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The amount of energy produced from the collapsing core of a massive star is pretty inconceivable. The mechanism that facilitates the creation and distribution of this energy is just as wild. If you're like me you may have heard that Supernovae are the result of stellar masses "bouncing" off the incredibly dense proto-neutron star core. Like many things in this world, reality is far more complicated. The research presented here was conducted by the Princeton Supernovae Group. David Vartanyan acknowledges NSF and DoE funding and the computational facilities at NERSC, TACC, and ALCF, with special thanks to Joseph Insley for visualization. The research was published in 🤍 and 🤍 Special thanks to: - Dr. David Vartanyan for supplying high def simulation footage and answering questions - Prof. Robin Jeffries for answering some questions and clearing up some misconceptions I had about the the Direct Urca Process and the collapse mechanism Sources/Further Reading: - Core-collapse supernova explosion theory: 🤍 - Supernova Explosions: David Branch • J. Craig Wheeler - Understanding Stellar Evolution: Henny J.G.L.M. Lamers, Emily M. Levesque - Exploding Superstars|Understanding Supernovae and Gamma-Ray Bursts: Alain Mazure - Direct URCA process in neutron stars with strong magnetic fields: 🤍 - The mechanism(s) of core-collapse supernovae: 🤍 - Neutrino transport in core collapse supernovae: 🤍 - ASASSN-15lh: A highly super-luminous supernova: 🤍 - Core Collapse Supernovae: 🤍 - Direct Urca process in a neutron star mantle: 🤍 - The Life And Death Of Stars: 🤍
Watch the entire series here: 🤍 This is part of my complete intro Astronomy class that I taught at Willam Paterson University and CUNY Hunter. If you want to watch all the videos in the correct order, please visit my website at 🤍 WOOPS LIST! 1) I made a bungle in speaking. Neither nickel-58 nor nickel-62 are radioactive. Nickel-58 actually makes up 68% of nickel. 2) Be sure to plug your ears at 🤍24:49 - bit of an audio super-nova With all the news about the fainting of Betelguese, learn why a supernova happens. Learning about Stellar Evolution of massive stars, we explore the violent Type II Supernova. They explode when they try to fuse iron and nickel in their core, but cannot, because these reactions and others near and past the "Iron Peak" have Binding Energies that are lower than for less-massive elements and isotopes. We examine Supernova 1987a as an odd example. When massive stars die, they go out with a huge bang. They seed the cosmos with their remains. The process by which they die is catastrophic and astonishing. Supplement the videos with "OpenStax Astronomy" 🤍 22: Stars from Adolescence to Old Age 🤍 23: The Death of Stars 🤍 Stellar Evolution 🤍 Supernovae 🤍 Type II Supernova 🤍 Iron Peak 🤍 Binding Energy 🤍 Supernova 1987a 🤍 30th Anniversary of SN 1987A 🤍 AAVSO Light Curve for SN 1987a 🤍 SNR 2014j in M82 🤍 The Lund/LBNL Nuclear Data Search 🤍 Live Chart of Nuclides 🤍 Stellar Nucleosynthesis This is part of an entire online introductory college course. This video series was used at William Paterson University and CUNY Hunter in online classes as well as to supplement course material. Notes and links are present in the videos at the start of each lecture. The Sun will live and die. I discuss its fate and the fate of stars with lower mass than the Sun. Along the way, we learn about red giants, helium fusion, white dwarfs, planetary nebulae, and exactly what will happen to our home Earth in about 5 billion years. Next, I explore the evolution of high mass stars. High mass stars evolve much more rapidly, and their endings are extraordinary. They are responsible for many of the elements that make up your body! The evolution of elements in the cores of high mass stars leads us to what exactly happens in the moments of their deaths. We then talk about core-collapse supernovae. When massive stars die, they go out with a huge bang. They seed the cosmos with their remains. The process by which they die is catastrophic and astonishing. Learning about Stellar Evolution of massive stars, we explore the violent Type II Supernova. They explode when they try to fuse iron and nickel in their core, but cannot, because these reactions and others near and past the "Iron Peak" have Binding Energies that are lower than for less-massive elements and isotopes. We examine Supernova 1987a as an odd example. Finally, we look at their trailings, the supernova remnants. I’ll look in detail at the results of the labors of the most massive stars in the cosmos, and some of the most beautiful sights in a telescope. The remnants of supernova explosions. We look at historical supernovae, as well as the closest, most recent one. We even learn what we might see in our Winter skies sometime very soon, when Betelguese blows up.
