Ebony Hole

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Ebony Hole
August 25, 2022, 12:56 AM · 3 min read
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NASA shared a video this week that gives us a glimpse into what a black hole sounds like — and it's terrifying.
NASA's Exoplanets team, a group of researchers that search for planets and life outside of our solar system, reposted a video NASA originally published in May, sharing audio of sound waves it had previously identified, but were inaudible — until now.
The Exoplanets team shared the ominous 34-second clip on Twitter and explained why there's a misconception there's no sound in space.
The misconception that there is no sound in space originates because most space is a ~vacuum, providing no way for sound waves to travel. A galaxy cluster has so much gas that we've picked up actual sound. Here it's amplified, and mixed with other data, to hear a black hole! pic.twitter.com/RobcZs7F9e
— NASA Exoplanets (@NASAExoplanets) August 21, 2022
"The misconception that there is no sound in space originates because most space is a ~vacuum, providing no way for sound waves to travel," the NASA team said. "A galaxy cluster has so much gas that we’ve picked up actual sound. Here it’s amplified, and mixed with other data, to hear a black hole!"
TODAY hosts Hoda Kotb, Craig Melvin, Al Roker and Tom Llamas reacted on Tuesday to the video , which comes from a black hole 250 million light years away from Earth.
Hoda's jaw dropped while listening to the clip, while Al explained how scientists were able to create the audio.
"Well, it picked up the sound because of the amount of gas that a galaxy cluster has," Al said while laughing.
"Don't, Al, I'm begging you," Hoda responded, trying to hold in her giggles.
"So, so, so ... there's that," Al continued with a smile.
NASA says the video features a "sonification" of the black hole at the center of the Perseus galaxy cluster, which has grappled astronomers after they previously discovered pressure waves in the black hole could be translated into one, inaudible note.
The issue with the note is it is about 57 octaves below middle C, meaning humans can't hear it, NASA says. But researchers produced a new sonification, or a translation of astronomical data into sound, for Black Hole Week earlier this year.
The video went viral this week after the NASA Exoplanets team reshared the clip, leading many on the internet to fear ever hearing the noise in real life.
"According to NASA, a black hole sounds like billions of souls wailing in anguish from the depths of hell," one tweet r ead. "Neat! I didn’t plan on sleeping anytime in the foreseeable future, anyway..."
According to NASA, a black hole sounds like billions of souls wailing in anguish from the depths of hell. Neat! I didn't plan on sleeping anytime in the foreseeable future, anyway... https://t.co/iROsVdn4g1
— Bryan "The FBI has not seized my passport" Schott (@SchottHappens) August 22, 2022
"Turns out the sound of black hole is 100 times more frightening than you could have imagined," another tweet read.
"Hey @NASAExoplanets it’s not #halloween yet we don’t appreciate this early delivery of nightmare fuel," j oked another.
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From Wikipedia, the free encyclopedia
Astronomical object that has a very strong gravity such that nothing can escape





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Λ

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{\displaystyle G_{\mu \nu }+\Lambda g_{\mu \nu }={\kappa }T_{\mu \nu }}


Simple illustration of a non-spinning black hole
Artistic depiction of a black hole and its features
Far away from the black hole, a particle can move in any direction, as illustrated by the set of arrows. It is restricted only by the speed of light.
Closer to the black hole, spacetime starts to deform. There are more paths going towards the black hole than paths moving away. [Note 3]
Inside of the event horizon, all paths bring the particle closer to the centre of the black hole. It is no longer possible for the particle to escape.
The formula for the Bekenstein–Hawking entropy ( S ) of a black hole, which depends on the area of the black hole ( A ). The constants are the speed of light ( c ), the Boltzmann constant ( k ), Newton's constant ( G ), and the reduced Planck constant ( ħ ). In Planck units, this reduces to S = A / 4 .

^ The value of cJ/GM 2 can exceed 1 for objects other than black holes. The largest value known for a neutron star is ≤ 0.4, and commonly used equations of state would limit that value to < 0.7. [76]

^ The (outer) event horizon radius scales as:



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{\displaystyle M+{\sqrt {M^{2}-{(J/M)}^{2}-Q^{2}}}.}



^ The set of possible paths, or more accurately the future light cone containing all possible world lines (in this diagram the light cone is represented by the V-shaped region bounded by arrows representing light ray world lines), is tilted in this way in Eddington–Finkelstein coordinates (the diagram is a "cartoon" version of an Eddington–Finkelstein coordinate diagram), but in other coordinates the light cones are not tilted in this way, for example in Schwarzschild coordinates they simply narrow without tilting as one approaches the event horizon, and in Kruskal–Szekeres coordinates the light cones do not change shape or orientation at all. [79]

^ This is true only for four-dimensional spacetimes. In higher dimensions more complicated horizon topologies like a black ring are possible. [91] [92]

^ In particular, he assumed that all matter satisfies the weak energy condition .



