- published: 27 Nov 2016
- views: 11634
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Hello and welcome to What Da Math!
In this video, we will use the new effects from Universe Sandbox 2 to create an accretion disk around a black hole.
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Computational Plasma Astrophysics: July 25, 2016
Prospects in Theoretical Physics is an intensive two-week summer program typically designed for graduate students and postdoctoral scholars considering a career in theoretical physics (for 2014 only the program was one week in length). First held by the School of Natural Sciences at the Institute for Advanced Study in the summer of 2002, the PiTP program is designed to provide lectures and informal sessions on the latest advances and open questions in various areas of theoretical physics.
One of the goals of the program is to help the physics community train the next generation of scholars in theoretical physics. A special effort is made to reach out to women and minorities, as well as to graduate students in small universities who typically do not have the same opportunities and access to leaders in the field as graduate students in large research institutions.
Prospects in Theoretical Physics builds on the strong relationship of the research groups at the Institute and Princeton University, and many faculty members from the physics departments at both institutions are actively involved in the program together with scientists from neighboring institutions.
More videos on http://video.ias.edu
- published: 25 Jul 2016
- views: 2340
What is ACCRETION DISK? What does ACCRETION DISK mean? ACCRETION DISK meaning - ACCRETION DISK definition - ACCRETION DISK explanation.
An accretion disk is a structure (often a circumstellar disk) formed by diffused material in orbital motion around a massive central body. The central body is typically a star. Gravity causes material in the disk to spiral inward towards the central body. Gravitational and frictional forces compress and raise the temperature of the material causing the emission of electromagnetic radiation. The frequency range of that radiation depends on the central object's mass. Accretion disks of young stars and protostars radiate in the infrared; those around neutron stars and black holes in the X-ray part of the spectrum. The study of oscillation modes in accretion disks is referred to as diskoseismology.
Accretion disks are a ubiquitous phenomenon in astrophysics; active galactic nuclei, protoplanetary disks, and gamma ray bursts all involve accretion disks. These disks very often give rise to astrophysical jets coming from the vicinity of the central object. Jets are an efficient way for the star-disk system to shed angular momentum without losing too much mass.
The most spectacular accretion disks found in nature are those of active galactic nuclei and of quasars, which are believed to be massive black holes at the center of galaxies. As matter enters the accretion disc, it follows a trajectory called a tendex line, which describes an inward spiral. This is because particles rub and bounce against each other in a turbulent flow, causing frictional heating which radiates energy away, reducing the particles' angular momentum, allowing the particle to drift inwards, driving the inward spiral. The loss of angular momentum manifests as a reduction in velocity; at a slower velocity, the particle wants to adopt a lower orbit. As the particle falls to this lower orbit, a portion of its gravitational potential energy is converted to increased velocity and the particle gains speed. Thus, the particle has lost energy even though it is now travelling faster than before; however, it has lost angular momentum. As a particle orbits closer and closer, its velocity increases, as velocity increases frictional heating increases as more and more of the particle's potential energy (relative to the black hole) is radiated away; the accretion disk of a black hole is hot enough to emit X-rays just outside the event horizon. The large luminosity of quasars is believed to be a result of gas being accreted by supermassive black holes (Lynden-Bell, 1969). Elliptical accretion disks formed at tidal disruption of stars can be typical in galactic nuclei and quasars (Gurzadyan and Ozernoy, 1979). Accretion process can convert about 10 percent to over 40 percent of the mass of an object into energy as compared to around 0.7 percent for nuclear fusion processes.
In close binary systems the more massive primary component evolves faster and has already become a white dwarf, a neutron star, or a black hole, when the less massive companion reaches the giant state and exceeds its Roche lobe. A gas flow then develops from the companion star to the primary. Angular momentum conservation prevents a straight flow from one star to the other and an accretion disk forms instead.
Accretion disks surrounding T Tauri stars or Herbig stars are called protoplanetary disks because they are thought to be the progenitors of planetary systems. The accreted gas in this case comes from the molecular cloud out of which the star has formed rather than a companion star.
- published: 01 Oct 2016
- views: 1569
Interstellar is the first Hollywood movie to attempt depicting a black hole as it would actually be seen by somebody nearby.
Get more Science at The Speaker Science: http://thespeaker.co/science/
For this, our team at Double Negative Visual Effects, in collaboration with physicist Kip Thorne, developed a code called Double Negative Gravitational Renderer (DNGR) to solve the equations for ray-bundle (light-beam) propagation through the curved spacetime of a spinning (Kerr) black hole, and to render IMAX-quality, rapidly changing images.
Our ray-bundle techniques were crucial for achieving IMAX-quality smoothness without flickering; and they differ from physicists' image-generation techniques (which generally rely on individual light rays rather than ray bundles), and also differ from techniques previously used in the film industry's CGI community.
This paper has four purposes: (i) to describe DNGR for physicists and CGI practitioners, who may find interesting and useful some of our unconventional techniques. (ii)
To present the equations we use, when the camera is in arbitrary motion at an arbitrary location near a Kerr black hole, for mapping light sources to camera images via elliptical ray bundles. (iii)
To describe new insights, from DNGR, into gravitational lensing when the camera is near the spinning black hole, rather than far away as in almost all prior studies; we focus on the shapes, sizes and influence of caustics and critical curves, the creation and annihilation of stellar images, the pattern of multiple images, and the influence of almost-trapped light rays, and we find similar results to the more familiar case of a camera far from the hole. (iv)
To describe how the images of the black hole Gargantua and its accretion disk, in the movie Interstellar, were generated with DNGR—including, especially, the influences of (a) colour changes due to doppler and gravitational frequency shifts, (b) intensity changes due to the frequency shifts, (c) simulated camera lens flare, and (d) decisions that the film makers made about these influences and about the Gargantua's spin, with the goal of producing images understandable for a mass audience. There are no new astrophysical insights in this accretion-disk section of the paper, but disk novices may find it pedagogically interesting, and movie buffs may find its discussions of Interstellar interesting.
Gravitational lensing by spinning black holes in astrophysics, and in the movie Interstellar.
Oliver James et al (2015), Classical and Quantum Gravity http://dx.doi.org/10.1088/0264-9381/3...
- published: 28 Oct 2015
- views: 26305
On June 15, NASA's Swift caught the onset of a rare X-ray outburst from a stellar-mass black hole in the binary system V404 Cygni. Astronomers around the world are watching the event. In this system, a stream of gas from a star much like the sun flows toward a 10 solar mass black hole. Instead of spiraling toward the black hole, the gas accumulates in an accretion disk around it. Every couple of decades, the disk switches into a state that sends the gas rushing inward, starting a new outburst.
Download this video in HD formats from NASA Goddard's Scientific Visualization Studio
http://svs.gsfc.nasa.gov/cgi-bin/details.cgi?aid=11110
- published: 30 Jun 2015
- views: 278949
Welcome to another experiment in Universe Sandbox 2 Let's play series.
Today we'll be testing a user made suggestion asking if we can form an accretion disk in Universe Sandbox 2, let's find out!
Universe Sandbox 2 is a space sandbox that is still a work in progress, and is an awesome game and educational tool. But, keep in mind the physics and results depicted in this game are to be taken with a grain a salt, the game tries to, but does not always accurately reproduce the expectations of our current knowledge of physics, the game is still an early access alpha and is still being worked on!
A lot of the ideas in this series are suggestions by viewers and aren't always intended to be "educational," so take the results of this test with a grain of salt!
Buy and Support Universe Sandbox 2 on Steam
http://store.steampowered.com/app/230290/
You read descriptions! ツ
- published: 10 Apr 2018
- views: 478
The disk is based on a non-relativistic Smoothed-Particle-Hydrodynamics (SPH) simulation.
The apparent distortion of the disk is due to the bending of light within the Schwarzschild spacetime. Besides the primary image of the disk, there are also higher order images (lower ring and upper thin ring) visible. The lower ring shows the rear bottom side of the disk. The color encodes the apparent temperature where blue is hot and red is cold. The left part of the disk approaches the observer and, thus, appears hotter due to the Doppler effect. You also see some bright spots which smear out already after one revolution around the black hole.
- published: 27 Oct 2014
- views: 15521
An "accretion disk" is a structure formed by diffused material in orbital motion around a massive central body. The central body is typically a star. Gravity causes material in the disc to spiral inward towards the central body. Gravitational and frictional forces compress and raise the temperature of the material causing the emission of electromagnetic radiation. The frequency range of that radiation depends on the central object's mass. Accretion discs of young stars and protostars radiate in the infrared; those around neutron stars and black holes in the X-ray part of the spectrum. The study of oscillation modes in accretion discs is referred to as "diskoseismology".
Accretion discs are a ubiquitous phenomenon in astrophysics; active galactic nuclei, protoplanetary discs, and gamma ray bursts all involve accretion discs. These discs very often give rise to astrophysical jets coming from the vicinity of the central object. Jets are an efficient way for the star-disc system to shed angular momentum without losing too much mass.
The most spectacular accretion discs found in nature are those of active galactic nuclei and of quasars, which are believed to be massive black holes at the center of galaxies. As matter follows the tendex line into a black hole, the intense gravitational gradient gives rise to intense frictional heating; the accretion disc of a black hole is hot enough to emit X-rays just outside of the event horizon. The large luminosity of quasars is believed to be a result of gas being accreted by supermassive black holes . Elliptical accretion discs formed at tidal disruption of stars can be typical in galactic nuclei and quasars . Accretion process can convert about 10 percent to over 40 percent of the mass of an object into energy as compared to around 0.7 percent for nuclear fusion processes.
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Disclaimer: This video is for your information only. The author or publisher does not guarantee the accuracy of the content presented in this video. USE AT YOUR OWN RISK.
Background Music:
"The Place Inside" by Silent Partner (royalty-free) from YouTube Audio Library.
This video uses material/images from https://en.wikipedia.org/wiki/Accretion+disc, which is released under Creative Commons Attribution-Share-Alike License 3.0 http://creativecommons.org/licenses/by-sa/3.0/ . This video is licensed under Creative Commons Attribution-Share-Alike License 3.0 http://creativecommons.org/licenses/by-sa/3.0/ . To reuse/adapt the content in your own work, you must comply with the license terms.
Wiz Science™ is "the" learning channel for children and all ages.
SUBSCRIBE TODAY
Disclaimer: This video is for your information only. The author or publisher does not guarantee the accuracy of the content presented in this video. USE AT YOUR OWN RISK.
Background Music:
"The Place Inside" by Silent Partner (royalty-free) from YouTube Audio Library.
This video uses material/images from https://en.wikipedia.org/wiki/Accretion+disc, which is released under Creative Commons Attribution-Share-Alike License 3.0 http://creativecommons.org/licenses/by-sa/3.0/ . This video is licensed under Creative Commons Attribution-Share-Alike License 3.0 http://creativecommons.org/licenses/by-sa/3.0/ . To reuse/adapt the content in your own work, you must comply with the license terms.
- published: 10 Sep 2015
- views: 778
Full Playlist of Starbound Soundtrack:
https://www.youtube.com/playlist?list=PL7DXTXnlwEuN4eTTyMIOZJfoZN4IQgx8z&feature;=mh_lolz
- published: 08 Dec 2013
- views: 39347
Using two of the world's largest telescopes, an international team of astronomers have found evidence of a collision between galaxies driving intense activity in a highly luminous quasar. The scientists, led by Montserrat Villar Martin of the Instituto de Astrofisica de Andalucía-CSIC in Spain, used the Very Large Telescope (VLT) in Chile and the Gran Telescopio Canarias (GTC) on La Palma in the Canary Islands, to study activity from the quasar SDSS J0123+00. They publish their work in a paper in the journal Monthly Notices of the Royal Astronomical Society.
