Core-collapse supernova simulations in three dimensions
|
|
|
- Bernice Reynolds
- 6 years ago
- Views:
Transcription
1 Core-collapse supernova simulations in three dimensions Eric J Lentz University of Tennessee, Knoxville S. Bruenn (FAU), W. R. Hix (ORNL/UTK), O. E. B. Messer (ORNL), A. Mezzacappa (UTK), J. Blondin (NCSU), J. Casanova (ORNL), E. Endeve (ORNL), J. A. Harris (LBL), C. Keeling, R. Landfield (UTK), P. Marronetti (NSF), C. Mauney(OrSt), K. Yakunin (UTK)
2 Why study supernovae? Why do some stars explode? What leads up to the collapse? How does collapse of the core result in an explosion? Study exotic physics (nuclear matter, neutrinos, GR) and signals (neutrino, GW) Understand the generation of elements and their ejection. SN 1987a in LMC
3 Reviving stalled shock with neutrino heating standing accretion shock Adapted from Hillebrandt, Janka, & Müller, 2006, Sci. Am 295, 4, 42
4 Ingredients Matching the physical conditions to numerical inputs to reflect the physical fidelity of the system. Supernovae Simulations Pre-supernova stellar history Stellar evolution models General Relativity Full/Approximate/Newtonian Fluid dynamics & Instabilities Grids/Resolution/Symmetry Equation of State Nuclear/Electron/Network Neutrino Transport Relativity/Moments/Spectral/Ray-by-Ray Neutrino-matter interactions Which ones are needed?
5 CHIMERA CHIMERA has 3 heads Spectral Neutrino Transport (MGFLD-TRANS, Bruenn) in Ray-by-Ray Approximation using modern neutrino opacities Shock-capturing Hydrodynamics (VH1 [PPM], Blondin) Nuclear Kinetics (XNet, Hix & Thielemann) Multipole gravity w/ Spherical GR correction Equations of State: Lattimer-Swesty (K=220 MeV) Cooperstein/BCK: ρ<10 11 g/cm 3 Passive Lagrangian Tracers for post-processing Ray-by-Ray Approximation
6 Yellow/green, Red: hot plumes; blue =~ shock Lentz et al., (2015), ApJL, 807, L31
7 3D resolution Study Highest Medium Lowest 180 theta x 180 phi 90 theta x 180 phi 60 theta x 135 phi 400 km
8 Key Explosion Diagnostics Shock revives slower at lower resolution Explosion energy grows slower at lower resolution Lentz et al., in prep.
9 Neutrino driving impact Luminosities are very similar Lower resolution models are less efficient at heating
10 Contemporary model at 1-degree resolution shows early small convective features... Lentz et al., in prep.
11 ... "pre-explosion" state shows development of large plumes and an axis alignment Large, hot plumes, w/ (non-grid) dipole orientation, near shock revival
12 9.6 solar mass, zero metal Primordial composition, low-mass on border between core-collapse and white dwarf. Low densities outside Fe-core trigger quick explosion, even in 1D. Previously examined in 3D by Melson, Janka, & Marek (2015) [ApJL, 801, L24] (2-deg. Yin/Yang) showing a rapid explosion explosion boosted by multi-dimensional convection/ turbulence. 1-degree Yin/Yang, 160-species network, 259k tracer particles
13 Si-flash during collapse During collapse oxygen burning at base of Silicon shell triggers a "silicon flash" propagating outward. Burns material to Fe-peak and silicon.
14 Shock launches quickly. The silicon flash pulse remains ahead of the neutrino-powered shock until about 250 ms after bounce (~3000 km) radius.
15 Late evolution: Electron fraction (left wedge) Neutron-rich (orange) ejecta form from early plumes. Proton rich material in proto-ns wind after 400 ms.
16 Explosion energy 2D model is similar, but slightly more energetic than 3D. 0.2 B explosion, is on low end of observation, expected for some low mass stars, perhaps similar to SN 1054 (Crab) Melson+ 2015, E=0.1 FOE Lentz, Hix, Harris, et al. in prep.
