LHChamber Music, CERN scientists perform musical compositions created using data sonification of LHC experimental results (Video: CERN)
Yaron Herman plays piano jazz that is utterly unique. He learned to play based on a method using math and philosophy.
Bijan Chemirani, French-born percussionist, was initiated into the art of Iranian percussion by his father, Djamchid Chemirani, at an early age and has acquired enormous experience in adapting his playing style to other genres of music.
Here they perform together for the first time at TEDxCERN.
Published on Oct 19, 2012 The Kitchener-Waterloo Symphony and the Institute for Quantum Computing teamed up on Sept. 29, 2012, to present an innovative musical experiment called "Quantum: Music at the Frontier of Science." The concert served as the the grand finale of the grand opening celebrations of the Mike & Ophelia Lazaridis Quantum-Nano Centre at the University of Waterloo. Through narration, an eclectic musical programme, live narration and "sound experiments," the concert explored the surprisingly parallel paths followed by quantum science and orchestral music over the past century. The concert was created over the period of a year through meetings and brainstorming sessions between KW Symphony Music Director Edwin Outwater and researchers from the Institute for Quantum Computing.
What does the universe look like at high energies? Thanks to the FermiLarge Area Telescope (LAT), we can extend our sense of sight to “see”the universe in gamma rays. But humans not only have a sense of sight,we also have a sense of sound. If we could listen to the high-energy universe, what would we hear? What does the universe sound like?The Sound of a Fermi Gamma-ray BurstPutting a Fermi Gamma-ray burst to music. Made by Sylvia Zhu
The universe is expected to be permeated by a stochastic background of gravitational radiation of astrophysical and cosmological origin. This background is capable of exciting oscillations in solar-like stars. Here we show that solar-like oscillators can be employed as giant hydrodynamical detectors for such a background in the muHz to mHz frequency range, which has remained essentially unexplored until today. We demonstrate this approach by using high-precision radial velocity data for the Sun to constrain the normalized energy density of the stochastic gravitational-wave background around 0.11 mHz. These results open up the possibility for asteroseismic missions like CoRoT and Kepler to probe fundamental physics. See: An upper bound from helioseismology on the stochastic background of gravitational waves
|The heart-shaped vibrations for the star KIC12253350.|
The search for distant planets starts with the vibrations of their stars, and in those vibrations lies a kind of music.
This page has links to sound files that are "sonification of light curves" of Kepler stars. The light curves contain certain frequencies of brightness variation that are akin to sound waves, but the frequencies are not audible to the human ear. In the sonification process, those inaudible frequencies are analyzed by a mathematical technique called fourier analysis and then scaled to frequencies that the human ear can hear. See: Kepler Star Sounds
Gravitational waves have a polarization pattern that causes objects to expand in one direction, while contracting in the perpendicular direction. That is, they have spin two. This is because gravity waves are fluctuations in the tensorial metric of space-time.
|WMAP image of the Cosmic Microwave Background Radiation|
In this example I’m going to map speed to the pitch of the note, length/postion to the duration of the note and number of turns/legs/puffs to the loudness of the note.See: How to make sound out of anything.
In the late 1950s, Weber became intrigued by the relationship between gravitational theory and laboratory experiments. His book, General Relativity and Gravitational Radiation, was published in 1961, and his paper describing how to build a gravitational wave detector first appeared in 1969. Weber's first detector consisted of a freely suspended aluminium cylinder weighing a few tonnes. In the late 1960s and early 1970s, Weber announced that he had recorded simultaneous oscillations in detectors 1000 km apart, waves he believed originated from an astrophysical event. Many physicists were sceptical about the results, but these early experiments initiated research into gravitational waves that is still ongoing. Current gravitational wave experiments, such as the Laser Interferometer Gravitational Wave Observatory (LIGO) and Laser Interferometer Space Antenna (LISA), are descendants of Weber's original work. See:Joseph Weber 1919 - 2000
A NASA spacecraft has recorded eerie-sounding radio emissions coming from our own planet. These beautiful "songs of Earth" could, ironically, be responsible for the proliferation of deadly electrons in the Van Allen Belts.