Several types of galaxies, known as active galaxies, emit enormous amounts of energy from their central region or nucleus, with the most luminous objects known as quasars. Most scientists argue that quasars contain a central black hole, with a mass of at least several million Suns.
The intense gravitational field created by the black hole drags material inexorably inwards. Before falling in, this material settles in an accretion disk where it becomes very hot and emits large amounts of energy responsible for most of the brightness of the quasar. Around the central quasar 'engine' is a torus (thick ring) opaque to the visible light emitted by the accretion disk. From a terrestrial perspective, if the torus is face-on then the radiation from the disk can be seen and the system is designated type 1, whereas in type 2 quasars the torus is edge-on and the radiation is concealed.
source: http://www.iaa.es/~rosa/AYA2010/AYA2010/Novedades/Entradas/2010/6/23_Galaxy_encounter_fire_up_quasar.html
- published: 25 Jun 2010
- views: 8073
In this video, the camera rotates around a spinning (Kerr) black hole that is surrounded by an accretion disk (a vortex of matter attracted by the black hole that orbits it and eventually falls in).
The accreting matter emits synchrotron radiation at various frequencies; in the video, we see radiation emitted at 230 GHz.
If you have any questions, feel free to ask!
Credits:
T. Bronzwaer, J. Davelaar, Z. Younsi 2017.
The video was made using the general relativistic radiative transfer code RAPTOR (see [1]). The video uses a GRMHD data slice generated by HARM (see [2] and [3]).
[1] Bronzwaer, T., Davelaar, J., et al. 2017 in prep.
[2] Gammie, C. F., McKinney, J. C., & Toth, G., 2003, Astrophysical Journal, 589, 444.
[3] Noble, S. C., Gammie, C. F., McKinney, J. C., & Del Zanna, L., 2006, Astrophysical Journal, 641, 626.
- published: 29 Jun 2017
- views: 323
developed with YouTube
Accretion disk
An accretion disk is a structure (often a circumstellar disk) formed by diffused material in orbital motion around a massive central body. The central body is typically a star. Gravity causes material in the disk to spiral inward towards the central body. Gravitational and frictional forces compress and raise the temperature of the material causing the emission of electromagnetic radiation. The frequency range of that radiation depends on the central object's mass. Accretion disks of young stars and protostars radiate in the infrared; those around neutron stars and black holes in the X-ray part of the spectrum. The study of oscillation modes in accretion disks is referred to as diskoseismology.
Manifestations
Accretion disks are a ubiquitous phenomenon in astrophysics; active galactic nuclei, protoplanetary disks, and gamma ray bursts all involve accretion disks. These disks very often give rise to astrophysical jets coming from the vicinity of the central object. Jets are an efficient way for the star-disk system to shed angular momentum without losing too much mass.
This page contains text from Wikipedia, the Free Encyclopedia -
https://wn.com/Accretion_disk
Black hole
A black hole is a geometrically defined region of spacetime exhibiting such strong gravitational effects that nothing—including particles and electromagnetic radiation such as light—can escape from inside it. The theory of general relativity predicts that a sufficiently compact mass can deform spacetime to form a black hole. The boundary of the region from which no escape is possible is called the event horizon. Although crossing the event horizon has enormous effect on the fate of the object crossing it, it appears to have no locally detectable features. In many ways a black hole acts like an ideal black body, as it reflects no light. Moreover, quantum field theory in curved spacetime predicts that event horizons emit Hawking radiation, with the same spectrum as a black body of a temperature inversely proportional to its mass. This temperature is on the order of billionths of a kelvin for black holes of stellar mass, making it essentially impossible to observe.
Objects whose gravitational fields are too strong for light to escape were first considered in the 18th century by John Michell and Pierre-Simon Laplace. The first modern solution of general relativity that would characterize a black hole was found by Karl Schwarzschild in 1916, although its interpretation as a region of space from which nothing can escape was first published by David Finkelstein in 1958. Black holes were long considered a mathematical curiosity; it was during the 1960s that theoretical work showed they were a generic prediction of general relativity. The discovery of neutron stars sparked interest in gravitationally collapsed compact objects as a possible astrophysical reality.
This page contains text from Wikipedia, the Free Encyclopedia -
https://wn.com/Black_hole
Universe Sandbox
Universe Sandbox is an interactive space and gravity simulator, developed as proprietary software. Using Universe Sandbox, one can see the effects of gravity on objects in the universe and run scale simulations of the Solar System, various galaxies or other simulations, while at the same time interacting and maintaining control over gravity, time, and other objects in the universe (moons, planets, asteroids, comets, black holes, etc.). Universe Sandbox version 2.0 was released on May 2, 2010. The original Universe Sandbox is only available for Windows-based PCs, but the new version Universe Sandbox ² is on Windows, Mac, and GNU/Linux.
See also
References
External links
This page contains text from Wikipedia, the Free Encyclopedia -
https://wn.com/Universe_Sandbox
Creative Commons
Creative Commons (CC) is a non-profit organization devoted to expanding the range of creative works available for others to build upon legally and to share. The organization has released several copyright-licenses known as Creative Commons licenses free of charge to the public. These licenses allow creators to communicate which rights they reserve, and which rights they waive for the benefit of recipients or other creators. An easy-to-understand one-page explanation of rights, with associated visual symbols, explains the specifics of each Creative Commons license. Creative Commons licenses do not replace copyright, but are based upon it. They replace individual negotiations for specific rights between copyright owner (licensor) and licensee, which are necessary under an "all rights reserved" copyright management, with a "some rights reserved" management employing standardized licenses for re-use cases where no commercial compensation is sought by the copyright owner. The result is an agile, low-overhead and low-cost copyright-management regime, profiting both copyright owners and licensees. Wikipedia uses one of these licenses.
This page contains text from Wikipedia, the Free Encyclopedia -
https://wn.com/Creative_Commons
Hole
A hole is an opening.
Hole or holes may also refer to:
Science
Technology
Construction
Entertainment
- Holes (film), a 2003 theatrical adaptation of the novel
- Holes (play), a 1998 stage adaptation of the novel
This page contains text from Wikipedia, the Free Encyclopedia -
https://wn.com/Hole
-
7:24Creating a Black Hole Accretion Disk Using Universe Sandbox²
Creating a Black Hole Accretion Disk Using Universe Sandbox²Creating a Black Hole Accretion Disk Using Universe Sandbox²
Hello and welcome to What Da Math! In this video, we will use the new effects from Universe Sandbox 2 to create an accretion disk around a black hole. Patreon page: https://www.patreon.com/user?u=2318196&ty;=h Enjoy and please subscribe. Other videos here: https://www.youtube.com/playlist?list=PL9hNFus3sjE7jgrGJYkZeTpR7lnyVAk-x Twitter: https://twitter.com/WhatDaMath Facebook: https://www.facebook.com/whatdamath Twitch: http://www.twitch.tv/whatdamath -
1:32:35Astrophysics of accretion disks - Charles Gammie
Astrophysics of accretion disks - Charles GammieAstrophysics of accretion disks - Charles Gammie
Computational Plasma Astrophysics: July 25, 2016 Prospects in Theoretical Physics is an intensive two-week summer program typically designed for graduate students and postdoctoral scholars considering a career in theoretical physics (for 2014 only the program was one week in length). First held by the School of Natural Sciences at the Institute for Advanced Study in the summer of 2002, the PiTP program is designed to provide lectures and informal sessions on the latest advances and open questions in various areas of theoretical physics. One of the goals of the program is to help the physics community train the next generation of scholars in theoretical physics. A special effort is made to reach out to women and minorities, as well as to graduate students in small universities who typically do not have the same opportunities and access to leaders in the field as graduate students in large research institutions. Prospects in Theoretical Physics builds on the strong relationship of the research groups at the Institute and Princeton University, and many faculty members from the physics departments at both institutions are actively involved in the program together with scientists from neighboring institutions. More videos on http://video.ias.edu -
4:14What is ACCRETION DISK? What does ACCRETION DISK mean? ACCRETION DISK meaning
What is ACCRETION DISK? What does ACCRETION DISK mean? ACCRETION DISK meaningWhat is ACCRETION DISK? What does ACCRETION DISK mean? ACCRETION DISK meaning
What is ACCRETION DISK? What does ACCRETION DISK mean? ACCRETION DISK meaning - ACCRETION DISK definition - ACCRETION DISK explanation. An accretion disk is a structure (often a circumstellar disk) formed by diffused material in orbital motion around a massive central body. The central body is typically a star. Gravity causes material in the disk to spiral inward towards the central body. Gravitational and frictional forces compress and raise the temperature of the material causing the emission of electromagnetic radiation. The frequency range of that radiation depends on the central object's mass. Accretion disks of young stars and protostars radiate in the infrared; those around neutron stars and black holes in the X-ray part of the spectrum. The study of oscillation modes in accretion disks is referred to as diskoseismology. Accretion disks are a ubiquitous phenomenon in astrophysics; active galactic nuclei, protoplanetary disks, and gamma ray bursts all involve accretion disks. These disks very often give rise to astrophysical jets coming from the vicinity of the central object. Jets are an efficient way for the star-disk system to shed angular momentum without losing too much mass. The most spectacular accretion disks found in nature are those of active galactic nuclei and of quasars, which are believed to be massive black holes at the center of galaxies. As matter enters the accretion disc, it follows a trajectory called a tendex line, which describes an inward spiral. This is because particles rub and bounce against each other in a turbulent flow, causing frictional heating which radiates energy away, reducing the particles' angular momentum, allowing the particle to drift inwards, driving the inward spiral. The loss of angular momentum manifests as a reduction in velocity; at a slower velocity, the particle wants to adopt a lower orbit. As the particle falls to this lower orbit, a portion of its gravitational potential energy is converted to increased velocity and the particle gains speed. Thus, the particle has lost energy even though it is now travelling faster than before; however, it has lost angular momentum. As a particle orbits closer and closer, its velocity increases, as velocity increases frictional heating increases as more and more of the particle's potential energy (relative to the black hole) is radiated away; the accretion disk of a black hole is hot enough to emit X-rays just outside the event horizon. The large luminosity of quasars is believed to be a result of gas being accreted by supermassive black holes (Lynden-Bell, 1969). Elliptical accretion disks formed at tidal disruption of stars can be typical in galactic nuclei and quasars (Gurzadyan and Ozernoy, 1979). Accretion process can convert about 10 percent to over 40 percent of the mass of an object into energy as compared to around 0.7 percent for nuclear fusion processes. In close binary systems the more massive primary component evolves faster and has already become a white dwarf, a neutron star, or a black hole, when the less massive companion reaches the giant state and exceeds its Roche lobe. A gas flow then develops from the companion star to the primary. Angular momentum conservation prevents a straight flow from one star to the other and an accretion disk forms instead. Accretion disks surrounding T Tauri stars or Herbig stars are called protoplanetary disks because they are thought to be the progenitors of planetary systems. The accreted gas in this case comes from the molecular cloud out of which the star has formed rather than a companion star. -
5:07How Black Holes Would Look To Someone Beside One!
How Black Holes Would Look To Someone Beside One!How Black Holes Would Look To Someone Beside One!