17 Nucleosynthesis Late images of abundances in parallel 2D model (717 ms) Inner (wind) regions have not yet combined into heavier nuclei Ni-60 Ni-64 proton alpha
18 Summary The CHIMERA group continues to make progress in 3D (and 2D) supernova simulation with several projects coming soon to an arxiv near you... * Full model 3D resolution study. Examining resolution, turbulence, convection, and other instabilities. * The zero-metal 9.6 M_sun star explodes readily in 3D (and 2D) with large in situ network and a Silicon burning flash during collapse. * Turbulence and resolution effects in high resolution 3D wedge models (next talk) Also: * Neutrino signals from published 3D model. * Detailed nucleosynthesis from tracers in published 2D models * Gravitational wave signals of published 3D model (arxiv: ) * Error estimate analysis for tracer nucleosynthesis (arxiv: ) * Chimera methods paper
Core-collapse Supernove through Cosmic Time...
Core-collapse Supernove through Cosmic Time... Eric J Lentz University of Tennessee, Knoxville S. Bruenn (FAU), W. R.Hix (ORNL/UTK), O. E. B. Messer (ORNL), A. Mezzacappa (UTK), J. Blondin (NCSU), E. Endeve
Core-Collapse Supernova Simulation A Quintessentially Exascale Problem
Core-Collapse Supernova Simulation A Quintessentially Exascale Problem Bronson Messer Deputy Director of Science Oak Ridge Leadership Computing Facility Theoretical Astrophysics Group Oak Ridge National
Core Collapse Supernovae An Emerging Picture Stephen W. Bruenn
Core Collapse Supernovae An Emerging Picture Stephen W. Bruenn 19th Rencontres de Blois Matter and Energy in the Universe: from nucleosynthesis to cosmology Collaborators Anthony Mezzacappa John M. Blondin
Weak Interaction Physics in Core-Collapse Supernova Simulation
Weak Interaction Physics in Core-Collapse Supernova Simulation Bronson Messer Oak Ridge Leadership Computing Facility & Theoretical Astrophysics Group Oak Ridge National Laboratory MICRA 2011 Department
Two- and three-dimensional simulations of core-collapse supernovae with CHIMERA
Two- and three-dimensional simulations of core-collapse supernovae with CHIMERA ab, Stephen W. Bruenn c, J. Austin Harris a, Merek Austin Chertkow a, W. Raphael Hix ba, Anthony Mezzacappa ba, O. E. Bronson
Recent 2D/3D Core-Collapse Supernovae Simulations Results Obtained with the CHIMERA Code Stephen W. Bruenn
Recent 2D/3D Core-Collapse Supernovae Simulations Results Obtained with the CHIMERA Code Stephen W. Bruenn bruenn@fau.edu Core Collapse Supernovae 101 1 2 neutrinos 3 4 5 shock 6 7 Core Collapse Supernovae
τ coll 10 V ff g cm 3 Core collapse triggered by K-captures, photodissociation 1000 km Collapse (only core inner ~1.5 MO) Free-fall 1010 g cm-3
Core collapse triggered by Collapse (only core inner ~1.5 MO) Free-fall K-captures, photodissociation 1000 km 1010 g cm-3 30 km nuclear dens. ~ 1014 g cm-3 Bounce Shock wave Nuclear repulsion Collapse
Supernova events and neutron stars
Supernova events and neutron stars So far, we have followed stellar evolution up to the formation of a C-rich core. For massive stars ( M initial > 8 M Sun ), the contracting He core proceeds smoothly
Life of a High-Mass Stars
Life of a High-Mass Stars 1 Evolutionary Tracks Paths of high-mass stars on the HR Diagram are different from those of low-mass stars. Once these stars leave the main sequence, they quickly grow in size
Three-dimensional simulation of magneto-rotationally driven core-collapse supernovae
Three-dimensional simulation of magneto-rotationally driven core-collapse supernovae Roger Käppeli Collaborators: Christian Winteler Albino Perego Almudena Arcones Nicolas Vasset Nobuya Nishimura Matthias
Advancing Nucleosynthesis in Self-consistent, Multidimensional Models of Core-Collapse Supernovae
Advancing Nucleosynthesis in Self-consistent, Multidimensional Models of Core-Collapse Supernovae a, W. Raphael Hix ba, Merek A. Chertkow a, Stephen W. Bruenn c, Eric J. Lentz ab, O. E. Bronson Messer
Type II Supernovae Overwhelming observational evidence that Type II supernovae are associated with the endpoints of massive stars: Association with
Type II Supernovae Overwhelming observational evidence that Type II supernovae are associated with the endpoints of massive stars: Association with spiral arms in spiral galaxies Supernova in M75 Type
Neutrinos and Nucleosynthesis from Black Hole Accretion Disks. Gail McLaughlin North Carolina State University
Neutrinos and Nucleosynthesis from Black Hole Accretion Disks Gail McLaughlin North Carolina State University 1 Neutrino Astrophysics What do neutrinos do in astrophysical environments? What do neutrinos
Friday, April 29, 2011
Lecture 29: The End Stages of Massive Stellar Evolution & Supernova Review: Elemental Abundances in the Solar System Review: Elemental Abundances in the Solar System Synthesized by S and R-processes Review:
Chapter 17 Lecture. The Cosmic Perspective Seventh Edition. Star Stuff Pearson Education, Inc.