The explosion of very massive stars as supernovae enriches the interstellar medium with chemical elements synthesized by nuclear fusion, while giving birth to a neutron star or a black hole by the collapse of the stellar core. The transition between the collapse of the core and the ejection of the stellar envelope is a challenge for the theoretical understanding of supernovae. A hydraulic experiment designed and built at CEA made it possible to reproduce by analogy one of the phenomena of hydrodynamic instability which facilitates the explosion. This experimental approach is complementary to numerical simulations. Discover this experiment in this animation. This animated film was produced and co-funded by the CEA and the ERC, and directed by Studio Animea. Scientific and technical design: T. Foglizzo, J. Guilet, G. Durand (CEA) Don’t forget to like, comment and subscribe to our channel: 🤍 To learn more about the supernova fountain: 🤍 To learn more about the stars (in french): 🤍 To learn more about neutron stars (in french): 🤍
This movie shows the time-evolution of the shock wave that is created when the core of a massive star collapses to a proto-neutron star. The shock does not immediately explode the star but "stalls" (because the outer parts of the star [not shown in the movie] are excerting ram pressure on it). The shock is "revived" within a tenth of a second or so, most likely, by heating by neutrinos emitted from the proto-neutron star. The different colors correspond to gas of different temperature (the variable shown is "specific entropy", which is closely related to temperature). Blue corresponds to the coldest gas, green is hotter gas, and yellow and red are the hottest gas. The box-like features visible at the beginning of the movie are an artifact of the simulation method that was used. They appear when the newborn shock crosses a grid boundary of the computational grid. This movie was generated by the Simulating eXtreme Spacetimes (SXS) project. 🤍. The simulation work was led by Christian Ott at Caltech and the movie was rendered by Steve Drasco at Cal Poly San Luis Obsipo. This movie is licensed under the Creative Commons 4.0 Attribution International License, 🤍
Supernovae are some of the brightest and most powerful explosions in the universe, bright enough to outshine entire galaxies. These cosmic catastrophes come in many varieties, characterised by their elements and light. Today, we will cover the various types of supernova as we take a deep dive into these tremendous explosions. Do you use these videos to sleep or for night time watching? Check out the new sleeping space playlist, a collection of my most chilled out and ambient videos. 🤍 You can now support me on Patreon: 🤍 Patrons get ad-free access to my videos, and also get early access sneak peaks! Alternatively, you can become a channel member through YouTube: 🤍 All support is hugely appreciated and helps me in my full-time job of creating these videos! Join the official #SeaSquad Discord Server: 🤍 Business Enquiries: SEA.Enquiries🤍gmail.com SOUNDTRACK: - Woodstock | Joni Mitchell: 🤍 - Spenta Mainyu | Jesse Gallagher (YouTube Audio Library) - Access Astronomy Pt. 1 | CO.AG: 🤍 - Away | Patrick Patrikios (YouTube Audio Library) - Orbiting Knowhere | Corbyn Kites (YouTube Audio Library) - Guardian of the Threshold | I Think I Can Help You (YouTube Audio Library) - What Am I | CO.AG Music: 🤍 - The End | Kyote Hearing (YouTube Audio Library) - Attraction | Density & Time (YouTube Audio Library) - The Four Masks | I Think I Can Help You (YouTube Audio Library) - Black Moon | CO.AG Music: 🤍 - Magnetic Lullaby | Amulets (YouTube Audio Library) - So Dark | CO.AG Music: 🤍 - No. 8 Reqium | Esther Abrami (YouTube Audio Library) CO.AG Music's Channel: 🤍 FOOTAGE: The space scenes in this video were captured using SpaceEngine Pro, a virtual universe simulator: 🤍 Get SpaceEngine on Steam: 🤍 Multiple sequences are public domain footage by NASA and the European Space Agency [ESA]: - NASA: 🤍 - ESA: 🤍 Multiple stock footage clips were provided by Videezy.com Multiple graphic sequences were provided by Vecteezy.com SOURCES OF INFORMATION: - Lumen Learning, Supernova Lecture: 🤍 - Lumen Learning, Observing Supernovae: 🤍 - Ohio State University Supernova Lecture: 🤍 - Types of Supernova: 🤍 - Type 1a: 🤍 - White Dwarfs & Neutron Stars: 🤍 - Kilanovae: 🤍 CHAPTERS: 0:00 Stardust 1:58 What is a Supernova? 4:41 Historic Supernovae Observations 6:58 SN-1987A 9:41 Classifying Supernovae 12:00 Core Collapse Supernova 18:40 Types of Core Collapse Supernovae 21:35 Type 1a Supernova 24:05 Standard Candles 26:23 Kilonova (NON-ENGLISH VIEWERS) To get subtitles in another language, click the [CC] button in the bottom right corner of the screen, then click the Settings (cogwheel) icon next to it, click "Subtitles / CC" and click "Auto-Translate", and select your language from there.
A 3D core-collapse supernova simulation with a moderate rotation.