Interstellar is the first Hollywood movie to attempt depicting a black hole as it would actually be seen by somebody nearby. Get more Science at The Speaker Science: http://thespeaker.co/science/ For this, our team at Double Negative Visual Effects, in collaboration with physicist Kip Thorne, developed a code called Double Negative Gravitational Renderer (DNGR) to solve the equations for ray-bundle (light-beam) propagation through the curved spacetime of a spinning (Kerr) black hole, and to render IMAX-quality, rapidly changing images. Our ray-bundle techniques were crucial for achieving IMAX-quality smoothness without flickering; and they differ from physicists' image-generation techniques (which generally rely on individual light rays rather than ray bundles), and also differ from techniques previously used in the film industry's CGI community. This paper has four purposes: (i) to describe DNGR for physicists and CGI practitioners, who may find interesting and useful some of our unconventional techniques. (ii) To present the equations we use, when the camera is in arbitrary motion at an arbitrary location near a Kerr black hole, for mapping light sources to camera images via elliptical ray bundles. (iii) To describe new insights, from DNGR, into gravitational lensing when the camera is near the spinning black hole, rather than far away as in almost all prior studies; we focus on the shapes, sizes and influence of caustics and critical curves, the creation and annihilation of stellar images, the pattern of multiple images, and the influence of almost-trapped light rays, and we find similar results to the more familiar case of a camera far from the hole. (iv) To describe how the images of the black hole Gargantua and its accretion disk, in the movie Interstellar, were generated with DNGR—including, especially, the influences of (a) colour changes due to doppler and gravitational frequency shifts, (b) intensity changes due to the frequency shifts, (c) simulated camera lens flare, and (d) decisions that the film makers made about these influences and about the Gargantua's spin, with the goal of producing images understandable for a mass audience. There are no new astrophysical insights in this accretion-disk section of the paper, but disk novices may find it pedagogically interesting, and movie buffs may find its discussions of Interstellar interesting. Gravitational lensing by spinning black holes in astrophysics, and in the movie Interstellar. Oliver James et al (2015), Classical and Quantum Gravity http://dx.doi.org/10.1088/0264-9381/3... -
0:31Flaring Black Hole Accretion Disk in the Binary System V404 Cygni
Flaring Black Hole Accretion Disk in the Binary System V404 CygniFlaring Black Hole Accretion Disk in the Binary System V404 Cygni
On June 15, NASA's Swift caught the onset of a rare X-ray outburst from a stellar-mass black hole in the binary system V404 Cygni. Astronomers around the world are watching the event. In this system, a stream of gas from a star much like the sun flows toward a 10 solar mass black hole. Instead of spiraling toward the black hole, the gas accumulates in an accretion disk around it. Every couple of decades, the disk switches into a state that sends the gas rushing inward, starting a new outburst. Download this video in HD formats from NASA Goddard's Scientific Visualization Studio http://svs.gsfc.nasa.gov/cgi-bin/details.cgi?aid=11110 -
12:57Forming an Accretion Disk around a Black Hole
Forming an Accretion Disk around a Black HoleForming an Accretion Disk around a Black Hole
Welcome to another experiment in Universe Sandbox 2 Let's play series. Today we'll be testing a user made suggestion asking if we can form an accretion disk in Universe Sandbox 2, let's find out! Universe Sandbox 2 is a space sandbox that is still a work in progress, and is an awesome game and educational tool. But, keep in mind the physics and results depicted in this game are to be taken with a grain a salt, the game tries to, but does not always accurately reproduce the expectations of our current knowledge of physics, the game is still an early access alpha and is still being worked on! A lot of the ideas in this series are suggestions by viewers and aren't always intended to be "educational," so take the results of this test with a grain of salt! Buy and Support Universe Sandbox 2 on Steam http://store.steampowered.com/app/230290/ You read descriptions! ツ -
1:21Accretion Disk around Black Hole
Accretion Disk around Black HoleAccretion Disk around Black Hole
The disk is based on a non-relativistic Smoothed-Particle-Hydrodynamics (SPH) simulation. The apparent distortion of the disk is due to the bending of light within the Schwarzschild spacetime. Besides the primary image of the disk, there are also higher order images (lower ring and upper thin ring) visible. The lower ring shows the rear bottom side of the disk. The color encodes the apparent temperature where blue is hot and red is cold. The left part of the disk approaches the observer and, thus, appears hotter due to the Doppler effect. You also see some bright spots which smear out already after one revolution around the black hole. -
2:20Accretion disc - Video Learning - WizScience.com
Accretion disc - Video Learning - WizScience.comAccretion disc - Video Learning - WizScience.com
An "accretion disk" is a structure formed by diffused material in orbital motion around a massive central body. The central body is typically a star. Gravity causes material in the disc to spiral inward towards the central body. Gravitational and frictional forces compress and raise the temperature of the material causing the emission of electromagnetic radiation. The frequency range of that radiation depends on the central object's mass. Accretion discs of young stars and protostars radiate in the infrared; those around neutron stars and black holes in the X-ray part of the spectrum. The study of oscillation modes in accretion discs is referred to as "diskoseismology". Accretion discs are a ubiquitous phenomenon in astrophysics; active galactic nuclei, protoplanetary discs, and gamma ray bursts all involve accretion discs. These discs very often give rise to astrophysical jets coming from the vicinity of the central object. Jets are an efficient way for the star-disc system to shed angular momentum without losing too much mass. The most spectacular accretion discs found in nature are those of active galactic nuclei and of quasars, which are believed to be massive black holes at the center of galaxies. As matter follows the tendex line into a black hole, the intense gravitational gradient gives rise to intense frictional heating; the accretion disc of a black hole is hot enough to emit X-rays just outside of the event horizon. The large luminosity of quasars is believed to be a result of gas being accreted by supermassive black holes . Elliptical accretion discs formed at tidal disruption of stars can be typical in galactic nuclei and quasars . Accretion process can convert about 10 percent to over 40 percent of the mass of an object into energy as compared to around 0.7 percent for nuclear fusion processes. Wiz Science™ is "the" learning channel for children and all ages. SUBSCRIBE TODAY Disclaimer: This video is for your information only. The author or publisher does not guarantee the accuracy of the content presented in this video. USE AT YOUR OWN RISK. Background Music: "The Place Inside" by Silent Partner (royalty-free) from YouTube Audio Library. This video uses material/images from https://en.wikipedia.org/wiki/Accretion+disc, which is released under Creative Commons Attribution-Share-Alike License 3.0 http://creativecommons.org/licenses/by-sa/3.0/ . This video is licensed under Creative Commons Attribution-Share-Alike License 3.0 http://creativecommons.org/licenses/by-sa/3.0/ . To reuse/adapt the content in your own work, you must comply with the license terms. Wiz Science™ is "the" learning channel for children and all ages. SUBSCRIBE TODAY Disclaimer: This video is for your information only. The author or publisher does not guarantee the accuracy of the content presented in this video. USE AT YOUR OWN RISK. Background Music: "The Place Inside" by Silent Partner (royalty-free) from YouTube Audio Library. This video uses material/images from https://en.wikipedia.org/wiki/Accretion+disc, which is released under Creative Commons Attribution-Share-Alike License 3.0 http://creativecommons.org/licenses/by-sa/3.0/ . This video is licensed under Creative Commons Attribution-Share-Alike License 3.0 http://creativecommons.org/licenses/by-sa/3.0/ . To reuse/adapt the content in your own work, you must comply with the license terms. -
4:58Starbound Soundtrack - Accretion Disc
Starbound Soundtrack - Accretion DiscStarbound Soundtrack - Accretion Disc
Full Playlist of Starbound Soundtrack: https://www.youtube.com/playlist?list=PL7DXTXnlwEuN4eTTyMIOZJfoZN4IQgx8z&feature;=mh_lolz -
0:27Quasar With Accretion Disk and Jet
Quasar With Accretion Disk and JetQuasar With Accretion Disk and Jet
Using two of the world's largest telescopes, an international team of astronomers have found evidence of a collision between galaxies driving intense activity in a highly luminous quasar. The scientists, led by Montserrat Villar Martin of the Instituto de Astrofisica de Andalucía-CSIC in Spain, used the Very Large Telescope (VLT) in Chile and the Gran Telescopio Canarias (GTC) on La Palma in the Canary Islands, to study activity from the quasar SDSS J0123+00. They publish their work in a paper in the journal Monthly Notices of the Royal Astronomical Society. Several types of galaxies, known as active galaxies, emit enormous amounts of energy from their central region or nucleus, with the most luminous objects known as quasars. Most scientists argue that quasars contain a central black hole, with a mass of at least several million Suns. The intense gravitational field created by the black hole drags material inexorably inwards. Before falling in, this material settles in an accretion disk where it becomes very hot and emits large amounts of energy responsible for most of the brightness of the quasar. Around the central quasar 'engine' is a torus (thick ring) opaque to the visible light emitted by the accretion disk. From a terrestrial perspective, if the torus is face-on then the radiation from the disk can be seen and the system is designated type 1, whereas in type 2 quasars the torus is edge-on and the radiation is concealed. source: http://www.iaa.es/~rosa/AYA2010/AYA2010/Novedades/Entradas/2010/6/23_Galaxy_encounter_fire_up_quasar.html -
0:21Accretion disk - planetary formation
Accretion disk - planetary formationAccretion disk - planetary formation
-
0:22Black Hole Accretion Disk
Black Hole Accretion DiskBlack Hole Accretion Disk
In this video, the camera rotates around a spinning (Kerr) black hole that is surrounded by an accretion disk (a vortex of matter attracted by the black hole that orbits it and eventually falls in). The accreting matter emits synchrotron radiation at various frequencies; in the video, we see radiation emitted at 230 GHz. If you have any questions, feel free to ask! Credits: T. Bronzwaer, J. Davelaar, Z. Younsi 2017. The video was made using the general relativistic radiative transfer code RAPTOR (see [1]). The video uses a GRMHD data slice generated by HARM (see [2] and [3]). [1] Bronzwaer, T., Davelaar, J., et al. 2017 in prep. [2] Gammie, C. F., McKinney, J. C., & Toth, G., 2003, Astrophysical Journal, 589, 444. [3] Noble, S. C., Gammie, C. F., McKinney, J. C., & Del Zanna, L., 2006, Astrophysical Journal, 641, 626. -
0:51Accretion DIsk SImulation
Accretion DIsk SImulation -
7:05Vortex Technologies Accretion Disk Demonstration
Vortex Technologies Accretion Disk DemonstrationVortex Technologies Accretion Disk Demonstration
Watch and see what happens when two electromagnetic vortex fields collide! -
2:01Evolution of magnetic field in a thick accretion disk
Evolution of magnetic field in a thick accretion diskEvolution of magnetic field in a thick accretion disk
-
Creating a Black Hole Accretion Disk Using Universe Sandbox²
Hello and welcome to What Da Math! In this video, we will use the new effects from Universe Sandbox 2 to create an accretion disk around a black hole. Patreon page: https://www.patreon.com/user?u=2318196&ty;=h Enjoy and please subscribe. Other videos here: https://www.youtube.com/playlist?list=PL9hNFus3sjE7jgrGJYkZeTpR7lnyVAk-x Twitter: https://twitter.com/WhatDaMath Facebook: https://www.facebook.com/whatdamath Twitch: http://www.twitch.tv/whatdamath
published: 27 Nov 2016 -
Astrophysics of accretion disks - Charles Gammie
Computational Plasma Astrophysics: July 25, 2016 Prospects in Theoretical Physics is an intensive two-week summer program typically designed for graduate students and postdoctoral scholars considering a career in theoretical physics (for 2014 only the program was one week in length). First held by the School of Natural Sciences at the Institute for Advanced Study in the summer of 2002, the PiTP program is designed to provide lectures and informal sessions on the latest advances and open questions in various areas of theoretical physics. One of the goals of the program is to help the physics community train the next generation of scholars in theoretical physics. A special effort is made to reach out to women and minorities, as well as to graduate students in small universities who typical...
published: 25 Jul 2016 -
What is ACCRETION DISK? What does ACCRETION DISK mean? ACCRETION DISK meaning
What is ACCRETION DISK? What does ACCRETION DISK mean? ACCRETION DISK meaning - ACCRETION DISK definition - ACCRETION DISK explanation. An accretion disk is a structure (often a circumstellar disk) formed by diffused material in orbital motion around a massive central body. The central body is typically a star. Gravity causes material in the disk to spiral inward towards the central body. Gravitational and frictional forces compress and raise the temperature of the material causing the emission of electromagnetic radiation. The frequency range of that radiation depends on the central object's mass. Accretion disks of young stars and protostars radiate in the infrared; those around neutron stars and black holes in the X-ray part of the spectrum. The study of oscillation modes in accretion ...
published: 01 Oct 2016 -
How Black Holes Would Look To Someone Beside One!