^ Oldham, L. J.; Auger, M. W. (March 2016). "Galaxy structure from multiple tracers – II. M87 from parsec to megaparsec scales". Monthly Notices of the Royal Astronomical Society . 457 (1): 421–439. arXiv : 1601.01323 . Bibcode : 2016MNRAS.457..421O . doi : 10.1093/mnras/stv2982 . S2CID 119166670 .

^ Wald 1984 , pp. 299–300

^ Jump up to: a b Wald, R. M. (1997). "Gravitational Collapse and Cosmic Censorship". In Iyer, B. R.; Bhawal, B. (eds.). Black Holes, Gravitational Radiation and the Universe . Dordrecht: Springer. pp. 69–86. arXiv : gr-qc/9710068 . doi : 10.1007/978-94-017-0934-7 . ISBN 978-9401709347 .

^ Overbye, Dennis (8 June 2015). "Black Hole Hunters" . NASA . Archived from the original on 9 June 2015 . Retrieved 8 June 2015 .

^ Hamilton, A. "Journey into a Schwarzschild black hole" . jila.colorado.edu . Archived from the original on 3 September 2019 . Retrieved 28 June 2020 .

^ Schutz, Bernard F. (2003). Gravity from the ground up . Cambridge University Press. p. 110. ISBN 978-0-521-45506-0 . Archived from the original on 2 December 2016.

^ Davies, P. C. W. (1978). "Thermodynamics of Black Holes" (PDF) . Reports on Progress in Physics . 41 (8): 1313–1355. Bibcode : 1978RPPh...41.1313D . doi : 10.1088/0034-4885/41/8/004 . S2CID 250916407 . Archived from the original (PDF) on 10 May 2013.

^ Jump up to: a b c Montgomery, Colin; Orchiston, Wayne; Whittingham, Ian (2009). "Michell, Laplace and the origin of the black hole concept". Journal of Astronomical History and Heritage . 12 (2): 90–96. Bibcode : 2009JAHH...12...90M .

^ Webster, B. Louise; Murdin, Paul (1972), "Cygnus X-1—a Spectroscopic Binary with a Heavy Companion?", Nature , 235 (5332): 37–38, Bibcode : 1972Natur.235...37W , doi : 10.1038/235037a0 , S2CID 4195462

^ Bolton, C. T. (1972), "Identification of Cygnus X-1 with HDE 226868", Nature , 235 (5336): 271–273, Bibcode : 1972Natur.235..271B , doi : 10.1038/235271b0 , S2CID 4222070

^ Clery D (2020). "Black holes caught in the act of swallowing stars". Science . 367 (6477): 495. Bibcode : 2020Sci...367..495C . doi : 10.1126/science.367.6477.495 . PMID 32001633 . S2CID 210984462 .

^ Jump up to: a b c d Abbott, B.P.; et al. (2016). "Observation of Gravitational Waves from a Binary Black Hole Merger". Phys. Rev. Lett. 116 (6): 061102. arXiv : 1602.03837 . Bibcode : 2016PhRvL.116f1102A . doi : 10.1103/PhysRevLett.116.061102 . PMID 26918975 . S2CID 124959784 .

^ Event Horizon Telescope, The (2019). "First M87 Event Horizon Telescope Results. I. The Shadow of the Supermassive Black Hole". The Astrophysical Journal . 875 (1): L1. arXiv : 1906.11238 . Bibcode : 2019ApJ...875L...1E . doi : 10.3847/2041-8213/ab0ec7 . S2CID 145906806 .

^ Bouman, Katherine L. ; Johnson, Michael D.; Zoran, Daniel; Fish, Vincent L.; Doeleman, Sheperd S.; Freeman, William T. (2016). "Computational Imaging for VLBI Image Reconstruction". 2016 IEEE Conference on Computer Vision and Pattern Recognition (CVPR) . pp. 913–922. arXiv : 1512.01413 . doi : 10.1109/CVPR.2016.105 . hdl : 1721.1/103077 . ISBN 978-1-4673-8851-1 . S2CID 9085016 .

^ Gardiner, Aidan (12 April 2018). "When a Black Hole Finally Reveals Itself, It Helps to Have Our Very Own Cosmic Reporter – Astronomers announced Wednesday that they had captured the first image of a black hole. The Times's Dennis Overbye answers readers' questions" . The New York Times . Archived from the original on 1 January 2022 . Retrieved 15 April 2019 .

^ "ESO Instrument Finds Closest Black Hole to Earth" . European Southern Observatory . 6 May 2020. Archived from the original on 6 May 2020 . Retrieved 2 April 2021 .

^ Riazuelo, Alain (2019). "Seeing relativity -- I. Ray tracing in a Schwarzschild metric to explore the maximal analytic extension of the metric and making a proper rendering of the stars". International Journal of Modern Physics D . 28 (2): 1950042. arXiv : 1511.06025 . Bibcode : 2019IJMPD..2850042R . doi : 10.1142/S0218271819500421 . S2CID 54548877 .