October 10, 2019 Phillips Auditorium Adam Burrows Princeton University Host: Edo Berger Abstract: Using our state-of-the-art code Fornax we have simulated the collapse and explosion of the cores of many massive-star models in three spatial dimensions. This is the most comprehensive set of realistic 3D core-collapse supernova simulations yet performed and has provided very important insights into the mechanism and character of this 50-year-old astrophysical puzzle. I will present detailed results from this suite of runs and the novel conclusions derived from our new capacity to simulate many 3D, as opposed to 2D and 1D, full physics models every year. This new capability, enabled by this new algorithm and modern HPC assets, is poised to transform our understanding of this central astrophysical phenomenon.
When a massive star reaches the end of its life, it can explode as a supernova. How quickly does this process happen? Support us at: 🤍 More stories at: 🤍 Follow us on Twitter: 🤍universetoday Follow us on Tumblr: 🤍 Like us on Facebook: 🤍 Google+ - 🤍 Instagram - 🤍 Team: Fraser Cain - 🤍fcain Jason Harmer - 🤍jasoncharmer Susie Murph - 🤍susiemmurph Brian Koberlein - 🤍briankoberlein Chad Weber - weber.chad🤍gmail.com Kevin Gill - 🤍kevinmgill Created by: Fraser Cain and Jason Harmer Edited by: Chad Weber Music: Left Spine Down - “X-Ray” 🤍 Our Sun will die a slow sad death, billions of years from now when it runs out of magic sunjuice. Sure, it’ll be a dramatic red giant for a bit, but then it’ll settle down as a white dwarf. Build a picket fence, relax on the porch with some refreshing sunjuice lemonade. Gently drifting into its twilight years, and slowly cooling down until it becomes the background temperature of the Universe. If our Sun had less mass, it would suffer an even slower fate. So then, unsurprisingly, if it had more mass it would die more quickly. In fact, stars with several times the mass of our Sun will die as a supernova, exploding in an instant. Often we talk about things that take billions of years to happen on the Guide to Space. So what about a supernova? Any guesses on how fast that happens? There are actually several different kinds of supernovae out there, and they have different mechanisms and different durations. But I’m going to focus on a core collapse supernova, the “regular unleaded” of supernovae. Stars between 8 and about 50 times the mass of the Sun exhaust the hydrogen fuel in their cores quickly, in few short million years. Just like our Sun, they convert hydrogen into helium through fusion, releasing a tremendous amounts of energy which pushes against the star’s gravity trying to collapse in on itself. Once the massive star runs out of hydrogen in its core, it switches to helium, then carbon, then neon, all the way up the periodic table of elements until it reaches iron. The problem is that iron doesn't produce energy through the fusion process, so there’s nothing holding back the mass of the star from collapsing inward. … and boom, supernova. The outer edges of the core collapse inward at 70,000 meters per second, about 23% the speed of light. In just a quarter of a second, infalling material bounces off the iron core of the star, creating a shockwave of matter propagating outward. This shockwave can take a couple of hours to reach the surface. As the wave passes through, it creates exotic new elements the original star could never form in its core. And this is where we get all get rich. All gold, silver, platinum, uranium and anything higher than iron on the periodic table of elements are created here. A supernova will then take a few months to reach its brightest point, potentially putting out as much energy as the rest of its galaxy combined. Supernova 1987A, named to commemorate the induction of the first woman into the Rock and Roll Hall of Fame, the amazing Aretha Franklin. Well, actually, that’s not true, it was the first supernova we saw in 1987. But we should really name supernovae after things like that. Still, 1987A went off relatively nearby, and took 85 days to reach its peak brightness. Slowly declining over the next 2 years. Powerful telescopes like the Hubble Space Telescope can still see the shockwave expanding in space, decades later. Our “regular flavor” core collapse supernova is just one type of exploding star. The type 1a supernovae are created when a white dwarf star sucks material off a binary partner like a gigantic parasitic twin, until it reaches 1.4 times the mass of the Sun, and then it explodes. In just a few days, these supernovae peak and fade much more rapidly than our core collapse friends. So, how long does a supernova take to explode? A few million years for the star to die, less than a quarter of a second for its core to collapse, a few hours for the shockwave to reach the surface of the star, a few months to brighten, and then just few years to fade away. Which star would you like to explode? Tell us in the comments below. Thanks for watching! Never miss an episode by clicking subscribe. Our Patreon community is the reason these shows happen. We’d like to thank David Hall and the rest of the members who support us in making great space and astronomy content. Members get advance access to episodes, extras, contests, and other shenanigans with Jay, myself and the rest of the team. Want to get in on the action? Click here.