EARTH: If you're squeamish, you may not want to listen to the strange whistle of ultra-cold liquid helium-3 that changes volume relative to the North Pole and Earth's rotation.
Dr. Subodh Patil is a cosmologist at CERN and is the inspiration partner for Bill Fontana, 2012-2013 Prix Ars Electronica Collide@CERN winner, during his residency at CERN. Bill began his 3-month residency at CERN at an event called "The Universe of Sound" on July 4th, 2013, in the CERN Globe of Science & Innovation. In this excerpt from this event, Dr. Patil explains the parallels between physics, cosmology, sound, and music.
Watch the video of Bill Fontana's talk here: http://www.youtube.com/watch?v=6Zjy8v...
Bernie Krause has been recording wild soundscapes -- the wind in the trees, the chirping of birds, the subtle sounds of insect larvae -- for 45 years. In that time, he has seen many environments radically altered by humans, sometimes even by practices thought to be environmentally safe. A surprising look at what we can learn through nature's symphonies, from the grunting of a sea anemone to the sad calls of a beaver in mourning.
Bill Fontana is a renowned American sound sculptor who studied with John Cage and is the 2012-2013 Prix Ars Electronica Collide@CERN winner. He began his 2-month residency at CERN with an event entitled "The Universe of Sound" on 4 July 2013, in the CERN Globe of Science & Innovation, from which this excerpt was taken. Guided by his mantra, "All sound is music," Fontana gives samples of his previous work as well as some hints of what is to come during his residency.
Watch the video of Dr. Subodh Patil, CERN cosmologist and inspiration partner for Bill Fontana: http://www.youtube.com/watch?v=0mCkKD...
Find out more via http://arts.web.cern.ch/collide/digit...
|Different oscillation modes penetrate to different depths inside a star.|
Asteroseismology (from Greek ἀστήρ, astēr, "star"; σεισμός, seismos, "earthquake"; and -λογία, -logia) also known as stellar seismology is the science that studies the internal structure of pulsating stars by the interpretation of their frequency spectra. Different oscillation modes penetrate to different depths inside the star. These oscillations provide information about the otherwise unobservable interiors of stars in a manner similar to how seismologists study the interior of Earth and other solid planets through the use of earthquake oscillations.
Asteroseismology provides the tool to find the internal structure of stars. The pulsation frequencies give the information about the density profile of the region where the waves originate and travel. The spectrum gives the information about its chemical constituents. Both can be used to give information about the internal structure. Astroseismology effectively turns tiny variations in the star's light into sounds.
OscillationsThe oscillations studied by asteroseismologists are driven by thermal energy converted into kinetic energy of pulsation. This process is similar to what goes on with any heat engine, in which heat is absorbed in the high temperature phase of oscillation and emitted when the temperature is low. The main mechanism for stars is the net conversion of radiation energy into pulsational energy in the surface layers of some classes of stars. The resulting oscillations are usually studied under the assumption that they are small, and that the star is isolated and spherically symmetric. In binary star systems, stellar tides can also have a significant influence on the star's oscillations. One application of asteroseismology is neutron stars, whose inner structure cannot be directly observed, but may be possible to infer through studies of neutron-star oscillations.
Waves in sun-like stars can be divided into three different types;
Within a sun-like star, such as Alpha Centauri, the p-modes are the most prominent as the g-modes are essentially confined to the core by the convection zone. However, g-modes have been observed in white dwarf stars.
- p-mode: Acoustic or pressure (p) modes, driven by internal pressure fluctuations within a star; their dynamics being determined by the local speed of sound.
- g-mode: Gravity (g) modes, driven by buoyancy,
- f-mode: Surface gravity (f) modes, akin to ocean waves along the stellar surface.
Helioseismology, also known as Solar seismology, is the closely related field of study focused on the Sun. Oscillations in the Sun are excited by convection in its outer layers, and observing solar-like oscillations in other stars is a new and expanding area of asteroseismology.
