Higgs boson.

The only particle from the Standard Model that has not been detected is this Higgs boson.  (Note that gravity is not described by the Standard Model.)  This is because the Higgs boson is very massive for a fundamental particle at about 133 times the mass of a proton.  The amount of energy conversion needed to produce this mass is much larger than we have been able to create in the past.  That is, until CERN built the Large Hadron Collider (LHC)...


WHAT DID CERN SEE?

View of the CMS experiment [note the person near the center] (© CERN)

CERN is the home to several experiments including CMS and ATLAS.  Both of these experiments smash together protons with very large energies.  The protons and their energy can change into a Higgs boson (if there is enough energy).  The Higgs boson decays (changes into something else) almost immediately, so the LHC experiments look for the Higgs boson's signature in the resulting particles.  There are 5 pairs of particles that result from the decay of a Higgs boson, including 2 photons.

Both CMS and ATLAS saw the Higgs signature in 2 of the 5 different resulting decay pairs.  Only CMS had sufficient data to look for all 5 kinds of decay pairs and saw with high certainty signatures in 4 of the pairs.  More research is needed for the signature CMS didn't see.

Diagram of the ATLAS experiment [note the people on the bottom left] (© CERN)

WHY IT'S A BIG DEAL!

The official conclusion is that CERN has indeed observed a Higgs-like particle.  "Higgs-like" does not mean that they are unsure if they found what they were looking for.  Instead, it appears that the Higgs boson they observed has more properties to it than the Standard Model predicted.  The LHC has found what it is looking for as well as hints that there is new physics to be discovered.

So this is the big deal: the population of the Standard Model is complete but the model itself doesn't appear to describe everything.  That is something we knew before, but now we are seeing it with the apparent complication in what was and wasn't observed in the discovery of the Higgs boson.

I am a physicist because every time you discover something new, not only do you understand the Universe better, but you have even more exciting questions to answer!  Soon enough, it is going to be gravitational waves stirring up excitement like this and I am going to be in the midst of it all!


Side Note:
IT'S NOT THE 'GOD PARTICLE'

The Higgs boson is sometimes referred to as the "God particle," especially by the media.  However, it has nothing more to do with God than any other particle in the Universe.  The origin of this misnomer is a book by Nobel Laureate Leon Lederman titled The God Particle: If the Universe Is the Answer, What Is the Question?.  Likening the Higgs boson as a God particle refers to it being the origin of all matter's mass.  Physicists (like me as well as Lederman himself) generally dislike this nickname since it places much more import on this particle than it deserves.  But above that, it is offensive to people of faith and makes us look like we are trying to replace God.  We aren't. 


Want More? ...
Watch the announcement seminar
Read the official CERN press release

Q: What Do Gravitational Waves "Sound" Like?

Okay, this isn't a question that I usually get asked but the answer to this question is the basis of my answer to questions about how we can determine information about what produced a gravitational wave from the signals we detect.  So, how do we do that?

One convenient feature of LIGO is that it is most sensitive in the frequencies that the human ear could hear if gravitational waves made sound - but they don't.  I can't stress this enough: gravitational waves do NOT make sounds since a sound waves are fundamentally different from gravitational waves.  But, if we take the data we gather from LIGO of a gravitational wave, we can put that signal through speakers and convert them into sound.  In this way, LIGO is very much like a gravitational-wave radio...


LIGO AS A GRAVITATIONAL-WAVE RADIO

Radio stations broadcast radio waves at a specific frequency (this is the number that you tune your radio to) and music is encoded onto this wave.  Whereever you are right now, you are most likely surrounded by radio waves from numerous stations but you can't hear radio waves or the music that is encoded onto them.  To hear this music, you need to have an instrument that can detect the radio waves, decode the music from them, and turn this signal into sound using a speaker.  Now, you can hear the music.

LIGO is a completely passive detector (meaning we just wait for something to happen, we cause nothing that we can detect other than noise) just like your radio is passive (it can't create music).  We wait for a gravitational wave to pass by Earth, and if it is strong enough and in the frequency range that we are sensitive to, then LIGO will detect a signal.  From that signal, we can extract information about what made the gravitational wave, like a radio decodes the music from the broadcast radio waves.  Once we have detected the signal, we can put that signal through speakers to convert it into sound.  Just like a radio, it is the speakers that make the sound and not the detector.  Since LIGO is sensitive to frequencies that are in the same ranges of sounds we can hear, we can hear the gravitational-wave signals when put through a speaker.  Now we can extract information about what made the gravitational wave just like we can hear the different instruments and voices in music.