You can buy Universe Sandbox 2 game here: 🤍 Hello and welcome to What Da Math! In this video, we will talk about supernovae Support this channel on Patreon to help me make this a full time job: 🤍 Space Engine is available for free here: 🤍 Enjoy and please subscribe. Twitter: 🤍 Facebook: 🤍 Twitch: 🤍 Bitcoins to spare? Donate them here to help this channel grow! 1GFiTKxWyEjAjZv4vsNtWTUmL53HgXBuvu
This movie shows the time-evolution of the shock wave that is created when the core of a massive star collapses to a proto-neutron star. The shock does not immediately explode the star but "stalls" (because the outer parts of the star [not shown in the movie] are excerting ram pressure on it). The shock is "revived" within a tenth of a second or so, most likely, by heating by neutrinos emitted from the proto-neutron star. The different colors correspond to gas of different temperature (the variable shown is "specific entropy", which is closely related to temperature). Blue corresponds to the coldest gas, green is hotter gas, and yellow and red are the hottest gas. The box-like features visible at the beginning of the movie are an artifact of the simulation method that was used. They appear when the newborn shock crosses a grid boundary of the computational grid. This movie was generated by the Simulating eXtreme Spacetimes (SXS) project. 🤍. The simulation work was led by Christian Ott at Caltech and the movie was rendered by Steve Drasco at Cal Poly San Luis Obispo. This movie is licensed under the Creative Commons 4.0 Attribution International License, 🤍
Massive stars fuse heavier elements in their cores than lower-mass stars. This leads to the creation of heavier elements up to iron. Iron robs critical energy from the core, causing it to collapse. The shock wave, together with a huge swarm of neutrinos, blasts through the star’s outer layers, causing it to explode. The resulting supernova creates even more heavy elements, scattering them through space. Also, happily, we’re in no danger from a nearby supernova. Check out the Crash Course Astronomy solar system poster here: 🤍 Chapters: Introduction: High Mass Stars 00:00 Core Fusion Creates Heavier Elements 0:51 Other Stages of High Mass Stars 2:22 Silicone & Iron Fusion 3:43 Core Collapse 6:20 Supernova Remnants 8:22 Explosive Nucleosynthesis 9:50 Review 11:04 PBS Digital Studios: 🤍 Follow Phil on Twitter: 🤍 Want to find Crash Course elsewhere on the internet? Facebook - 🤍 Twitter - 🤍 Tumblr - 🤍 Support CrashCourse on Patreon: 🤍 PHOTOS/VIDEOS Blowing Bubbles 🤍 [credit: NASA/CXC/April Jubett] The Sizes of Stars 🤍 [credit: ESO/M. Kornmesser] Red giants 🤍 [credit: Wikimedia Commons] Alpha Orionis 🤍 [credit: A. Dupree (CfA), NASA, ESA] Sun and VY Canis Majoris 🤍 [credit: Wikimedia Commons] Witch Head Nebula and Rigel 🤍 [credit: Rogelio Bernal Andreo] Layers of a massive star 🤍 [credit: Wikimedia Commons] NASA's Swift Reveals New Phenomenon in a Neutron Star 🤍 [credit: NASA's Goddard Space Flight Center] What is a black hole? 🤍 [credit: NASA/CXC/M.Weiss] The Death of Stars 🤍 [credit: ESA/Hubble] Giant Mosaic of the Crab Nebula 🤍 [credit: NASA, ESA, J. Hester (Arizona State University)] Hubble and Chandra spot a celestial bauble 🤍 [credit: NASA, ESA, the Hubble Heritage Team (STScI/AURA), and NASA/CXC/SAO/J. Hughes] Vela Supernova Remnant 🤍 [credit: Marco Lorenzi] Spica [credit: Phil Plait] Cassiopeia A 🤍 [credit: Oliver Krause (Steward Observatory) George H. Rieke (Steward Observatory) Stephan M. Birkmann (Max-Planck-Institut fur Astronomie) Emeric Le Floc'h (Steward Observatory) Karl D. Gordon (Steward Observatory) Eiichi Egami (Steward Observatory) John Bieging (Steward Observatory) John P. Hughes (Rutgers University) Erick Young (Steward Observatory) Joannah L. Hinz (Steward Observatory) Sascha P. Quanz (Max-Planck-Institut fur Astronomie) Dean C. Hines (Space Science Institute)] Sloshing Supernova 🤍 [credit: NASA's Goddard Space Flight Center Video and images courtesy of NASA/JPL-Caltech] Star Burst 🤍 [credit: NASA's Goddard Space Flight Center Video courtesy of ESA/Hubble/L. Calcada]
Volume rendering of entropy from a high-fidelity 3D simulation of massive stellar core collapse including rotation and magnetic fields leading up to a supernova explosion. This simulation is part of a first-of-its-kind exploration of the impact of rotation and magnetic fields on the neutrino-driven supernova mechanism and is being used to help us understand the origins of pulsars and magnetars, as well as the chemical evolution of the universe. Simulations were run using the FLASH simulation framework on the Argonne Leadership Computing Facility's Mira supercomptuer. Visualization: Sean M. Couch (Michigan State University), Kuo-Chuan Pan (National Tsinghua University), Evan P. O’Connor (Stockholm University) This research used resources of the Argonne Leadership Computing Facility, which is a DOE Office of Science User Facility supported under Contract DE-AC02-06CH11357.