A number of active spacecraft have asteroseismology studies as a significant part of their mission.
- MOST – A Canadian satellite launched in 2003. The first spacecraft dedicated to asteroseismology.
- COROT – A French led ESA planet-finder and asteroseismology satellite launched in 2006
- WIRE – A NASA satellite launched in 1999. A failed infrared telescope now used for asteroseismology.
- SOHO – A joint ESA / NASA spacecraft launched in 1995 to study the Sun.
- Kepler – A NASA planet-finder spacecraft launched in 2009 that is currently making asteroseismology studies of over a thousand stars in its field, including the now well-studied subgiant KIC 11026764.
Red giants and asteroseismology
Red giants are a later stage of evolution of sun-like stars after the core hydrogen fusion ceases as the fuel runs out. The outer layers of the star expand by about 200 times and the core contracts. However, there are two different stages, first one when there is fusion of hydrogen in a layer outside the core, but none of helium in the core, and then a later stage when the core is hot enough to fuse helium. Previously, these two stages could not be directly distinguished by observing the star's spectrum, and the details of these stages were incompletely understood. With the Kepler mission, asteroseismology of hundreds of relatively nearby red giants enabled these two types of red giant to be distinguished. The hydrogen-shell-burning stars have gravity-mode period spacing mostly ~50 seconds and those that are also burning helium have period spacing ~100 to 300 seconds. It was assumed that, by conservation of angular momentum, the expansion of the outer layers and contraction of the core as the red giant forms would result in the core rotating faster and the outer layers slower. Asteroseismology showed this to indeed be the case with the core rotating at least ten times as fast as the surface. Further asteroseismological observations could help fill in some of the remaining unknown details of star evolution.
- Ghosh, Pallab (23 October 2008). "Team records 'music' from stars". BBC News. Retrieved 2008-10-24.
- Guenther, David. "Solar and Stellar Seismology". Saint Mary's University. Retrieved 2008-10-24.
- Palmer, Jason (20 February 2013). "Exoplanet Kepler 37b is tiniest yet - smaller than Mercury". BBC News. Retrieved 2013-02-20.
- Unno W, Osaki Y, Ando H, Saio H, Shibahashi H (1989). Nonradial Oscillations of Stars (2nd ed.). Tokyo, Japan: University of Tokyo Press.
- Christensen-Dalsgaard, Jørgen (June 2003). "Chapter 1" (PDF). Lecture Notes on Stellar Oscillations (5th ed.). p. 3. Retrieved 2008-10-24.
- Christensen-Dalsgaard, Jørgen (June 2003). "Chapter 2" (PDF). Lecture Notes on Stellar Oscillations (5th ed.). p. 23. Retrieved 2008-10-24.
- Metcalfe, T. S.; et al (2010-10-25). "A Precise Asteroseismic Age and Radius for the Evolved Sun-like Star KIC 11026764". The Astrophysical Journal 723 (2): 1583. arXiv:1010.4329. Bibcode:2010ApJ...723.1583M. doi:10.1088/0004-637X/723/2/1583.
- "Graphics for 2010 Oct 26 webcast – Images from the Kepler Asteroseismology Science Consortium (KASC) webcast of 2010 Oct 26". NASA. 2010-10-26. Retrieved 3 November 2010.
- Bedding TR, Mosser B, Huber D, Montalbaan J, et al. (Mar 2011). "Gravity modes as a way to distinguish between hydrogen- and helium-burning red giant stars". Nature 471 (7340): 608–611. arXiv:1103.5805. Bibcode:2011Natur.471..608B. doi:10.1038/nature09935. PMID 21455175.
- Beck, Paul G.; Montalban, Josefina; Kallinger, Thomas; De Ridder, Joris; et al. (Jan 2012). "Fast core rotation in red-giant stars revealed by gravity-dominated mixed modes". Nature 481 (7379): 55–57. arXiv:1112.2825. Bibcode:2012Natur.481...55B. doi:10.1038/nature10612. PMID 22158105.