Interstellar is the first Hollywood movie to attempt depicting a black hole as it would actually be seen by somebody nearby. Get more Science at The Speaker Science: http://thespeaker.co/science/ For this, our team at Double Negative Visual Effects, in collaboration with physicist Kip Thorne, developed a code called Double Negative Gravitational Renderer (DNGR) to solve the equations for ray-bundle (light-beam) propagation through the curved spacetime of a spinning (Kerr) black hole, and to render IMAX-quality, rapidly changing images. Our ray-bundle techniques were crucial for achieving IMAX-quality smoothness without flickering; and they differ from physicists' image-generation techniques (which generally rely on individual light rays rather than ray bundles), and also differ from t...
published: 28 Oct 2015 -
Flaring Black Hole Accretion Disk in the Binary System V404 Cygni
On June 15, NASA's Swift caught the onset of a rare X-ray outburst from a stellar-mass black hole in the binary system V404 Cygni. Astronomers around the world are watching the event. In this system, a stream of gas from a star much like the sun flows toward a 10 solar mass black hole. Instead of spiraling toward the black hole, the gas accumulates in an accretion disk around it. Every couple of decades, the disk switches into a state that sends the gas rushing inward, starting a new outburst. Download this video in HD formats from NASA Goddard's Scientific Visualization Studio http://svs.gsfc.nasa.gov/cgi-bin/details.cgi?aid=11110
published: 30 Jun 2015 -
Forming an Accretion Disk around a Black Hole
Welcome to another experiment in Universe Sandbox 2 Let's play series. Today we'll be testing a user made suggestion asking if we can form an accretion disk in Universe Sandbox 2, let's find out! Universe Sandbox 2 is a space sandbox that is still a work in progress, and is an awesome game and educational tool. But, keep in mind the physics and results depicted in this game are to be taken with a grain a salt, the game tries to, but does not always accurately reproduce the expectations of our current knowledge of physics, the game is still an early access alpha and is still being worked on! A lot of the ideas in this series are suggestions by viewers and aren't always intended to be "educational," so take the results of this test with a grain of salt! Buy and Support Universe Sandbo...
published: 10 Apr 2018 -
Accretion Disk around Black Hole
The disk is based on a non-relativistic Smoothed-Particle-Hydrodynamics (SPH) simulation. The apparent distortion of the disk is due to the bending of light within the Schwarzschild spacetime. Besides the primary image of the disk, there are also higher order images (lower ring and upper thin ring) visible. The lower ring shows the rear bottom side of the disk. The color encodes the apparent temperature where blue is hot and red is cold. The left part of the disk approaches the observer and, thus, appears hotter due to the Doppler effect. You also see some bright spots which smear out already after one revolution around the black hole.
published: 27 Oct 2014 -
Accretion disc - Video Learning - WizScience.com
An "accretion disk" is a structure formed by diffused material in orbital motion around a massive central body. The central body is typically a star. Gravity causes material in the disc to spiral inward towards the central body. Gravitational and frictional forces compress and raise the temperature of the material causing the emission of electromagnetic radiation. The frequency range of that radiation depends on the central object's mass. Accretion discs of young stars and protostars radiate in the infrared; those around neutron stars and black holes in the X-ray part of the spectrum. The study of oscillation modes in accretion discs is referred to as "diskoseismology". Accretion discs are a ubiquitous phenomenon in astrophysics; active galactic nuclei, protoplanetary discs, and gamma...
published: 10 Sep 2015 -
Starbound Soundtrack - Accretion Disc
Full Playlist of Starbound Soundtrack: https://www.youtube.com/playlist?list=PL7DXTXnlwEuN4eTTyMIOZJfoZN4IQgx8z&feature;=mh_lolz
published: 08 Dec 2013 -
Quasar With Accretion Disk and Jet
Using two of the world's largest telescopes, an international team of astronomers have found evidence of a collision between galaxies driving intense activity in a highly luminous quasar. The scientists, led by Montserrat Villar Martin of the Instituto de Astrofisica de Andalucía-CSIC in Spain, used the Very Large Telescope (VLT) in Chile and the Gran Telescopio Canarias (GTC) on La Palma in the Canary Islands, to study activity from the quasar SDSS J0123+00. They publish their work in a paper in the journal Monthly Notices of the Royal Astronomical Society. Several types of galaxies, known as active galaxies, emit enormous amounts of energy from their central region or nucleus, with the most luminous objects known as quasars. Most scientists argue that quasars contain a central black h...
published: 25 Jun 2010 -
Accretion disk - planetary formation
published: 09 Aug 2014 -
Black Hole Accretion Disk
In this video, the camera rotates around a spinning (Kerr) black hole that is surrounded by an accretion disk (a vortex of matter attracted by the black hole that orbits it and eventually falls in). The accreting matter emits synchrotron radiation at various frequencies; in the video, we see radiation emitted at 230 GHz. If you have any questions, feel free to ask! Credits: T. Bronzwaer, J. Davelaar, Z. Younsi 2017. The video was made using the general relativistic radiative transfer code RAPTOR (see [1]). The video uses a GRMHD data slice generated by HARM (see [2] and [3]). [1] Bronzwaer, T., Davelaar, J., et al. 2017 in prep. [2] Gammie, C. F., McKinney, J. C., & Toth, G., 2003, Astrophysical Journal, 589, 444. [3] Noble, S. C., Gammie, C. F., McKinney, J. C., & Del Zanna, L., 2006, As...
published: 29 Jun 2017 -
-
Vortex Technologies Accretion Disk Demonstration
Watch and see what happens when two electromagnetic vortex fields collide!
published: 18 Apr 2015 -
Evolution of magnetic field in a thick accretion disk
published: 10 Mar 2015
developed with YouTube
7:24
Creating a Black Hole Accretion Disk Using Universe Sandbox²
- Order: Reorder
- Duration: 7:24
- Updated: 27 Nov 2016
- views: 11634
Hello and welcome to What Da Math!
In this video, we will use the new effects from Universe Sandbox 2 to create an accretion disk around a black hole.
Patreon ...
Hello and welcome to What Da Math!
In this video, we will use the new effects from Universe Sandbox 2 to create an accretion disk around a black hole.
Patreon page:
https://www.patreon.com/user?u=2318196&ty;=h
Enjoy and please subscribe.
Other videos here: https://www.youtube.com/playlist?list=PL9hNFus3sjE7jgrGJYkZeTpR7lnyVAk-x
Twitter: https://twitter.com/WhatDaMath
Facebook: https://www.facebook.com/whatdamath
Twitch: http://www.twitch.tv/whatdamath
https://wn.com/Creating_A_Black_Hole_Accretion_Disk_Using_Universe_Sandbox²
Hello and welcome to What Da Math!
In this video, we will use the new effects from Universe Sandbox 2 to create an accretion disk around a black hole.
Patreon page:
https://www.patreon.com/user?u=2318196&ty;=h
Enjoy and please subscribe.
Other videos here: https://www.youtube.com/playlist?list=PL9hNFus3sjE7jgrGJYkZeTpR7lnyVAk-x
Twitter: https://twitter.com/WhatDaMath
Facebook: https://www.facebook.com/whatdamath
Twitch: http://www.twitch.tv/whatdamath
- published: 27 Nov 2016
- views: 11634
1:32:35
Astrophysics of accretion disks - Charles Gammie
- Order: Reorder
- Duration: 1:32:35
- Updated: 25 Jul 2016
- views: 2340
Computational Plasma Astrophysics: July 25, 2016
Prospects in Theoretical Physics is an intensive two-week summer program typically designed for graduate stude...
Computational Plasma Astrophysics: July 25, 2016
Prospects in Theoretical Physics is an intensive two-week summer program typically designed for graduate students and postdoctoral scholars considering a career in theoretical physics (for 2014 only the program was one week in length). First held by the School of Natural Sciences at the Institute for Advanced Study in the summer of 2002, the PiTP program is designed to provide lectures and informal sessions on the latest advances and open questions in various areas of theoretical physics.
One of the goals of the program is to help the physics community train the next generation of scholars in theoretical physics. A special effort is made to reach out to women and minorities, as well as to graduate students in small universities who typically do not have the same opportunities and access to leaders in the field as graduate students in large research institutions.
Prospects in Theoretical Physics builds on the strong relationship of the research groups at the Institute and Princeton University, and many faculty members from the physics departments at both institutions are actively involved in the program together with scientists from neighboring institutions.
More videos on http://video.ias.edu
https://wn.com/Astrophysics_Of_Accretion_Disks_Charles_Gammie
Computational Plasma Astrophysics: July 25, 2016
Prospects in Theoretical Physics is an intensive two-week summer program typically designed for graduate students and postdoctoral scholars considering a career in theoretical physics (for 2014 only the program was one week in length). First held by the School of Natural Sciences at the Institute for Advanced Study in the summer of 2002, the PiTP program is designed to provide lectures and informal sessions on the latest advances and open questions in various areas of theoretical physics.
One of the goals of the program is to help the physics community train the next generation of scholars in theoretical physics. A special effort is made to reach out to women and minorities, as well as to graduate students in small universities who typically do not have the same opportunities and access to leaders in the field as graduate students in large research institutions.
Prospects in Theoretical Physics builds on the strong relationship of the research groups at the Institute and Princeton University, and many faculty members from the physics departments at both institutions are actively involved in the program together with scientists from neighboring institutions.
More videos on http://video.ias.edu
- published: 25 Jul 2016
- views: 2340
4:14
What is ACCRETION DISK? What does ACCRETION DISK mean? ACCRETION DISK meaning
- Order: Reorder
- Duration: 4:14
- Updated: 01 Oct 2016
- views: 1569
What is ACCRETION DISK? What does ACCRETION DISK mean? ACCRETION DISK meaning - ACCRETION DISK definition - ACCRETION DISK explanation.
An accretion disk is a ...
What is ACCRETION DISK? What does ACCRETION DISK mean? ACCRETION DISK meaning - ACCRETION DISK definition - ACCRETION DISK explanation.
An accretion disk is a structure (often a circumstellar disk) formed by diffused material in orbital motion around a massive central body. The central body is typically a star. Gravity causes material in the disk to spiral inward towards the central body. Gravitational and frictional forces compress and raise the temperature of the material causing the emission of electromagnetic radiation. The frequency range of that radiation depends on the central object's mass. Accretion disks of young stars and protostars radiate in the infrared; those around neutron stars and black holes in the X-ray part of the spectrum. The study of oscillation modes in accretion disks is referred to as diskoseismology.
Accretion disks are a ubiquitous phenomenon in astrophysics; active galactic nuclei, protoplanetary disks, and gamma ray bursts all involve accretion disks. These disks very often give rise to astrophysical jets coming from the vicinity of the central object. Jets are an efficient way for the star-disk system to shed angular momentum without losing too much mass.