Collapse-induced thermonuclear explosion of a rotating massive star to yield a core-collapse supernova. Simulated by Doron Kushnir (Weizmann Institute of Science) with the FLASH code. FLASH was in part developed by the DOE NNSA-ASC OASCR Flash Center at the University of Chicago.
3D core-collapse supernova modeling and applications to Cas A and other supernova remnants by Thomas Janka on 11/01/2019.
Astronomy Seminar: State-of-the-Art 3D Core-Collapse Supernova Explosion Simulations Speaker: Adam Burrows, Princeton University Date: March 10, 2021, 14:00 (UTC-3) Venue: IAG USP, Instituto de Astronomia, Geofisica e Ciencias Atmosfericas, Sao Paolo, Brazil Abstract: Using our state-of-the-art code Fornax we have simulated the collapse and explosion of the cores of many massive-star models in three spatial dimensions. This is the most comprehensive set of realistic 3D core-collapse supernova simulations yet performed and has provided very important insights into the mechanism and character of this almost 60-year-old astrophysical puzzle. Importantly, most multi-D models explode without artifice by the neutrino mechanism, aided by the effects of neutrino-driven turbulence. I will present detailed results from this suite of runs and the novel conclusions derived from our new capacity to simulate many 3D, as opposed to 2D and 1D, full physics models every year. This new capability, enabled by this new algorithm and modern HPC assets, is poised to transform our understanding of this central astrophysical phenomenon. About Adam Burrows: Adam Burrows is currently a Professor of Astrophysical Sciences at Princeton University. He received his undergraduate degree in Physics from Princeton and his Ph.D. in Physics from the Massachusetts Institute of Technology. His primary research interests are supernova theory, exoplanet and brown dwarf theory, planetary atmospheres, computational astrophysics, and nuclear astrophysics. Well-known as a pioneer in the theory of exoplanets, brown dwarfs, and supernovae, he has written numerous fundamental and influential papers and reviews on these subjects during the last ~35 years. He has collaborated with more than 200 co-authors on more than 400 papers and given more than 350 invited talks and colloquia. He is a member of the National Academy of Sciences (NAS), a Fellow of the American Academy of Arts and Sciences, a Fellow of the American Association for the Advancement of Science, a Fellow of the American Physical Society, the 2010 Beatrice M. Tinsley Centennial Professor, winner of the Viktor Ambartsumian International Prize, and a former Alfred P. Sloan Fellow. He was the founding Director of the Princeton Planets and Life Certificate Program, a former member of the Board of Trustees of the Aspen Center for Physics, and a Fellow of the Princeton Center for Theoretical Science (PCTS). In addition, he is a past Chair of the Board on Physics and Astronomy (BPA) of the National Research Council (NRC) of the National Academy of Sciences; was the BPA Liaison to the 2010 Decadal Survey of Astronomy; and has been a consultant for the American Museum of Natural History in New York. He has served on the Committee on Astronomy and Astrophysics (CAA) of the NRC; on the NRC Rare Isotope Science Assessment Committee; on the Subcommittee on the Implementation of the DOE Long-Range Plan for Nuclear Physics; as the Chair of the Kavli Institute for Theoretical Physics (KITP) Advisory Board; as the co-Chair of NASA's Universe Subcommittee; as the Chair of NASA's Origins Subcommittee; as a co-Chair of NASA's Strategic Roadmapping Committee "Search for Earth-like Planets"; as a co-Chair of NASA's Origins/SEUS Roadmapping committee; and as a primary author of NASA 2003 Origins Roadmap. Currently, he serves on the Space Studies Board of the National Research Council of the NAS.
View more information on the DOE NNSA SSGF Program at 🤍 Luke Roberts University of California, Santa Cruz I will discuss some aspects of what happens in and around the proto-neutron star that is left behind after a successful core-collapse supernova. This hot extended neutron star cools by neutrino emission over a period of tens of seconds. The emitted neutrinos, if detected, give us a direct window into the dense core of the supernova. In addition to giving a direct probe of a proto-neutron star's properties, the neutrino flux drives a high-entropy wind from the neutron star's surface. Although they are but a small fraction of the mass ejected in core-collapse supernovae, neutrino-driven winds have the potential to contribute significantly to supernova nucleosynthesis. I will describe our efforts to model this phase of the neutron star's life, what can be learned about the properties of matter at supra-nuclear densities from the properties of the neutrino light curve (and whether or not this can be disentangled from convection), and to what extent the neutrino-driven wind may contribute to supernova nucleosynthesis.