If our experience of time and space share similar neural correlates, it begets a fundamental question: are space and time truly distinct in the mind, or are they the product of a generalized neurocognitive system that allows us to understand the world? See:Decoding Space and Time in the Brain
B-modes retain their special nature as manifest in the fact that they can possess a handedness that distinguishes left from right. For example here are two polarization fields with the same structure but in the E-mode on the left and the B-mode on the right:See: Anomalous Alignments in the Cosmic Microwave Background
If you sprinkle fine sand uniformly over a drumhead and then make it vibrate, the grains of sand will collect in characteristic spots and figures, called Chladni patterns. These patterns reveal much information about the size and the shape of the drum and the elasticity of its membrane. In particular, the distribution of spots depends not only on the way the drum vibrated initially but also on the global shape of the drum, because the waves will be reflected differently according to whether the edge of the drumhead is a circle, an ellipse, a square, or some other shape.The Shape of Space after WMAP data
In cosmology, the early Universe was crossed by real acoustic waves generated soon after Big Bang. Such vibrations left their imprints 300 000 years later as tiny density fluctuations in the primordial plasma. Hot and cold spots in the present-day 2.7 K CMB radiation reveal those density fluctuations. Thus the CMB temperature fluctuations look like Chaldni patterns resulting from a complicated three-dimensional drumhead that.
Spectra are complex because each spectrum holds a wide variety of information. For instance, there are many different mechanisms by which an object, like a star, can produce light - or using the technical term for light, electromagnetic radiation. Each of these mechanisms has a characteristic spectrum. Let's look at a spectrum and examine each part of it. Introduction to Spectroscopy
The crystalline state is the simplest known example of a quantum , a stable state of matter whose generic low-energy properties are determined by a higher organizing principle and nothing else. Robert Laughlin
This image depicts the interaction of nine plane waves—expanding sets of ripples, like the waves you would see if you simultaneously dropped nine stones into a still pond. The pattern is called a quasicrystal because it has an ordered structure, but the structure never repeats exactly. The waves produced by dropping four or more stones into a pond always form a quasicrystal.See: 59. Medieval Mosque Shows Amazing Math Discovery
Because of the wavelike properties of matter at subatomic scales, this pattern could also be seen in the waveform that describes the location of an electron. Harvard physicist Eric Heller created this computer rendering and added color to make the pattern’s structure easier to see. See: What Is This? A Psychedelic Place Mat?
To “hear” the data we can map physical properties (The Data) to audible properties (The Sound) in pretty much any way we choose. For a physicist, an obvious way to do this might be to map speed to pitch. I think this is obvious for a physicist because both of these things are measured “per second” (pitch or frequency is measured in Hertz, which means vibrations per second). But we don’t have to do the obvious, we can map any physical property to any audible property. In this example I’m going to map speed to the pitch of the note, length/position to the duration of the note and number of turns/legs/puffs to the loudness of the note. Now I have to choose starting positions and ranges. When I do this I have to consider that:How to make sound out of anything.