LIGO'S SENSITIVE FREQUENCIES = AUDIBLE FREQUENCIES

Initial LIGO's most sensitive range (as we were before we started our current upgrades) was between about 60 Hz to 800 Hz.  This corresponds to the lowest note on a cello (click here to hear what 65.41 Hz sounds like) to the lower notes on a piccolo (click here to hear what 523.25 Hz sounds like), respectively (according to Wikipedia).  Once Advanced LIGO is complete and operating at sensitivity, it will be more than 10x as sensitive as Initial LIGO and its most sensitive region will be between about 20 Hz to 2000 Hz (this is the range that produces at least 10x the sensitivity of the sensitive range noted for Initial LIGO).  This corresponds to the lowest frequencies humans can hear (like the lowest note on a tuba) which is usually felt more than heard to a little below the highest note on a flute (click hear to hear what 2093 Hz sounds like).  LIGO's sensitivity to different frequencies are shown graphically below:

LIGO sensitivity vs. frequency (see this post for a description of how to interpret this plot).
Click on the graph to see a larger image.

Recall from a previous post that it is because LIGO is most sensitive to the audible frequency range that we cannot detect gravitational waves from the Moon, Sun, and planets; they produce gravitational waves at much lower frequencies.


THE "SOUNDS" OF DIFFERENT KINDS OF GRAVITATIONAL WAVES

We can tell just from what a gravitational wave "sounds" like what category it is classified as; there are 4 major categories:

1. Inspiral gravitational waves: two massive objects orbiting each other faster and faster as they get closer together and eventually merge into one.  Pairs of neutron stars, black holes, or the combination of the two are prime candidates for detection.
     ⇒These waves are expected to sound like a "chirp" (click here to hear the example in the plot below):





2. Continuous gravitational waves: a distorted object rotating about its axis with a constant frequency (the Earth rotates with a very constant frequency of once per day).  A neutron star rotating rapidly with a "mountain" on it are prime candidates.  ("Mountain" is in quotation marks because it is a deformation as little as a few inches high on the nearly perfectly spherical neutron star.)
     ⇒These waves are expected to sound like a single tone (click here to hear the example in the plot below):





3. Stochastic gravitational waves: many weak signals from different sources combining into one "jumble" of a signal.  Relic gravitational waves from the Big Bang are expected to be candidates for detection.
      ⇒These waves are expected to sound like static noise (click here to hear the example in the plot below):





4. Burst gravitational waves: these waves are short duration and from unanticipated sources or from known sources where we can't be sure what the gravitational waves will "sound" like.  I like to call these the gravitational waves that go 'bump' in the night.
      ⇒These waves are expected to sound like 'snaps', 'crackles', and 'pops' (click here to hear the example in the plot below):

While is is great to see and hear the differences between the different kinds of gravitational waves, it is harder to see how we can glean more specific information about the thing(s) that made the gravitational wave.  The answer is that we can use general relativity to predict what kinds of signals ("sounds") a certain situation will create.  Below is a movie by Steve Drasco (Caltech/CalPoly) showing the sped up evolution of a body 270 times the mass of our Sun orbiting and finally merging with a supermassive black hole 3 million times the mass of our Sun.  The movie starts one year before the two objects merge and the bottom of the frame shows a graph of the gravitational waves while the majority of the frame shows the orbit of the system.  As you listen, you can hear how the tone changes into the chirp that is characteristic of this kind of system (the movie is ~13 MB so it may take a minute or two to load):

 

By studying the predictions of what different gravitational waves will "sound" like, we can translate a detected gravitational wave into information on the system that made it.


DO WE ACTUALLY LISTEN FOR GRAVITATIONAL WAVES?

Yes and no...  The option to listen to the data as it is collected is available to scientists working in the LIGO control room.  I've done it but I don't make a habit out of it since almost all of what LIGO detects is small vibrations from our environment.  You can listen to real LIGO noise by clicking here (if you carefully listen all the way to the end, you can hear a fake inspiral chirp that has been added to the data - you may miss it).  Since what you predominantly hear sounds like static, it can lull you to sleep which isn't advisable when you are the responsible scientist on duty!  Also, almost all gravitational waves will be too weak to hear with our ears which is why we mainly analyze data using sophisticated data analysis techniques that have been specially designed to search for each of the four categories of gravitational waves.  (This is what I do for a living!)