Recorded 01 December 2021. Irene Di Palma of the Sapienza University of Rome presents "Deep learning algorithm for core-collapse supernova detection" at IPAM's Workshop IV: Big Data in Multi-Messenger Astrophysics. Abstract: The recent discovery of gravitational waves and high-energy cosmic neutrinos, marked the beginning of a new era of the multimessenger astronomy. These new messengers, along with electromagnetic radiation and cosmic rays, give new insights into the most extreme energetic cosmic events. Among them supernovae explosion is one of the challenging targets of this new astronomical approach. Gravitational waves, much like neutrinos, are emitted from the innermost region of the core collapse supernova and thus convey information on the dynamics in the supernova core to the observer. They potentially carry information not only on the general degree of asymmetry in the dynamics of the core collapse supernova, but also more directly on the explosion mechanism, on the structural and compositional evolution of the protoneutron star, the rotation rate of the collapsed core, and the nuclear equation of state. The development of a new machine learning algorithm will be described to further improve the detectability of a gravitational wave signal from core collapse supernova and the results obtained in real detector noise data will be discussed. Learn more online at: 🤍
A rotating 20 solar mass progenitor.
People have witnessed supernovae for millennia, but what threat do they pose to life on Earth? This video is sponsored by Brilliant. You can get started for free, or the first 200 people to sign up via 🤍 get 20% off a yearly subscription. ▀▀▀ A massive thanks to Prof. Hans-Thomas Janka for helping us with the physics of supernovae and GRBs. A massive thanks to Prof. Brian Thomas for all of his help with the terrestrial effects of supernovae and GRBs. This video would not have been possible without them. Also thanks to Dr. Luke Barnes for his initial help with the literature search. Hydrogen bomb vs Supernova fact was taken from this great article by xkcd/Randall Munroe – 🤍 (based on the calculation by Andrew Karam, 2002) Cosmic bubble footage from 🤍 Neutrino driven SN explosion simulations from 🤍 ▀▀▀ References: Melott, A. et al. (2019). Hypothesis: Muon radiation dose and marine megafaunal extinction at the End-Pliocene supernova. Astrobiology, 19(6), 825-830. – 🤍 Thomas, B. C. et al. (2016). Terrestrial effects of nearby supernovae in the early Pleistocene. The Astrophysical Journal Letters, 826(1), L3 – 🤍 Melott, A. L., & Thomas, B. C. (2019). From cosmic explosions to terrestrial fires?. The Journal of Geology, 127(4), 475-481. – 🤍 Fields, B. et al. (2019). Near-Earth supernova explosions: Evidence, implications, and opportunities. arXiv preprint arXiv:1903.04589. – 🤍 Thomas, B. C., Atri, D., & Melott, A. L. (2021). Gamma-ray bursts: not so much deadlier than we thought. Monthly Notices of the Royal Astronomical Society, 500(2), 1970-1973. – 🤍 Melott, A. et al. (2004). Did a gamma-ray burst initiate the late Ordovician mass extinction?. International Journal of Astrobiology, 3(1), 55-61. – 🤍 Firestone, R. B. (2014). Observation of 23 supernovae that exploded less than 300 pc from Earth during the past 300 kyr. The Astrophysical Journal, 789(1), 29. – 🤍 Janka, H. T. (2017). Neutrino emission from supernovae. arXiv preprint arXiv:1702.08713. – 🤍 Janka, H. T., & Hillebrandt, W. (1989). Neutrino emission from type II supernovae-an analysis of the spectra. Astronomy and astrophysics, 224, 49-56. – 🤍 Janka, H. T. (2017). Neutrino-driven explosions. arXiv preprint arXiv:1702.08825. – 🤍 Karam, P. A. (2002). Gamma and neutrino radiation dose from gamma ray bursts and nearby supernovae. Health physics, 82(4), 491-499. – 🤍 Melott, A. L., Thomas, et al.. (2017). A supernova at 50 pc: effects on the Earth's atmosphere and biota. The Astrophysical Journal, 840(2), 105. – 🤍 Ludwig, P., et al. (2016). Time-resolved 2-million-year-old supernova activity discovered in Earth’s microfossil record. Proceedings of the National Academy of Sciences, 113(33), 9232-9237. – 🤍 Gritschneder, et al. (2011). The supernova triggered formation and enrichment of our solar system. The Astrophysical Journal, 745(1), 22. – 🤍 Motizuki, Y., Takahashi, et al. (2009). An Antarctic ice core recording both supernovae and solar cycles. arXiv preprint arXiv:0902.3446. – 🤍 Zucker, C. et al. (2022). Star formation near the Sun is driven by expansion of the Local Bubble. Nature, 601(7893), 334-337. – 🤍 Hirata, K. et al.