Chapter 17 Lecture The Cosmic Perspective Seventh Edition Star Stuff Star Stuff 17.1 Lives in the Balance Our goals for learning: How does a star's mass affect nuclear fusion? How does a star's mass affect
2D and 3D core-collapse supernovae simulation
2D and 3D core-collapse supernovae simulation results obtained with the CHIMERA code S. W. Bruenn 1, A. Mezzacappa 2, W. R. Hix 2, J. M. Blondin 3, P. Marronetti 1, O. E. B. Messer 4, C. J. Dirk 1 and
PUSHing CORE-COLLAPSE SUPERNOVAE TO EXPLOSIONS IN SPHERICAL SYMMETRY
PUSHing CORE-COLLAPSE SUPERNOVAE TO EXPLOSIONS IN SPHERICAL SYMMETRY Fifty-One Ergs Oregon State June 2017 Ebinger In collaboration with: Sanjana Sinha Carla Fröhlich Albino Perego Matthias Hempel Outline
Tomoya Takiwaki (RIKEN)
2014/8/25 GRB-SN Workshop@RIKEN Explosion Mechanism of Core-collapse Supernovae Tomoya Takiwaki (RIKEN) Multi-scale & Multi-physics Hydrodynamics Bar-mode Gravitational Strong General relativity Gravitational
Today. Stars. Evolution of High Mass Stars. Nucleosynthesis. Supernovae - the explosive deaths of massive stars
Today Stars Evolution of High Mass Stars Nucleosynthesis Supernovae - the explosive deaths of massive stars 1 Another good job on exam! Class average was 71% Given the difficulty of the exam, this was
Instabilities and Mixing in Supernova Envelopes During Explosion. Xuening Bai AST 541 Seminar Oct.21, 2009
Instabilities and Mixing in Supernova Envelopes During Explosion Xuening Bai AST 541 Seminar Oct.21, 2009 Outline Overview Evidence of Mixing SN 1987A Evidence in supernova remnants Basic Physics Rayleigh-Taylor
Supernova Explosions and Observable Consequences
SFB-TR7 Supernova Explosions and Observable Consequences Hans-Thomas Janka Max Planck Institute for Astrophysics, Garching Outline Introduction: The neutrino-driven mechanism Status of self-consistent
14 Supernovae (short overview) introduc)on to Astrophysics, C. Bertulani, Texas A&M-Commerce 1
14 Supernovae (short overview) introduc)on to Astrophysics, C. Bertulani, Texas A&M-Commerce 1 The core-collapse of a supernova The core of a pre-supernova is made of nuclei in the iron-mass range A ~
Theoretical Supernova Modeling: Exploring the Progenitor-Explosion-Remnant Connection by Neutrino-Driven Explosion Models
SFB-TR7 Workshop on "Probing the Supernova Mechanism by Observations" Seattle, July 16 20, 2012 Theoretical Supernova Modeling: Exploring the Progenitor-Explosion-Remnant Connection by Neutrino-Driven
Numerical simulations of core-collapse supernovae
Numerical simulations of core-collapse supernovae Jérôme Novak (Jerome.Novak@obspm.fr) Laboratoire Univers et Théories (LUTH) CNRS / Observatoire de Paris / Université Paris-Diderot 10 th Rencontres du
Stellar Explosions (ch. 21)
Stellar Explosions (ch. 21) First, a review of low-mass stellar evolution by means of an illustration I showed in class. You should be able to talk your way through this diagram and it should take at least
Evolution of High Mass Stars
Luminosity (L sun ) Evolution of High Mass Stars High Mass Stars O & B Stars (M > 4 M sun ): Burn Hot Live Fast Die Young Main Sequence Phase: Burn H to He in core Build up a He core, like low-mass stars