I also wrote in March 2011 about a fake signal that was placed (injected) into the LIGO data to test if our data analysis techniques could really detect a gravitational wave if there was one.  This was a blind test (called the "Big Dog" due to its apparent location in the constellation Canis Major) meaning that only a few individuals knew about this fake signal and the rest of us were left to find it and interpret its results.  While we did not detect this signal by listening to it, it can be heard in both the LIGO detectors (about 17 seconds into the recording linked below).  This is real LIGO data and the sound may be VERY LOUD - so turn your volume down before you play it and then adjust it!
     ⇒Click here to hear the data around the blind injection for LIGO Hanford, WA.
     ⇒Click here to hear the data around the blind injection for LIGO Livingston, LA.*
          *Note that there is a audible instrumental "glitch" in the Livingston data about 8 seconds into the recording; this is unrelated to the injection.

While it is difficult to hear gravitational waves that will be buried in detector noise, there is no denying that the human brain is very effective at breaking sounds down into their individual components.  A recent Physics Today article titled "Shhhh.  Listen to the Data" discusses the advantages of humans listening to data and features a discussion of this application to LIGO.  Also, if you want to test your ear's talent at "hearing" gravitational waves, there is a fantastic website called Black Hole Hunter which places black hole gravitational wave "sounds" (like the system in the movie above) into simulated data and tests if you can discern the signal.  I've spent many an hour playing with this and even use some of the cell phone ringtones they've made (also available on the Black Hole Hunter site).

*** If you are interested in more gravity games, see my Gravity Games page (link here and under the blog banner)! ***


WANT TO HEAR MORE?

There are some great sites that feature the "sounds" of gravitational waves.  Here are a few of my favorites:

• Black Hole Hunter
• Scott Hughes' (MIT) page of gravitational wave sounds (and a more out of date one)
• black-holes.org page of gravitational wave sounds

Q: What Would a Gravitational Wave Feel Like?

Several people who have found this blog were led here after searching for this question:

What would a gravitational wave feel like?

This is an excellent question so I decided to answer it directly in today's post...


HOW DOES A GRAVITATIONAL WAVE INTERACT WITH MATTER?

First, let us review what a gravitational wave does to matter as it passes by.  Gravitational waves will expand space in one direction and compress it in the perpendicular direction.  This stretching and squishing happen in the plane that forms the cross-section of the wave; this is perpendicular to the direction the wave is traveling.  For a gravitational wave traveling into your computer screen, a circle of stuff will be affected like this:

Image from Wikipedia [gravitational waves]

HOW WOULD A GRAVITATIONAL WAVE FEEL FOR A SOURCE FAR AWAY?

Now let us consider what you are likely to feel here on Earth from what we here at LIGO consider to be "big" gravitational waves.  These waves are produced by some of the most violent, energetic things in the Universe like black holes colliding and stars exploding.  These sources are rare and there are none nearby us, say within a few light-years.  Since the strength of a gravitational wave decreases as the distance from its source increases, by the time these reach us here at Earth they are incredibly small.  A once every ten years gravitational wave will squish and stretch LIGO less than 1000x smaller than the diameter of a proton (< 1x10^-18m).

Therefore, a person will not feel anything from even the strongest gravitational waves we expect to detect with LIGO.  


HOW WOULD A GRAVITATIONAL WAVE FEEL FROM A STRONG, NEARBY SOURCE?

If we were near one of the huge, violent sources LIGO is sensitive to, the gravitational waves would be strong enough to rip us to pieces!  (So it is a very good thing that these sources are very far away!)  This is due to a phenomenon known as "spaghettification".  In a previous post, I described a gravitational wave as simply a change in the gravitational field moving out into the Universe like a ripple in a pond.  The gravitational field is a measure of how much a mass would feel at any given place.  So, if the gravitational wave is a changing gravitational field, then the force of gravity that a mass would feel as the gravitational wave passes should change too.  If the change is so large (due to a very large gravitational wave), then it is possible that your feet will feel a strong enough force, compared to your head, to rip your legs off your body!  And to make matters worse, the sides of your body would be compressed at the same time.

Below is a clip of Neil deGrasse Tyson giving a humorous description of spaghettification.  His description focuses on what would happen to you if you fell into a black hole, but the concept is the same for super-strong gravitational waves:

CONCLUSION

Given where the Earth is in the Universe and how far away sources of strong gravitational waves are, any passing gravitational waves will be so small that we will never be able to feel them.  But if we were close to a strong source of gravitational waves, they could tear us apart!