(1987). Observation of a neutrino burst from the supernova SN1987A. – 🤍 Hayes, L. A., & Gallagher, P. T. (2022). A Significant Sudden Ionospheric Disturbance Associated with Gamma-Ray Burst GRB 221009A. Research Notes of the AAS, 6(10), 222. ▀▀▀ Special thanks to our Patron supporters: James Sanger, Louis Lebbos, Elliot Miller, Brian Busbee, Jerome Barakos M.D., Amadeo Bee, TTST, Balkrishna Heroor, Chris LaClair, John H. Austin, Jr., OnlineBookClub.org, Matthew Gonzalez, Eric Sexton, John Kiehl, Diffbot, Gnare, Dave Kircher, Burt Humburg, Blake Byers, Evgeny Skvortsov, Meekay, Bill Linder, Paul Peijzel, Josh Hibschman, Mac Malkawi, Mike Schneider, John Bauer, jim buckmaster, Juan Benet, Sunil Nagaraj, Richard Sundvall, Lee Redden, Stephen Wilcox, Marinus Kuivenhoven, Michael Krugman, Cy 'kkm' K'Nelson, Sam Lutfi ▀▀▀ Written by Petr Lebedev & Derek Muller Edited by Fabio Albertelli Animation by Fabio Albertelli, Jakub Misiek, Alex Drakoulis, Ivy Tello, Mike Radjabov, and Charlie Davies Filmed by Derek Muller Additional Research by Kovi Rose & Katie Barnshaw Video/photos supplied by NASA, ESA, Pond5, and Getty Images Music from Epidemic Sound & Jonny Hyman Produced by Derek Muller, Petr Lebedev, and Emily Zhang
Simulations such as this are being used to understand the process by which stars many times more massive than the Sun explode. Research into this long-standing mystery in astrophysics is being dramatically advanced by Leadership-class computing. In this visualization, the supernova shock wave is visible in faint blue while the neutrino-driven convection is shown in yellow and orange. The nascent neutron star is just visible in purple in the center of the maw. CREDITS: Sean M. Couch and Kuo-Chuan Pan, Michigan State University An award of computer time was provided by the Innovative and Novel Computational Impact on Theory and Experiment (INCITE) program. This research used resources of the Argonne Leadership Computing Facility, which is a DOE Office of Science User Facility supported under Contract DE-AC02-06CH11357.
Recorded 18 November 2021. Jose Antonio Font of the University of Valencia presents "Inference with core-collapse supernova waveforms" at IPAM's Workshop III: Source inference and parameter estimation in Gravitational Wave Astronomy. Abstract: Parameter estimation of core-collapse supernovae (CCSN) is challenged by the unmodeled nature of post-bounce gravitational waveforms and by the intrinsic difficulties involved in the modeling of explosions of massive stars. Asteroseismology of proto-neutron stars (PNS) may offer a promising approach to do so. Numerical simulations of CCSN show that g-modes are commonly excited in PNS and they are responsible for a significant fraction of the gravitational-wave signal produced by most (i.e. neutrino-driven) supernova explosions. The time-frequency evolution of those modes is linked to the physical properties of the PNS through quasi-universal relations. This talk discusses recent work aimed at inferring PNS properties through the analysis of its modes of oscillation and the gravitational waves they provoke. Observational constraints of our findings for current and third-generation gravitational-wave detectors are also reported. If time permits the talk will also cover recent results for the rather specific case of rapidly-rotating CCSN. Learn more online at: 🤍
Learn more: 🤍 Science lessons with Robert 'Uncle Bob' Martin #CleanCoders #ScienceLessons
After last week's excitement (see our astronomy sister channel at 🤍 for more details), we turn our attention to types of supernova. Featuring Professor Mike Merrifield. Deep Sky Videos on last week's Type II can be found at: 🤍 🤍 As usual, here is Mike explaining the Atlas of Creation on his shelf: 🤍 Visit our website at 🤍 We're on Facebook at 🤍 And Twitter at 🤍 This project features scientists from The University of Nottingham Sixty Symbols videos by Brady Haran
Speaker: Endeve E (University of Tennessee, USA) - (authors: Endeve E (1,2); Casanova J (2); Lentz EJ (1); Bruenn SW (3); Hix WR (1,2); Mezzacappa A (1); Messer OEB (2); - University of Tennessee, USA (1); Oak Ridge National Laboratory, USA (2); Florida Atlantic University (3)) Conference: TMB-NET: Turbulent Mixing and Beyond - Non-Equilibrium Transport across the scales | (smr 3141) 2017_08_15-12_00-smr3141
Title: Core-collapse Supernova Theory: From Neutrino-driven Explosions to Observations Speaker: Hans-Thomas Janka (MPA) Date: 2021-07-15
"3D core-collapse supernova modeling and applications to Cas A and other supernova remnants" Prof. Dr. Hans-Thomas Janka, Max Planck Institute for Astrophysics, Garching, Germany Talk at the HITS Colloquium, October 15, 2018.