The most spectacular accretion disks found in nature are those of active galactic nuclei and of quasars, which are believed to be massive black holes at the center of galaxies. As matter enters the accretion disc, it follows a trajectory called a tendex line, which describes an inward spiral. This is because particles rub and bounce against each other in a turbulent flow, causing frictional heating which radiates energy away, reducing the particles' angular momentum, allowing the particle to drift inwards, driving the inward spiral. The loss of angular momentum manifests as a reduction in velocity; at a slower velocity, the particle wants to adopt a lower orbit. As the particle falls to this lower orbit, a portion of its gravitational potential energy is converted to increased velocity and the particle gains speed. Thus, the particle has lost energy even though it is now travelling faster than before; however, it has lost angular momentum. As a particle orbits closer and closer, its velocity increases, as velocity increases frictional heating increases as more and more of the particle's potential energy (relative to the black hole) is radiated away; the accretion disk of a black hole is hot enough to emit X-rays just outside the event horizon. The large luminosity of quasars is believed to be a result of gas being accreted by supermassive black holes (Lynden-Bell, 1969). Elliptical accretion disks formed at tidal disruption of stars can be typical in galactic nuclei and quasars (Gurzadyan and Ozernoy, 1979). Accretion process can convert about 10 percent to over 40 percent of the mass of an object into energy as compared to around 0.7 percent for nuclear fusion processes.
In close binary systems the more massive primary component evolves faster and has already become a white dwarf, a neutron star, or a black hole, when the less massive companion reaches the giant state and exceeds its Roche lobe. A gas flow then develops from the companion star to the primary. Angular momentum conservation prevents a straight flow from one star to the other and an accretion disk forms instead.
Accretion disks surrounding T Tauri stars or Herbig stars are called protoplanetary disks because they are thought to be the progenitors of planetary systems. The accreted gas in this case comes from the molecular cloud out of which the star has formed rather than a companion star.
https://wn.com/What_Is_Accretion_Disk_What_Does_Accretion_Disk_Mean_Accretion_Disk_Meaning
What is ACCRETION DISK? What does ACCRETION DISK mean? ACCRETION DISK meaning - ACCRETION DISK definition - ACCRETION DISK explanation.
An accretion disk is a structure (often a circumstellar disk) formed by diffused material in orbital motion around a massive central body. The central body is typically a star. Gravity causes material in the disk to spiral inward towards the central body. Gravitational and frictional forces compress and raise the temperature of the material causing the emission of electromagnetic radiation. The frequency range of that radiation depends on the central object's mass. Accretion disks of young stars and protostars radiate in the infrared; those around neutron stars and black holes in the X-ray part of the spectrum. The study of oscillation modes in accretion disks is referred to as diskoseismology.
Accretion disks are a ubiquitous phenomenon in astrophysics; active galactic nuclei, protoplanetary disks, and gamma ray bursts all involve accretion disks. These disks very often give rise to astrophysical jets coming from the vicinity of the central object. Jets are an efficient way for the star-disk system to shed angular momentum without losing too much mass.
The most spectacular accretion disks found in nature are those of active galactic nuclei and of quasars, which are believed to be massive black holes at the center of galaxies. As matter enters the accretion disc, it follows a trajectory called a tendex line, which describes an inward spiral. This is because particles rub and bounce against each other in a turbulent flow, causing frictional heating which radiates energy away, reducing the particles' angular momentum, allowing the particle to drift inwards, driving the inward spiral. The loss of angular momentum manifests as a reduction in velocity; at a slower velocity, the particle wants to adopt a lower orbit. As the particle falls to this lower orbit, a portion of its gravitational potential energy is converted to increased velocity and the particle gains speed. Thus, the particle has lost energy even though it is now travelling faster than before; however, it has lost angular momentum. As a particle orbits closer and closer, its velocity increases, as velocity increases frictional heating increases as more and more of the particle's potential energy (relative to the black hole) is radiated away; the accretion disk of a black hole is hot enough to emit X-rays just outside the event horizon. The large luminosity of quasars is believed to be a result of gas being accreted by supermassive black holes (Lynden-Bell, 1969). Elliptical accretion disks formed at tidal disruption of stars can be typical in galactic nuclei and quasars (Gurzadyan and Ozernoy, 1979). Accretion process can convert about 10 percent to over 40 percent of the mass of an object into energy as compared to around 0.7 percent for nuclear fusion processes.
In close binary systems the more massive primary component evolves faster and has already become a white dwarf, a neutron star, or a black hole, when the less massive companion reaches the giant state and exceeds its Roche lobe. A gas flow then develops from the companion star to the primary. Angular momentum conservation prevents a straight flow from one star to the other and an accretion disk forms instead.
Accretion disks surrounding T Tauri stars or Herbig stars are called protoplanetary disks because they are thought to be the progenitors of planetary systems. The accreted gas in this case comes from the molecular cloud out of which the star has formed rather than a companion star.
- published: 01 Oct 2016
- views: 1569
5:07
How Black Holes Would Look To Someone Beside One!
- Order: Reorder
- Duration: 5:07
- Updated: 28 Oct 2015
- views: 26305
Interstellar is the first Hollywood movie to attempt depicting a black hole as it would actually be seen by somebody nearby.
Get more Science at The Speaker S...
Interstellar is the first Hollywood movie to attempt depicting a black hole as it would actually be seen by somebody nearby.
Get more Science at The Speaker Science: http://thespeaker.co/science/
For this, our team at Double Negative Visual Effects, in collaboration with physicist Kip Thorne, developed a code called Double Negative Gravitational Renderer (DNGR) to solve the equations for ray-bundle (light-beam) propagation through the curved spacetime of a spinning (Kerr) black hole, and to render IMAX-quality, rapidly changing images.
Our ray-bundle techniques were crucial for achieving IMAX-quality smoothness without flickering; and they differ from physicists' image-generation techniques (which generally rely on individual light rays rather than ray bundles), and also differ from techniques previously used in the film industry's CGI community.
This paper has four purposes: (i) to describe DNGR for physicists and CGI practitioners, who may find interesting and useful some of our unconventional techniques. (ii)
To present the equations we use, when the camera is in arbitrary motion at an arbitrary location near a Kerr black hole, for mapping light sources to camera images via elliptical ray bundles. (iii)
To describe new insights, from DNGR, into gravitational lensing when the camera is near the spinning black hole, rather than far away as in almost all prior studies; we focus on the shapes, sizes and influence of caustics and critical curves, the creation and annihilation of stellar images, the pattern of multiple images, and the influence of almost-trapped light rays, and we find similar results to the more familiar case of a camera far from the hole. (iv)
To describe how the images of the black hole Gargantua and its accretion disk, in the movie Interstellar, were generated with DNGR—including, especially, the influences of (a) colour changes due to doppler and gravitational frequency shifts, (b) intensity changes due to the frequency shifts, (c) simulated camera lens flare, and (d) decisions that the film makers made about these influences and about the Gargantua's spin, with the goal of producing images understandable for a mass audience. There are no new astrophysical insights in this accretion-disk section of the paper, but disk novices may find it pedagogically interesting, and movie buffs may find its discussions of Interstellar interesting.
Gravitational lensing by spinning black holes in astrophysics, and in the movie Interstellar.
Oliver James et al (2015), Classical and Quantum Gravity http://dx.doi.org/10.1088/0264-9381/3...
https://wn.com/How_Black_Holes_Would_Look_To_Someone_Beside_One
Interstellar is the first Hollywood movie to attempt depicting a black hole as it would actually be seen by somebody nearby.
Get more Science at The Speaker Science: http://thespeaker.co/science/
For this, our team at Double Negative Visual Effects, in collaboration with physicist Kip Thorne, developed a code called Double Negative Gravitational Renderer (DNGR) to solve the equations for ray-bundle (light-beam) propagation through the curved spacetime of a spinning (Kerr) black hole, and to render IMAX-quality, rapidly changing images.
Our ray-bundle techniques were crucial for achieving IMAX-quality smoothness without flickering; and they differ from physicists' image-generation techniques (which generally rely on individual light rays rather than ray bundles), and also differ from techniques previously used in the film industry's CGI community.
This paper has four purposes: (i) to describe DNGR for physicists and CGI practitioners, who may find interesting and useful some of our unconventional techniques. (ii)
To present the equations we use, when the camera is in arbitrary motion at an arbitrary location near a Kerr black hole, for mapping light sources to camera images via elliptical ray bundles. (iii)
To describe new insights, from DNGR, into gravitational lensing when the camera is near the spinning black hole, rather than far away as in almost all prior studies; we focus on the shapes, sizes and influence of caustics and critical curves, the creation and annihilation of stellar images, the pattern of multiple images, and the influence of almost-trapped light rays, and we find similar results to the more familiar case of a camera far from the hole. (iv)
To describe how the images of the black hole Gargantua and its accretion disk, in the movie Interstellar, were generated with DNGR—including, especially, the influences of (a) colour changes due to doppler and gravitational frequency shifts, (b) intensity changes due to the frequency shifts, (c) simulated camera lens flare, and (d) decisions that the film makers made about these influences and about the Gargantua's spin, with the goal of producing images understandable for a mass audience. There are no new astrophysical insights in this accretion-disk section of the paper, but disk novices may find it pedagogically interesting, and movie buffs may find its discussions of Interstellar interesting.
Gravitational lensing by spinning black holes in astrophysics, and in the movie Interstellar.
Oliver James et al (2015), Classical and Quantum Gravity http://dx.doi.org/10.1088/0264-9381/3...
- published: 28 Oct 2015
- views: 26305
0:31
Flaring Black Hole Accretion Disk in the Binary System V404 Cygni
- Order: Reorder
- Duration: 0:31
- Updated: 30 Jun 2015
- views: 278949
On June 15, NASA's Swift caught the onset of a rare X-ray outburst from a stellar-mass black hole in the binary system V404 Cygni. Astronomers around the world ...
On June 15, NASA's Swift caught the onset of a rare X-ray outburst from a stellar-mass black hole in the binary system V404 Cygni. Astronomers around the world are watching the event. In this system, a stream of gas from a star much like the sun flows toward a 10 solar mass black hole. Instead of spiraling toward the black hole, the gas accumulates in an accretion disk around it. Every couple of decades, the disk switches into a state that sends the gas rushing inward, starting a new outburst.
Download this video in HD formats from NASA Goddard's Scientific Visualization Studio
http://svs.gsfc.nasa.gov/cgi-bin/details.cgi?aid=11110
https://wn.com/Flaring_Black_Hole_Accretion_Disk_In_The_Binary_System_V404_Cygni
On June 15, NASA's Swift caught the onset of a rare X-ray outburst from a stellar-mass black hole in the binary system V404 Cygni. Astronomers around the world are watching the event. In this system, a stream of gas from a star much like the sun flows toward a 10 solar mass black hole. Instead of spiraling toward the black hole, the gas accumulates in an accretion disk around it. Every couple of decades, the disk switches into a state that sends the gas rushing inward, starting a new outburst.
Download this video in HD formats from NASA Goddard's Scientific Visualization Studio
http://svs.gsfc.nasa.gov/cgi-bin/details.cgi?aid=11110
- published: 30 Jun 2015
- views: 278949
12:57
Forming an Accretion Disk around a Black Hole
- Order: Reorder
- Duration: 12:57
- Updated: 10 Apr 2018
- views: 478
Welcome to another experiment in Universe Sandbox 2 Let's play series.
Today we'll be testing a user made suggestion asking if we can form an accretion disk in...
Welcome to another experiment in Universe Sandbox 2 Let's play series.
Today we'll be testing a user made suggestion asking if we can form an accretion disk in Universe Sandbox 2, let's find out!
Universe Sandbox 2 is a space sandbox that is still a work in progress, and is an awesome game and educational tool. But, keep in mind the physics and results depicted in this game are to be taken with a grain a salt, the game tries to, but does not always accurately reproduce the expectations of our current knowledge of physics, the game is still an early access alpha and is still being worked on!