We know that colour is a psychophysical experience of an observer which changes from observer to observer and is therefore impossible to replicate absolutely. In order to quantify colour in meaningful terms we must be able to measure or represent the three attributes that together give a model of colour perception. i.e. light, object and the eye. All these attributes have been standardised by the CIE or Commission Internationale de l'Eclairage. The colours of the clothes we wear and the textiles we use in our homes must be monitored to ensure that they are correct and consistent. Colour measurement is therefore essential to put numbers to colour in order to remove physical samples and the interpretation of results.See:Colour measuring equipment
In the arts and of painting, graphic design, and photography, color theory is a body of practical guidance to color mixing and the visual impact of specific color combinations. Although color theory principles first appear in the writings of Alberti (c.1435) and the notebooks of Leonardo da Vinci (c.1490), a tradition of "colory theory" begins in the 18th century, initially within a partisan controversy around Isaac Newton's theory of color (Opticks, 1704) and the nature of so-called primary colors. From there it developed as an independent artistic tradition with only sporadic or superficial reference to colorimetry and vision science.See: Color Theory
CIE L*a*b* (CIELAB) is the most complete color model used conventionally to describe all the colors visible to the human eye. It was developed for this specific purpose by the International Commission on Illumination (Commission Internationale d'Eclairage, hence its CIE initialism). The * after L, a and b are part of the full name, since they represent L*, a* and b*, derived from L, a and b. CIELAB is an Adams Chromatic Value Space. The three parameters in the model represent the lightness of the color (L*, L*=0 yields black and L*=100 indicates white), its position between magenta and green (a*, negative values indicate green while positive values indicate magenta) and its position between yellow and blue (b*, negative values indicate blue and positive values indicate yellow). The Lab color model has been created to serve as a device independent model to be used as a reference. Therefore it is crucial to realize that the visual representations of the full gamut of colors in this model are never accurate. They are there just to help in understanding the concept, but they are inherently inaccurate. Since the Lab model is a three dimensional model, it can only be represented properly in a three dimensional space.See: CIE 1976 L*, a*, b* Color Space (CIELAB)So in a sense we have developed "a method" by which application of color in this case would be used. Is it highly subjective in one's own case without some kind of metered measure and one would have to consider, by which consensus such a model would be applied(production of specific colours chemically induced for instance) to have a desired effect.
Space, we all know what it looks like. We've been surrounded by images of space our whole lives, from the speculative images of science fiction to the inspirational visions of artists to the increasingly beautiful pictures made possible by complex technologies. But whilst we have an overwhelmingly vivid visual understanding of space, we have no sense of what space sounds like.Honor Harger: A history of the universe in soundSo while one might consider colorimetric space here one might convert such a space to what every point in that space represents in terms of a color? So you devise parameters.
Gravity is usually measured in units of acceleration. In the SI system of units, the standard unit of acceleration is 1 metre per second squared (abbreviated as m/s2). Other units include the gal (sometimes known as a galileo, in either case with symbol Gal), which equals 1 centimetre per second squared, and the g (gn), equal to 9.80665 m/s2. The value of the gn approximately equals the acceleration due to gravity at the Earth's surface (although the actual acceleration g varies fractionally from place to place). See: Gravimetry
It’s just a matter of lasers and mirrors, but using Michelson’s 19th-century techniques and LIGO’s 21st-century technology, scientists will soon “hear” a phenomenon first predicted by Einstein’s famous 20th-century theory.See: LIGO 02
Cornell University researchers already have been able to detect the mass of a single cell using submicroscopic devices. Now they're zeroing in on viruses. And the scale of their work is becoming so indescribably small that they have moved beyond the prefixes "nano" "pico" and "femto" to "atto." And just in sight is "zepto."
Members of the Cornell research group headed by engineering professor Harold Craighead report they have used tiny oscillating cantilevers to detect masses as small as 6 attograms by noting the change an added mass produces in the frequency of vibration.
Their submicroscopic devices, whose size is measured in nanometers (the width of three silicon atoms), are called nanoelectromechanical systems, or NEMS. But the masses they measure are now down to attograms. The mass of a small virus, for example, is about 10 attograms. An attogram is one-thousandth of a femtogram, which is one-thousandth of a picogram, which is one-thousandth of a nanogram, which is a billionth of a gram.‘Nano’ Becomes ‘Atto’ and Will Soon Be ‘Zepto’ for Cornell - New Technology
|Frequency range||Name||Usually associated with:|
|> 40 Hz||Gamma waves||Higher mental activity, including perception, problem solving, fear, and consciousness|
|13–39 Hz||Beta waves||Active, busy or anxious thinking and active concentration, arousal, cognition, and or paranoia|
|7–13 Hz||Alpha waves||Relaxation (while awake), pre-sleep and pre-wake drowsiness, REM sleep, Dreams|
|8–12 Hz||Mu waves||Sensorimotor rhythm Mu_rhythm, Sensorimotor_rhythm|
|4–7 Hz||Theta waves||deep meditation/relaxation, NREM sleep|
|< 4 Hz||Delta waves||Deep dreamless sleep, loss of body awareness|