So it is both a blessing and a curse that the strong sources of gravitational waves are far away:  a blessing because we will never be harmed by them and a curse because they are so small, that we need huge, extraordinarily sensitive detectors like LIGO to detect them.

Q: How Can Gravitational Waves Help Mankind, Part II: Spin-Off Technology

Previously, I have blogged about how gravitational waves can help mankind.  In that post, I noted that observing gravitational waves will allow us to perform unprecedented astronomy, investigate physics in extreme situations that cannot be replicated on Earth, and allow us to further test general relativity.  I also noted that there have been huge advances in technology developed by LIGO scientists and engineers just to make LIGO work.  LIGO has started to document these spin-off technologies on a new webpage: LIGO Technology Development and Migration.

The page describes many methods of how new technology and techniques move from the LIGO research environment to industry or other research applications.  These modes include patents to serendipity (among many others).  I found the descriptions here interesting myself; as a scientist in the thick of it, I am not always aware of how the things I and my colleagues are developing are affecting the world outside of my own little universe.  Also documented on the LIGO Technology Development and Migration page are descriptions of some of the spin-off technology LIGO has produced.

I want to take this opportunity to tell you about just few of the spin-offs that I am most familiar with: 

HOW DO YOU HANG MASSIVE OBJECT FROM A THIN GLASS WIRE?

One of the new additions to Advanced LIGO will be that the mirrors used to measure gravitational waves will be suspended like pendula from glass wires (the pendulum suspension isn't new, it is the glass wire that is new).  It turns out that the metal wires we use like to vibrate right around our most sensitive region in LIGO (about 320 Hz).  This frequency is due to the fact the the wires are made of metal.  If we use wires made from the same material as our mirror is made of (fused silica) then the frequency that they like to vibrate at is outside of our "sweet spot" region (between 100-1000 Hz).  But, our new mirror will be about 40 kg (~88 lb).  It may be surprising, but the glass wires are strong enough to support this weight (which is also the weight of a small child).

Silica fibers bonded to "ears" that are attached to a glass mass

But how do you connect these delicate glass wires (they may be strong, but they are brittle)?  That is the work of Sheila Rowan, James Hough, and Eoin John Eliffe from the University of Glasgow and Stanford University.  They has developed and patented a new technology that not only bonds the wire to the mass, but also minimized contamination of the collected gravitational wave data from glass' thermal noise.  This technology has already been transferred to several optical industry vendors!

Read more about this here!

HOW CAN YOU KEEP THE SHAPE OF A LENS FROM CHANGING WHEN A LASER PASSES THROUGH IT?

In LIGO, it is very important to keep the shape of our mirrors controlled so that we can keep the laser light bounding back and forth in an arm many times before it recombines with the light from the other arms (this makes the light think that our arms are 70-100 times larger than they are and that gives a gravitational wave more time to affect the light in the arm).  Even though our mirrors are nearly perfectly reflecting, a small amount of the light gets absorbed by the mirror and this causes it to heat up.  When the mirror heats up, it warps its shape and this distortion can make it VERY difficult to keep the light focused between two mirrors that are 4 km (~2.5 mi) apart.  What to do?

The solution to this is the heat the mirror in a controlled way so that you can cause your own distortions that compensate for the warping that the laser is causing.  LIGO has spent much effort perfecting techniques light this (I even have a friend who did his Ph.D. research on this).  This also has wider application in industrial and military environments since higher power lasers are being introduced all the time (such applications include welding and material cutting).  The ability to control the shape of the optics that control and direct a laser beam is becoming increasingly important.

Read more about this here!


HOW CAN YOU USE LIGO DATA ANALYSIS METHODS TO ANALYZE OTHER KINDS OF DATA?


This one is dear to my heart since I specialize in LIGO data analysis!  It is not just physical technology that can be reapplied for other purposes; techniques and software can as well.  Of the many different analysis methods that LIGO executes, the one used to search for continuous (long duration with consistent frequency) gravitational waves produced by things light neutron stars with a "mountain" on it (I put "mountain" in quotation marks because a neutron star is so perfectly spherical, that a deformation of less than an inch is considered a "mountain"!).  This is the analysis that is performed by Einstein@Home (which I blogged about previously here).  