A lot of the ideas in this series are suggestions by viewers and aren't always intended to be "educational," so take the results of this test with a grain of salt!
Buy and Support Universe Sandbox 2 on Steam
http://store.steampowered.com/app/230290/
You read descriptions! ツ
https://wn.com/Forming_An_Accretion_Disk_Around_A_Black_Hole
Welcome to another experiment in Universe Sandbox 2 Let's play series.
Today we'll be testing a user made suggestion asking if we can form an accretion disk in Universe Sandbox 2, let's find out!
Universe Sandbox 2 is a space sandbox that is still a work in progress, and is an awesome game and educational tool. But, keep in mind the physics and results depicted in this game are to be taken with a grain a salt, the game tries to, but does not always accurately reproduce the expectations of our current knowledge of physics, the game is still an early access alpha and is still being worked on!
A lot of the ideas in this series are suggestions by viewers and aren't always intended to be "educational," so take the results of this test with a grain of salt!
Buy and Support Universe Sandbox 2 on Steam
http://store.steampowered.com/app/230290/
You read descriptions! ツ
- published: 10 Apr 2018
- views: 478
1:21
Accretion Disk around Black Hole
- Order: Reorder
- Duration: 1:21
- Updated: 27 Oct 2014
- views: 15521
The disk is based on a non-relativistic Smoothed-Particle-Hydrodynamics (SPH) simulation.
The apparent distortion of the disk is due to the bending of light wit...
The disk is based on a non-relativistic Smoothed-Particle-Hydrodynamics (SPH) simulation.
The apparent distortion of the disk is due to the bending of light within the Schwarzschild spacetime. Besides the primary image of the disk, there are also higher order images (lower ring and upper thin ring) visible. The lower ring shows the rear bottom side of the disk. The color encodes the apparent temperature where blue is hot and red is cold. The left part of the disk approaches the observer and, thus, appears hotter due to the Doppler effect. You also see some bright spots which smear out already after one revolution around the black hole.
https://wn.com/Accretion_Disk_Around_Black_Hole
The disk is based on a non-relativistic Smoothed-Particle-Hydrodynamics (SPH) simulation.
The apparent distortion of the disk is due to the bending of light within the Schwarzschild spacetime. Besides the primary image of the disk, there are also higher order images (lower ring and upper thin ring) visible. The lower ring shows the rear bottom side of the disk. The color encodes the apparent temperature where blue is hot and red is cold. The left part of the disk approaches the observer and, thus, appears hotter due to the Doppler effect. You also see some bright spots which smear out already after one revolution around the black hole.
- published: 27 Oct 2014
- views: 15521
2:20
Accretion disc - Video Learning - WizScience.com
- Order: Reorder
- Duration: 2:20
- Updated: 10 Sep 2015
- views: 778
An "accretion disk" is a structure formed by diffused material in orbital motion around a massive central body. The central body is typically a star. Gravity ...
An "accretion disk" is a structure formed by diffused material in orbital motion around a massive central body. The central body is typically a star. Gravity causes material in the disc to spiral inward towards the central body. Gravitational and frictional forces compress and raise the temperature of the material causing the emission of electromagnetic radiation. The frequency range of that radiation depends on the central object's mass. Accretion discs of young stars and protostars radiate in the infrared; those around neutron stars and black holes in the X-ray part of the spectrum. The study of oscillation modes in accretion discs is referred to as "diskoseismology".
Accretion discs are a ubiquitous phenomenon in astrophysics; active galactic nuclei, protoplanetary discs, and gamma ray bursts all involve accretion discs. These discs very often give rise to astrophysical jets coming from the vicinity of the central object. Jets are an efficient way for the star-disc system to shed angular momentum without losing too much mass.
The most spectacular accretion discs found in nature are those of active galactic nuclei and of quasars, which are believed to be massive black holes at the center of galaxies. As matter follows the tendex line into a black hole, the intense gravitational gradient gives rise to intense frictional heating; the accretion disc of a black hole is hot enough to emit X-rays just outside of the event horizon. The large luminosity of quasars is believed to be a result of gas being accreted by supermassive black holes . Elliptical accretion discs formed at tidal disruption of stars can be typical in galactic nuclei and quasars . Accretion process can convert about 10 percent to over 40 percent of the mass of an object into energy as compared to around 0.7 percent for nuclear fusion processes.
Wiz Science™ is "the" learning channel for children and all ages.
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Disclaimer: This video is for your information only. The author or publisher does not guarantee the accuracy of the content presented in this video. USE AT YOUR OWN RISK.
Background Music:
"The Place Inside" by Silent Partner (royalty-free) from YouTube Audio Library.
This video uses material/images from https://en.wikipedia.org/wiki/Accretion+disc, which is released under Creative Commons Attribution-Share-Alike License 3.0 http://creativecommons.org/licenses/by-sa/3.0/ . This video is licensed under Creative Commons Attribution-Share-Alike License 3.0 http://creativecommons.org/licenses/by-sa/3.0/ . To reuse/adapt the content in your own work, you must comply with the license terms.
Wiz Science™ is "the" learning channel for children and all ages.
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Disclaimer: This video is for your information only. The author or publisher does not guarantee the accuracy of the content presented in this video. USE AT YOUR OWN RISK.
Background Music:
"The Place Inside" by Silent Partner (royalty-free) from YouTube Audio Library.
This video uses material/images from https://en.wikipedia.org/wiki/Accretion+disc, which is released under Creative Commons Attribution-Share-Alike License 3.0 http://creativecommons.org/licenses/by-sa/3.0/ . This video is licensed under Creative Commons Attribution-Share-Alike License 3.0 http://creativecommons.org/licenses/by-sa/3.0/ . To reuse/adapt the content in your own work, you must comply with the license terms.
https://wn.com/Accretion_Disc_Video_Learning_Wizscience.Com
An "accretion disk" is a structure formed by diffused material in orbital motion around a massive central body. The central body is typically a star. Gravity causes material in the disc to spiral inward towards the central body. Gravitational and frictional forces compress and raise the temperature of the material causing the emission of electromagnetic radiation. The frequency range of that radiation depends on the central object's mass. Accretion discs of young stars and protostars radiate in the infrared; those around neutron stars and black holes in the X-ray part of the spectrum. The study of oscillation modes in accretion discs is referred to as "diskoseismology".
Accretion discs are a ubiquitous phenomenon in astrophysics; active galactic nuclei, protoplanetary discs, and gamma ray bursts all involve accretion discs. These discs very often give rise to astrophysical jets coming from the vicinity of the central object. Jets are an efficient way for the star-disc system to shed angular momentum without losing too much mass.
The most spectacular accretion discs found in nature are those of active galactic nuclei and of quasars, which are believed to be massive black holes at the center of galaxies. As matter follows the tendex line into a black hole, the intense gravitational gradient gives rise to intense frictional heating; the accretion disc of a black hole is hot enough to emit X-rays just outside of the event horizon. The large luminosity of quasars is believed to be a result of gas being accreted by supermassive black holes . Elliptical accretion discs formed at tidal disruption of stars can be typical in galactic nuclei and quasars . Accretion process can convert about 10 percent to over 40 percent of the mass of an object into energy as compared to around 0.7 percent for nuclear fusion processes.
Wiz Science™ is "the" learning channel for children and all ages.
SUBSCRIBE TODAY
Disclaimer: This video is for your information only. The author or publisher does not guarantee the accuracy of the content presented in this video. USE AT YOUR OWN RISK.
Background Music:
"The Place Inside" by Silent Partner (royalty-free) from YouTube Audio Library.
This video uses material/images from https://en.wikipedia.org/wiki/Accretion+disc, which is released under Creative Commons Attribution-Share-Alike License 3.0 http://creativecommons.org/licenses/by-sa/3.0/ . This video is licensed under Creative Commons Attribution-Share-Alike License 3.0 http://creativecommons.org/licenses/by-sa/3.0/ . To reuse/adapt the content in your own work, you must comply with the license terms.
Wiz Science™ is "the" learning channel for children and all ages.
SUBSCRIBE TODAY
Disclaimer: This video is for your information only. The author or publisher does not guarantee the accuracy of the content presented in this video. USE AT YOUR OWN RISK.
Background Music:
"The Place Inside" by Silent Partner (royalty-free) from YouTube Audio Library.
This video uses material/images from https://en.wikipedia.org/wiki/Accretion+disc, which is released under Creative Commons Attribution-Share-Alike License 3.0 http://creativecommons.org/licenses/by-sa/3.0/ . This video is licensed under Creative Commons Attribution-Share-Alike License 3.0 http://creativecommons.org/licenses/by-sa/3.0/ . To reuse/adapt the content in your own work, you must comply with the license terms.
- published: 10 Sep 2015
- views: 778
4:58
Starbound Soundtrack - Accretion Disc
- Order: Reorder
- Duration: 4:58
- Updated: 08 Dec 2013
- views: 39347
Full Playlist of Starbound Soundtrack:
https://www.youtube.com/playlist?list=PL7DXTXnlwEuN4eTTyMIOZJfoZN4IQgx8z&feature;=mh_lolz
Full Playlist of Starbound Soundtrack:
https://www.youtube.com/playlist?list=PL7DXTXnlwEuN4eTTyMIOZJfoZN4IQgx8z&feature;=mh_lolz
https://wn.com/Starbound_Soundtrack_Accretion_Disc
Full Playlist of Starbound Soundtrack:
https://www.youtube.com/playlist?list=PL7DXTXnlwEuN4eTTyMIOZJfoZN4IQgx8z&feature;=mh_lolz
- published: 08 Dec 2013
- views: 39347
0:27
Quasar With Accretion Disk and Jet
- Order: Reorder
- Duration: 0:27
- Updated: 25 Jun 2010
- views: 8073
Using two of the world's largest telescopes, an international team of astronomers have found evidence of a collision between galaxies driving intense activity i...
Using two of the world's largest telescopes, an international team of astronomers have found evidence of a collision between galaxies driving intense activity in a highly luminous quasar. The scientists, led by Montserrat Villar Martin of the Instituto de Astrofisica de Andalucía-CSIC in Spain, used the Very Large Telescope (VLT) in Chile and the Gran Telescopio Canarias (GTC) on La Palma in the Canary Islands, to study activity from the quasar SDSS J0123+00. They publish their work in a paper in the journal Monthly Notices of the Royal Astronomical Society.
Several types of galaxies, known as active galaxies, emit enormous amounts of energy from their central region or nucleus, with the most luminous objects known as quasars. Most scientists argue that quasars contain a central black hole, with a mass of at least several million Suns.
The intense gravitational field created by the black hole drags material inexorably inwards. Before falling in, this material settles in an accretion disk where it becomes very hot and emits large amounts of energy responsible for most of the brightness of the quasar. Around the central quasar 'engine' is a torus (thick ring) opaque to the visible light emitted by the accretion disk. From a terrestrial perspective, if the torus is face-on then the radiation from the disk can be seen and the system is designated type 1, whereas in type 2 quasars the torus is edge-on and the radiation is concealed.
source: http://www.iaa.es/~rosa/AYA2010/AYA2010/Novedades/Entradas/2010/6/23_Galaxy_encounter_fire_up_quasar.html
https://wn.com/Quasar_With_Accretion_Disk_And_Jet
Using two of the world's largest telescopes, an international team of astronomers have found evidence of a collision between galaxies driving intense activity in a highly luminous quasar. The scientists, led by Montserrat Villar Martin of the Instituto de Astrofisica de Andalucía-CSIC in Spain, used the Very Large Telescope (VLT) in Chile and the Gran Telescopio Canarias (GTC) on La Palma in the Canary Islands, to study activity from the quasar SDSS J0123+00. They publish their work in a paper in the journal Monthly Notices of the Royal Astronomical Society.