^ Schaffer, Simon (1979). "John Michell and black holes" . Journal for the History of Astronomy . 10 : 42–43. Bibcode : 1979JHA....10...42S . doi : 10.1177/002182867901000104 . S2CID 123958527 . Archived from the original on 22 May 2020 . Retrieved 27 August 2021 .

^ Michell, J. (1784). "On the Means of Discovering the Distance, Magnitude, &c. of the Fixed Stars, in Consequence of the Diminution of the Velocity of Their Light, in Case Such a Diminution Should be Found to Take Place in any of Them, and Such Other Data Should be Procured from Observations, as Would be Farther Necessary for That Purpose" . Philosophical Transactions of the Royal Society . 74 : 35–57. Bibcode : 1784RSPT...74...35M . doi : 10.1098/rstl.1784.0008 . JSTOR 106576 .

^ Jump up to: a b Thorne 1994 , pp. 123–124

^ Slayter, Elizabeth M.; Slayter, Henry S. (1992). Light and Electron Microscopy . Cambridge University Press. ISBN 978-0-521-33948-3 . Archived from the original on 30 November 2017.

^ Crass, Institute of Astronomy – Design by D.R. Wilkins and S.J. "Light escaping from black holes" . www.ast.cam.ac.uk . Archived from the original on 6 July 2019 . Retrieved 10 March 2018 .

^ Levy, Adam (11 January 2021). "How black holes morphed from theory to reality" . Knowable Magazine . doi : 10.1146/knowable-010921-1 . Retrieved 25 March 2022 .

^ Jump up to: a b Schwarzschild, K. (1916). "Über das Gravitationsfeld eines Massenpunktes nach der Einsteinschen Theorie" . Sitzungsberichte der Königlich Preussischen Akademie der Wissenschaften . 7 : 189–196. Bibcode : 1916SPAW.......189S .

Translation: Antoci, S.; Loinger, A. (1999). "On the gravitational field of a mass point according to Einstein's theory". arXiv : physics/9905030 . and Schwarzschild, K. (1916). "Über das Gravitationsfeld einer Kugel aus inkompressibler Flüssigkeit nach der Einsteinschen Theorie" . Sitzungsberichte der Königlich Preussischen Akademie der Wissenschaften . 18 : 424–434. Bibcode : 1916skpa.conf..424S .
Translation: Antoci, S. (1999). "On the gravitational field of a sphere of incompressible fluid according to Einstein's theory". arXiv : physics/9912033 .

^ Droste, J. (1917). "On the field of a single centre in Einstein's theory of gravitation, and the motion of a particle in that field" (PDF) . Proceedings Royal Academy Amsterdam . 19 (1): 197–215. Archived from the original (PDF) on 18 May 2013 . Retrieved 16 September 2012 .

^ Kox, A. J. (1992). "General Relativity in the Netherlands: 1915–1920" . In Eisenstaedt, Jean; Kox, A. J. (eds.). Studies in the history of general relativity . Birkhäuser. p. 41. ISBN 978-0-8176-3479-7 . Archived from the original on 10 August 2016 . Retrieved 23 February 2016 .

^ 't Hooft, G. (2009). "Introduction to the Theory of Black Holes" (PDF) . Institute for Theoretical Physics / Spinoza Institute. pp. 47–48. Archived from the original (PDF) on 21 May 2009 . Retrieved 24 June 2010 .

^ Eddington, Arthur (1926). The Internal Constitution of the Stars . Science . Vol. 52. Cambridge University Press. pp. 233–40. doi : 10.1126/science.52.1341.233 . ISBN 978-0-521-33708-3 . PMID 17747682 . Archived from the original on 11 August 2016.

^ Thorne, Kip S.; Hawking, Stephen (1994). Black Holes and Time Warps: Einstein's Outrageous Legacy . W. W. Norton & Company. pp. 134 –135. ISBN 978-0-393-31276-8 . Retrieved 12 April 2019 . The first conclusion was the Newtonian version of light not escaping; the second was a semi-accurate, relativistic description; and the third was typical Eddingtonian hyperbole ... when a star is as small as the critical circumference, the curvature is strong but not infinite, and space is definitely not wrapped around the star. Eddington may have known this, but his description made a good story, and it captured in a whimsical way the spirit of Schwarzschild's spacetime curvature."

^ Venkataraman, G. (1992). Chandrasekhar and his limit . Universities Press. p. 89. ISBN 978-81-7371-035-3 . Archived from the original on 11 August 2016.

^ Detweiler, S. (1981). "Resource letter BH-1: Black holes". American Journal of Physics . 49 (5): 394–400. Bibcode : 1981AmJPh..49..394D . doi : 10.1119/1.12686 .

^ Harpaz, A. (1994). Stellar evolution . A K Peters . p. 105. ISBN 978-1-56881-012-6 . Archived from the original on 11 August 2016.

^ Jump up to: a b Oppenheimer, J. R. ; Volkoff, G. M. (1939). "On Massive Neutron Cores". Physical Review . 55 (4): 374–381. Bibcode : 1939PhRv...55..374O . doi : 10.1103/PhysRev.55.374 .

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