Title: Core-Collapse Supernova Simulations in Three Dimensions Speaker: Sean Couch (U of Chicago) Date: October 10, 2013
SN2016aps can claim to be the brightest supernova ever observed, while it only looked like a faint 18th magnitude transient star from earth it was 3.5 billion light years away, and up close it outshone its parent galaxy by 200 times. Most interestingly it's a candidate for a supernova mechanism that's different from other core collapse supernovae - the pulsed pair production instability where the star gets so hot it starts generating electron-positron pairs in the core, reducing the core's ability to resist gravity. The Paper that documented most of this work: 🤍
When the core of a massive star collapses, a supernova explosion occurs and the collapsed core forms an extremely compact, rapidly spinning neutron star. Some theories propose that the neutrons could dissolve into free quarks, causing the neutron star to shrink further and become a strange quark star. NASA has announced the detection of a possible strange quark star. (Animation: CXC/D.Berry)
Title: Magnetic fields and rotation in core-collapse supernova Speaker: Martin Obergaulinger Date: 2009-12-15 Slides: 🤍
Elemental Iron literally sucks the life out of super-massive stars, initiating a catastrophic collapse that can culminate in a new black hole. Experts explain what goes on at this cosmic crux in the existence of stars.
3D Core collapse Supernova simulation. This simulation uses the Advanced Spectral Leakage as a neutrino treatment with 20 energy bins and 3 neutrino species. The simulation employs 2 million SPH particles and follows the catastrophic collapse of a 15 solar masses star, the subsequent formation of a proto-neutron star, and the stalling of the resulting accretion shock. The video shows a thin cut along the X-Y plane, and each sector uses a color code to show different magnitudes. Form top-left in clockwise order: temperature, the logarithm of baryonic density, electron abundance, entropy.
We've learned how stars form, and we've gone over some different types of stars, like main sequence stars, red giants, and white dwarfs. But a star will move between these categories over its lifetime. How does that happen, exactly? And what is leftover when a star dies? A white dwarf? A neutron star? A black hole? What are these objects? Let's answer all of these questions and more by analyzing the life cycle of a few different star types! Watch the whole Astronomy/Astrophysics playlist: 🤍 Classical Physics Tutorials: 🤍 Modern Physics Tutorials: 🤍 Mathematics Tutorials: 🤍 General Chemistry Tutorials: 🤍 Organic Chemistry Tutorials: 🤍 Biochemistry Tutorials: 🤍 Biology Tutorials: 🤍 EMAIL► ProfessorDaveExplains🤍gmail.com PATREON► 🤍 Check out "Is This Wi-Fi Organic?", my book on disarming pseudoscience! Amazon: 🤍 Bookshop: 🤍 Barnes and Noble: 🤍 Book Depository: 🤍
Presented as invited talk in JINA Horizons Online Conference. JINA-CEE and IReNA organized “JINA Horizons” on November 30 - December 4, 2020 - a virtual meeting that brought together the international nuclear astrophysics community to discuss open questions and future directions. 🤍 JINA-CEE provides dissemination of this video for educational purposes but does not claim ownership. JINA-CEE assumes that ownership and copyright of the online material presented here (video, audio, slides, text, etc) belongs to the author. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of JINA-CEE and/or of the National Science Foundation. Any person citing these materials for scholarly purposes should provide an appropriate reference.
A supernova is the colossal explosion of a star. Scientists have identified several types of supernova. One type, called a “core-collapse” supernova, occurs in the last stage in the life of massive stars that are at least eight times larger than our Sun. As these stars burn the fuel in their cores, they produce heat.
Type II supernova (a.k.a., core collapse supernova) AstroPictionary Astronomy Vocabulary
Dra. Melina Cecilia Bersten, Universidad Nacional de La Plata, Argentina. Supernovae (SNe) are excellent laboratories for testing many aspects of stellar-evolution theory with strong implications on many various areas of astrophysics. Their light curves are extremely sensitive to the properties of their progenitor stars or systems and their environments. With the increasing amount and improved quality of current data, new types of SNe or unexpected features in normal events are being detected. These discoveries challenge our standard knowledge of how massive stars explode, as well as the mechanisms that power these events. In this talk I will focus on the modelling efforts that we have been doing in order to understand the properties of normal and some peculiar objects.
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