Several types of galaxies, known as active galaxies, emit enormous amounts of energy from their central region or nucleus, with the most luminous objects known as quasars. Most scientists argue that quasars contain a central black hole, with a mass of at least several million Suns.
The intense gravitational field created by the black hole drags material inexorably inwards. Before falling in, this material settles in an accretion disk where it becomes very hot and emits large amounts of energy responsible for most of the brightness of the quasar. Around the central quasar 'engine' is a torus (thick ring) opaque to the visible light emitted by the accretion disk. From a terrestrial perspective, if the torus is face-on then the radiation from the disk can be seen and the system is designated type 1, whereas in type 2 quasars the torus is edge-on and the radiation is concealed.
source: http://www.iaa.es/~rosa/AYA2010/AYA2010/Novedades/Entradas/2010/6/23_Galaxy_encounter_fire_up_quasar.html
- published: 25 Jun 2010
- views: 8073
0:21
Accretion disk - planetary formation
- Order: Reorder
- Duration: 0:21
- Updated: 09 Aug 2014
- views: 1530
- published: 09 Aug 2014
- views: 1530
0:22
Black Hole Accretion Disk
- Order: Reorder
- Duration: 0:22
- Updated: 29 Jun 2017
- views: 323
In this video, the camera rotates around a spinning (Kerr) black hole that is surrounded by an accretion disk (a vortex of matter attracted by the black hole th...
In this video, the camera rotates around a spinning (Kerr) black hole that is surrounded by an accretion disk (a vortex of matter attracted by the black hole that orbits it and eventually falls in).
The accreting matter emits synchrotron radiation at various frequencies; in the video, we see radiation emitted at 230 GHz.
If you have any questions, feel free to ask!
Credits:
T. Bronzwaer, J. Davelaar, Z. Younsi 2017.
The video was made using the general relativistic radiative transfer code RAPTOR (see [1]). The video uses a GRMHD data slice generated by HARM (see [2] and [3]).
[1] Bronzwaer, T., Davelaar, J., et al. 2017 in prep.
[2] Gammie, C. F., McKinney, J. C., & Toth, G., 2003, Astrophysical Journal, 589, 444.
[3] Noble, S. C., Gammie, C. F., McKinney, J. C., & Del Zanna, L., 2006, Astrophysical Journal, 641, 626.
https://wn.com/Black_Hole_Accretion_Disk
In this video, the camera rotates around a spinning (Kerr) black hole that is surrounded by an accretion disk (a vortex of matter attracted by the black hole that orbits it and eventually falls in).
The accreting matter emits synchrotron radiation at various frequencies; in the video, we see radiation emitted at 230 GHz.
If you have any questions, feel free to ask!
Credits:
T. Bronzwaer, J. Davelaar, Z. Younsi 2017.
The video was made using the general relativistic radiative transfer code RAPTOR (see [1]). The video uses a GRMHD data slice generated by HARM (see [2] and [3]).
[1] Bronzwaer, T., Davelaar, J., et al. 2017 in prep.
[2] Gammie, C. F., McKinney, J. C., & Toth, G., 2003, Astrophysical Journal, 589, 444.
[3] Noble, S. C., Gammie, C. F., McKinney, J. C., & Del Zanna, L., 2006, Astrophysical Journal, 641, 626.
- published: 29 Jun 2017
- views: 323
0:51
Accretion DIsk SImulation
- Order: Reorder
- Duration: 0:51
- Updated: 29 May 2014
- views: 4378
Accretion DIsk SImulation
(Original credit : wikipedia)
(BGM info : The Rock Diamond - I'll Protect You)
Accretion DIsk SImulation
(Original credit : wikipedia)
(BGM info : The Rock Diamond - I'll Protect You)
https://wn.com/Accretion_Disk_Simulation
7:05
Vortex Technologies Accretion Disk Demonstration
- Order: Reorder
- Duration: 7:05
- Updated: 18 Apr 2015
- views: 6741
Watch and see what happens when two electromagnetic vortex fields collide!
Watch and see what happens when two electromagnetic vortex fields collide!
https://wn.com/Vortex_Technologies_Accretion_Disk_Demonstration
Watch and see what happens when two electromagnetic vortex fields collide!
- published: 18 Apr 2015
- views: 6741
2:01
Evolution of magnetic field in a thick accretion disk
- Order: Reorder
- Duration: 2:01
- Updated: 10 Mar 2015
- views: 55
- published: 10 Mar 2015
- views: 55
7:24
Creating a Black Hole Accretion Disk Using Universe Sandbox²
Hello and welcome to What Da Math!
In this video, we will use the new effects from Univers...
published: 27 Nov 2016
Creating a Black Hole Accretion Disk Using Universe Sandbox²
Creating a Black Hole Accretion Disk Using Universe Sandbox²
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- published: 27 Nov 2016
- views: 11634
Hello and welcome to What Da Math!
In this video, we will use the new effects from Universe Sandbox 2 to create an accretion disk around a black hole.
Patreon page:
https://www.patreon.com/user?u=2318196&ty;=h
Enjoy and please subscribe.
Other videos here: https://www.youtube.com/playlist?list=PL9hNFus3sjE7jgrGJYkZeTpR7lnyVAk-x
Twitter: https://twitter.com/WhatDaMath
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Twitch: http://www.twitch.tv/whatdamath
1:32:35
Astrophysics of accretion disks - Charles Gammie
Computational Plasma Astrophysics: July 25, 2016
Prospects in Theoretical Physics is an i...
published: 25 Jul 2016
Astrophysics of accretion disks - Charles Gammie
Astrophysics of accretion disks - Charles Gammie
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- published: 25 Jul 2016
- views: 2340
Computational Plasma Astrophysics: July 25, 2016
Prospects in Theoretical Physics is an intensive two-week summer program typically designed for graduate students and postdoctoral scholars considering a career in theoretical physics (for 2014 only the program was one week in length). First held by the School of Natural Sciences at the Institute for Advanced Study in the summer of 2002, the PiTP program is designed to provide lectures and informal sessions on the latest advances and open questions in various areas of theoretical physics.
One of the goals of the program is to help the physics community train the next generation of scholars in theoretical physics. A special effort is made to reach out to women and minorities, as well as to graduate students in small universities who typically do not have the same opportunities and access to leaders in the field as graduate students in large research institutions.
Prospects in Theoretical Physics builds on the strong relationship of the research groups at the Institute and Princeton University, and many faculty members from the physics departments at both institutions are actively involved in the program together with scientists from neighboring institutions.
More videos on http://video.ias.edu
4:14
What is ACCRETION DISK? What does ACCRETION DISK mean? ACCRETION DISK meaning
What is ACCRETION DISK? What does ACCRETION DISK mean? ACCRETION DISK meaning - ACCRETION ...
published: 01 Oct 2016
What is ACCRETION DISK? What does ACCRETION DISK mean? ACCRETION DISK meaning
What is ACCRETION DISK? What does ACCRETION DISK mean? ACCRETION DISK meaning
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- published: 01 Oct 2016
- views: 1569
What is ACCRETION DISK? What does ACCRETION DISK mean? ACCRETION DISK meaning - ACCRETION DISK definition - ACCRETION DISK explanation.
An accretion disk is a structure (often a circumstellar disk) formed by diffused material in orbital motion around a massive central body. The central body is typically a star. Gravity causes material in the disk to spiral inward towards the central body. Gravitational and frictional forces compress and raise the temperature of the material causing the emission of electromagnetic radiation. The frequency range of that radiation depends on the central object's mass. Accretion disks of young stars and protostars radiate in the infrared; those around neutron stars and black holes in the X-ray part of the spectrum. The study of oscillation modes in accretion disks is referred to as diskoseismology.
Accretion disks are a ubiquitous phenomenon in astrophysics; active galactic nuclei, protoplanetary disks, and gamma ray bursts all involve accretion disks. These disks very often give rise to astrophysical jets coming from the vicinity of the central object. Jets are an efficient way for the star-disk system to shed angular momentum without losing too much mass.
The most spectacular accretion disks found in nature are those of active galactic nuclei and of quasars, which are believed to be massive black holes at the center of galaxies. As matter enters the accretion disc, it follows a trajectory called a tendex line, which describes an inward spiral. This is because particles rub and bounce against each other in a turbulent flow, causing frictional heating which radiates energy away, reducing the particles' angular momentum, allowing the particle to drift inwards, driving the inward spiral. The loss of angular momentum manifests as a reduction in velocity; at a slower velocity, the particle wants to adopt a lower orbit. As the particle falls to this lower orbit, a portion of its gravitational potential energy is converted to increased velocity and the particle gains speed. Thus, the particle has lost energy even though it is now travelling faster than before; however, it has lost angular momentum. As a particle orbits closer and closer, its velocity increases, as velocity increases frictional heating increases as more and more of the particle's potential energy (relative to the black hole) is radiated away; the accretion disk of a black hole is hot enough to emit X-rays just outside the event horizon. The large luminosity of quasars is believed to be a result of gas being accreted by supermassive black holes (Lynden-Bell, 1969). Elliptical accretion disks formed at tidal disruption of stars can be typical in galactic nuclei and quasars (Gurzadyan and Ozernoy, 1979). Accretion process can convert about 10 percent to over 40 percent of the mass of an object into energy as compared to around 0.7 percent for nuclear fusion processes.
In close binary systems the more massive primary component evolves faster and has already become a white dwarf, a neutron star, or a black hole, when the less massive companion reaches the giant state and exceeds its Roche lobe. A gas flow then develops from the companion star to the primary. Angular momentum conservation prevents a straight flow from one star to the other and an accretion disk forms instead.
Accretion disks surrounding T Tauri stars or Herbig stars are called protoplanetary disks because they are thought to be the progenitors of planetary systems. The accreted gas in this case comes from the molecular cloud out of which the star has formed rather than a companion star.
5:07
How Black Holes Would Look To Someone Beside One!
Interstellar is the first Hollywood movie to attempt depicting a black hole as it would ac...
published: 28 Oct 2015
How Black Holes Would Look To Someone Beside One!
How Black Holes Would Look To Someone Beside One!
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- published: 28 Oct 2015
- views: 26305
Interstellar is the first Hollywood movie to attempt depicting a black hole as it would actually be seen by somebody nearby.
Get more Science at The Speaker Science: http://thespeaker.co/science/
For this, our team at Double Negative Visual Effects, in collaboration with physicist Kip Thorne, developed a code called Double Negative Gravitational Renderer (DNGR) to solve the equations for ray-bundle (light-beam) propagation through the curved spacetime of a spinning (Kerr) black hole, and to render IMAX-quality, rapidly changing images.
Our ray-bundle techniques were crucial for achieving IMAX-quality smoothness without flickering; and they differ from physicists' image-generation techniques (which generally rely on individual light rays rather than ray bundles), and also differ from techniques previously used in the film industry's CGI community.
This paper has four purposes: (i) to describe DNGR for physicists and CGI practitioners, who may find interesting and useful some of our unconventional techniques. (ii)
To present the equations we use, when the camera is in arbitrary motion at an arbitrary location near a Kerr black hole, for mapping light sources to camera images via elliptical ray bundles. (iii)
To describe new insights, from DNGR, into gravitational lensing when the camera is near the spinning black hole, rather than far away as in almost all prior studies; we focus on the shapes, sizes and influence of caustics and critical curves, the creation and annihilation of stellar images, the pattern of multiple images, and the influence of almost-trapped light rays, and we find similar results to the more familiar case of a camera far from the hole. (iv)
To describe how the images of the black hole Gargantua and its accretion disk, in the movie Interstellar, were generated with DNGR—including, especially, the influences of (a) colour changes due to doppler and gravitational frequency shifts, (b) intensity changes due to the frequency shifts, (c) simulated camera lens flare, and (d) decisions that the film makers made about these influences and about the Gargantua's spin, with the goal of producing images understandable for a mass audience. There are no new astrophysical insights in this accretion-disk section of the paper, but disk novices may find it pedagogically interesting, and movie buffs may find its discussions of Interstellar interesting.