Arecibo Radio Telescope (image from Wikipedia)

The data analysis challenge for these gravitational waves turns out to be similar to the challenge faced by astronomers looking for pulsars that emit either radio waves or gamma rays.  This data is collected by the Arecibo radio telescope in Puerto Rico and the Fermi gamma-ray satellite, respectively.  Using Einstein@Home, the continuous gravitational wave data analysis techniques are applied to data from these two detectors to great effect!  The number of known gamma ray pulsars (that don't produce radio waves) has been increased by a third thanks to discoveries made using the same data analysis Einstein@Home uses.  Radio pulsars are also being discovered on a regular basis with Einstein@Home; since the beginning of 2012, 22 new radio pulsars have been discovered!

Read more about this here!

Q: What is a Gravitational Wave?

Many times, when we scientists answer this question, we say "ripples on space-time".  It wasn't until I was in grad school that I really started to understand was "space-time" was.  Before that, anytime someone said the word I just nodded with an expression of recognition so I wouldn't look dumb.

So, when I talk to visitors to LIGO, I like to talk about gravitational waves (or, more specifically, space-time) in a different way.  First, let's go back to gravity as Newton described it...

NEWTON'S GRAVITY

There is a story about how Isaac Newton came upon the realization of gravity, often referred to as "Newton's Apple".  One day, Newton was sitting under a tree in an apple orchard.  This was one of those days when the Moon is visible in the afternoon sky.  He then saw an apple fall to the ground (some versions of the story say the apple fell on his head but I think that is too convenient).  It was then that he realized that the force that drew the apple to the ground without touching it was the same force that kept the Moon in orbit around the Earth.  This kind of force is called action at a distance.  The way two masses communicate the gravitational force between them is with a field (just like the magnetic or electric field).  Every mass (including you and me) fills up the Universe with a gravitational field that gets weaker with distance.  When objects move, the entire gravitational field of the object moves with it and every object in the Universe feels a change in the gravitational force because of this instantaneously.

EINSTEIN'S GRAVITY

In Einstein's relativity, nothing can travel faster than the speed of light, including information about where mass is in the Universe.  That means that there must be a change in the gravitational field that moves out into the Universe at a finite speed instead of everything "feeling" the change instantly.  A gravitational wave is really that change in the gravitational field propagating out into the Universe like a ripple on a pond.

SPACE-TIME

So, how is this moving change in gravitational field that is a gravitational wave related to space-time?  First, space-time measures the curvature of the Universe.  It is usually visualized as an elastic grid, but this is a large simplification since space-time would be better represented by an animated 3-dimensional grid - but that is beside the point for now.  When there is no mass, space-time is perfectly flat:

When there is mass present, space-time will be curved:

Consider another much smaller mass approaching this one: it will be deflected by the curvature of space-time.  This is gravitational attraction.

Ultimately, the strength of the gravitational field at any given place corresponds the the steepness of the curvature of space-time there.  In the flat space-time, there is no curvature and no gravitational field.

RIPPLES ON SPACE-TIME = RIPPLES OF GRAVITATIONAL FIELD

Now, we can go back to the phrase "ripples in space-time".  Now that we understand more about what space-time is, how it is represented, and how it affects mass moving through it we have a bigger picture of what gravitational waves are.  Any time a mass moves (accelerates - there are some subtleties here), that is going to create a change in the gravitational field (the curvature of space-time) and this change will ripple out into the Universe.

Below is an animation by the Jodrell Bank Center for Astrophysics of a pulsar-neutron star system merging into a black hole.  The green grid represents the surrounding space-time and the gravitational waves on it are evident:

So, what do you think?  Does this make more sense?  Let me know!


ADDENDUM added 15 July 2012:

The elastic 2-dimensional grid, while suitable for discussion here, has several important features that are imperfect for use as an analogy for spacetime.  The first is that an elastic sheet will create a curvature that is related to the object's mass and its size.  However, the size of a mass has nothing to do with the curvature of spacetime.  Another is that a passing gravitational wave will affect a mass but the mass will not continue to 'bounce' on spacetime thus creating more ripples on spacetime (think of a mass bouncing on a trampoline).  There are plenty of other features that make this 2-dimensional approximation imperfect, but these are two of the most important for our purposes.

A better visualization is found in the American Museum of Natural History's short documentary called Gravity: Making Waves (which can be seen in its entirety on my Viewing Fun! page).  This is grid-like scaffolding filling 3-dimensional space in which there is a depression caused by mass.  While it still isn't a perfect representation of spacetime, it is much better than the trampoline approximation above (but also overly complicated for this discussion).  Below is the relevant clip from Gravity: Making Waves (~ 2 MB):