Gravitational lensing by spinning black holes in astrophysics, and in the movie Interstellar.
Oliver James et al (2015), Classical and Quantum Gravity http://dx.doi.org/10.1088/0264-9381/3...
0:31
Flaring Black Hole Accretion Disk in the Binary System V404 Cygni
On June 15, NASA's Swift caught the onset of a rare X-ray outburst from a stellar-mass bla...
published: 30 Jun 2015
Flaring Black Hole Accretion Disk in the Binary System V404 Cygni
Flaring Black Hole Accretion Disk in the Binary System V404 Cygni
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- published: 30 Jun 2015
- views: 278949
On June 15, NASA's Swift caught the onset of a rare X-ray outburst from a stellar-mass black hole in the binary system V404 Cygni. Astronomers around the world are watching the event. In this system, a stream of gas from a star much like the sun flows toward a 10 solar mass black hole. Instead of spiraling toward the black hole, the gas accumulates in an accretion disk around it. Every couple of decades, the disk switches into a state that sends the gas rushing inward, starting a new outburst.
Download this video in HD formats from NASA Goddard's Scientific Visualization Studio
http://svs.gsfc.nasa.gov/cgi-bin/details.cgi?aid=11110
12:57
Forming an Accretion Disk around a Black Hole
Welcome to another experiment in Universe Sandbox 2 Let's play series.
Today we'll be tes...
published: 10 Apr 2018
Forming an Accretion Disk around a Black Hole
Forming an Accretion Disk around a Black Hole
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- published: 10 Apr 2018
- views: 478
Welcome to another experiment in Universe Sandbox 2 Let's play series.
Today we'll be testing a user made suggestion asking if we can form an accretion disk in Universe Sandbox 2, let's find out!
Universe Sandbox 2 is a space sandbox that is still a work in progress, and is an awesome game and educational tool. But, keep in mind the physics and results depicted in this game are to be taken with a grain a salt, the game tries to, but does not always accurately reproduce the expectations of our current knowledge of physics, the game is still an early access alpha and is still being worked on!
A lot of the ideas in this series are suggestions by viewers and aren't always intended to be "educational," so take the results of this test with a grain of salt!
Buy and Support Universe Sandbox 2 on Steam
http://store.steampowered.com/app/230290/
You read descriptions! ツ
1:21
Accretion Disk around Black Hole
The disk is based on a non-relativistic Smoothed-Particle-Hydrodynamics (SPH) simulation.
...
published: 27 Oct 2014
Accretion Disk around Black Hole
Accretion Disk around Black Hole
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- Report rights infringement
- published: 27 Oct 2014
- views: 15521
The disk is based on a non-relativistic Smoothed-Particle-Hydrodynamics (SPH) simulation.
The apparent distortion of the disk is due to the bending of light within the Schwarzschild spacetime. Besides the primary image of the disk, there are also higher order images (lower ring and upper thin ring) visible. The lower ring shows the rear bottom side of the disk. The color encodes the apparent temperature where blue is hot and red is cold. The left part of the disk approaches the observer and, thus, appears hotter due to the Doppler effect. You also see some bright spots which smear out already after one revolution around the black hole.
2:20
Accretion disc - Video Learning - WizScience.com
An "accretion disk" is a structure formed by diffused material in orbital motion around ...
published: 10 Sep 2015
Accretion disc - Video Learning - WizScience.com
Accretion disc - Video Learning - WizScience.com
- Show More
- Report rights infringement
- published: 10 Sep 2015
- views: 778
An "accretion disk" is a structure formed by diffused material in orbital motion around a massive central body. The central body is typically a star. Gravity causes material in the disc to spiral inward towards the central body. Gravitational and frictional forces compress and raise the temperature of the material causing the emission of electromagnetic radiation. The frequency range of that radiation depends on the central object's mass. Accretion discs of young stars and protostars radiate in the infrared; those around neutron stars and black holes in the X-ray part of the spectrum. The study of oscillation modes in accretion discs is referred to as "diskoseismology".
Accretion discs are a ubiquitous phenomenon in astrophysics; active galactic nuclei, protoplanetary discs, and gamma ray bursts all involve accretion discs. These discs very often give rise to astrophysical jets coming from the vicinity of the central object. Jets are an efficient way for the star-disc system to shed angular momentum without losing too much mass.
The most spectacular accretion discs found in nature are those of active galactic nuclei and of quasars, which are believed to be massive black holes at the center of galaxies. As matter follows the tendex line into a black hole, the intense gravitational gradient gives rise to intense frictional heating; the accretion disc of a black hole is hot enough to emit X-rays just outside of the event horizon. The large luminosity of quasars is believed to be a result of gas being accreted by supermassive black holes . Elliptical accretion discs formed at tidal disruption of stars can be typical in galactic nuclei and quasars . Accretion process can convert about 10 percent to over 40 percent of the mass of an object into energy as compared to around 0.7 percent for nuclear fusion processes.
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Background Music:
"The Place Inside" by Silent Partner (royalty-free) from YouTube Audio Library.
This video uses material/images from https://en.wikipedia.org/wiki/Accretion+disc, which is released under Creative Commons Attribution-Share-Alike License 3.0 http://creativecommons.org/licenses/by-sa/3.0/ . This video is licensed under Creative Commons Attribution-Share-Alike License 3.0 http://creativecommons.org/licenses/by-sa/3.0/ . To reuse/adapt the content in your own work, you must comply with the license terms.
Wiz Science™ is "the" learning channel for children and all ages.
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Disclaimer: This video is for your information only. The author or publisher does not guarantee the accuracy of the content presented in this video. USE AT YOUR OWN RISK.
Background Music:
"The Place Inside" by Silent Partner (royalty-free) from YouTube Audio Library.
This video uses material/images from https://en.wikipedia.org/wiki/Accretion+disc, which is released under Creative Commons Attribution-Share-Alike License 3.0 http://creativecommons.org/licenses/by-sa/3.0/ . This video is licensed under Creative Commons Attribution-Share-Alike License 3.0 http://creativecommons.org/licenses/by-sa/3.0/ . To reuse/adapt the content in your own work, you must comply with the license terms.
4:58
Starbound Soundtrack - Accretion Disc
Full Playlist of Starbound Soundtrack:
https://www.youtube.com/playlist?list=PL7DXTXnlwEu...
published: 08 Dec 2013
Starbound Soundtrack - Accretion Disc
Starbound Soundtrack - Accretion Disc
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- published: 08 Dec 2013
- views: 39347
Full Playlist of Starbound Soundtrack:
https://www.youtube.com/playlist?list=PL7DXTXnlwEuN4eTTyMIOZJfoZN4IQgx8z&feature;=mh_lolz
0:27
Quasar With Accretion Disk and Jet
Using two of the world's largest telescopes, an international team of astronomers have fou...
published: 25 Jun 2010
Quasar With Accretion Disk and Jet
Quasar With Accretion Disk and Jet
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- published: 25 Jun 2010
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Using two of the world's largest telescopes, an international team of astronomers have found evidence of a collision between galaxies driving intense activity in a highly luminous quasar. The scientists, led by Montserrat Villar Martin of the Instituto de Astrofisica de Andalucía-CSIC in Spain, used the Very Large Telescope (VLT) in Chile and the Gran Telescopio Canarias (GTC) on La Palma in the Canary Islands, to study activity from the quasar SDSS J0123+00. They publish their work in a paper in the journal Monthly Notices of the Royal Astronomical Society.
Several types of galaxies, known as active galaxies, emit enormous amounts of energy from their central region or nucleus, with the most luminous objects known as quasars. Most scientists argue that quasars contain a central black hole, with a mass of at least several million Suns.
The intense gravitational field created by the black hole drags material inexorably inwards. Before falling in, this material settles in an accretion disk where it becomes very hot and emits large amounts of energy responsible for most of the brightness of the quasar. Around the central quasar 'engine' is a torus (thick ring) opaque to the visible light emitted by the accretion disk. From a terrestrial perspective, if the torus is face-on then the radiation from the disk can be seen and the system is designated type 1, whereas in type 2 quasars the torus is edge-on and the radiation is concealed.
source: http://www.iaa.es/~rosa/AYA2010/AYA2010/Novedades/Entradas/2010/6/23_Galaxy_encounter_fire_up_quasar.html
0:21
Accretion disk - planetary formation
published: 09 Aug 2014
Accretion disk - planetary formation
Accretion disk - planetary formation
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- published: 09 Aug 2014
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0:22
Black Hole Accretion Disk
In this video, the camera rotates around a spinning (Kerr) black hole that is surrounded b...
published: 29 Jun 2017
Black Hole Accretion Disk
Black Hole Accretion Disk
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- published: 29 Jun 2017
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In this video, the camera rotates around a spinning (Kerr) black hole that is surrounded by an accretion disk (a vortex of matter attracted by the black hole that orbits it and eventually falls in).
The accreting matter emits synchrotron radiation at various frequencies; in the video, we see radiation emitted at 230 GHz.
If you have any questions, feel free to ask!
Credits:
T. Bronzwaer, J. Davelaar, Z. Younsi 2017.
The video was made using the general relativistic radiative transfer code RAPTOR (see [1]). The video uses a GRMHD data slice generated by HARM (see [2] and [3]).
[1] Bronzwaer, T., Davelaar, J., et al. 2017 in prep.
[2] Gammie, C. F., McKinney, J. C., & Toth, G., 2003, Astrophysical Journal, 589, 444.
[3] Noble, S. C., Gammie, C. F., McKinney, J. C., & Del Zanna, L., 2006, Astrophysical Journal, 641, 626.
0:51
Accretion DIsk SImulation
Accretion DIsk SImulation
(Original credit : wikipedia)
(BGM info : The Rock Diamond - I'l...
published: 29 May 2014
Accretion DIsk SImulation
7:05
Vortex Technologies Accretion Disk Demonstration
Watch and see what happens when two electromagnetic vortex fields collide!
published: 18 Apr 2015
Vortex Technologies Accretion Disk Demonstration
Vortex Technologies Accretion Disk Demonstration
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- published: 18 Apr 2015
- views: 6741
Watch and see what happens when two electromagnetic vortex fields collide!
Accretion disk
An accretion disk is a structure (often a circumstellar disk) formed by diffused material in orbital motion around a massive central body. The central body is typically a star. Gravity causes material in the disk to spiral inward towards the central body. Gravitational and frictional forces compress and raise the temperature of the material causing the emission of electromagnetic radiation. The frequency range of that radiation depends on the central object's mass. Accretion disks of young stars and protostars radiate in the infrared; those around neutron stars and black holes in the X-ray part of the spectrum. The study of oscillation modes in accretion disks is referred to as diskoseismology.
Manifestations
Accretion disks are a ubiquitous phenomenon in astrophysics; active galactic nuclei, protoplanetary disks, and gamma ray bursts all involve accretion disks. These disks very often give rise to astrophysical jets coming from the vicinity of the central object. Jets are an efficient way for the star-disk system to shed angular momentum without losing too much mass.
This page contains text from Wikipedia, the Free Encyclopedia -
https://wn.com/Accretion_disk
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