Introductory Astrophysics A113. Death of Stars. Relation between the mass of a star and its death White dwarfs and supernovae Enrichment of the ISM
Goals: Death of Stars Relation between the mass of a star and its death White dwarfs and supernovae Enrichment of the ISM Low Mass Stars (M
Neutrino Signatures from 3D Models of Core-Collapse Supernovae
Neutrino Signatures from 3D Models of Core-Collapse Supernovae Irene Tamborra Niels Bohr Institute, University of Copenhagen nueclipse Knoxville, August 20, 2017 Outline Supernova explosion mechanism Hydrodynamical
Compton Lecture #4: Massive Stars and. Supernovae. Welcome! On the back table:
Compton Lecture #4: Massive Stars and Welcome! On the back table: Supernovae Lecture notes for today s s lecture Extra copies of last week s s are on the back table Sign-up sheets please fill one out only
Type Ia supernovae observable nuclear astrophysics
Astrophysics and Nuclear Structure Hirschegg, January 27, 2013 Type Ia supernovae observable nuclear astrophysics Julius-Maximilians-Universität Würzburg, Germany W. Hillebrandt, S. Woosley, S. Sim, I.
Supernovae. Tomek Plewa. ASC Flash Center, University of Chicago. Konstantinos Kifonidis, Leonhard Scheck, H.-Thomas Janka, Ewald Müller
Supernovae Tomek Plewa ASC Flash Center, University of Chicago Konstantinos Kifonidis, Leonhard Scheck, H.-Thomas Janka, Ewald Müller MPA für Astrophysik, Garching FLASH, Nov. 2005 1 Outline Non-exotic
Chapter 14: The Bizarre Stellar Graveyard. Copyright 2010 Pearson Education, Inc.
Chapter 14: The Bizarre Stellar Graveyard Assignments 2 nd Mid-term to be held Friday Nov. 3 same basic format as MT1 40 mult. choice= 80 pts. 4 short answer = 20 pts. Sample problems on web page Origin
Unravelling the Explosion Mechanisms
SFB-TR7 Lectures, INAF-Osservatorio Astronomico di Brera 19. & 20. November 2013 The Violent Deaths of Massive Stars Unravelling the Explosion Mechanisms Connecting Theory to Observations Hans-Thomas Janka
Nucleosynthesis of heavy elements. Almudena Arcones Helmholtz Young Investigator Group
Nucleosynthesis of heavy elements Almudena Arcones Helmholtz Young Investigator Group The nuclear chart uranium masses measured at the ESR 82 silver gold r-proce path 126 stable nuclei 50 82 will be measured
17.3 Life as a High-Mass Star
17.3 Life as a High-Mass Star Our goals for learning: What are the life stages of a high-mass star? How do high-mass stars make the elements necessary for life? How does a high-mass star die? What are
In the Beginning. After about three minutes the temperature had cooled even further, so that neutrons were able to combine with 1 H to form 2 H;
In the Beginning Obviously, before we can have any geochemistry we need some elements to react with one another. The most commonly held scientific view for the origin of the universe is the "Big Bang"
Hirschegg Supernova core collapse. dynamics of core collapse. simple and efficient parameterization of deleptonization
Hirschegg 2006 Supernova core collapse M. Liebendörfer University of Basel U.-L. Pen & C. Thompson Canadian Institut for Theoretical Astrophysics dynamics of core collapse simple and efficient parameterization
PULSAR RECOIL BY LARGE-SCALE ANISOTROPIES IN SUPERNOVAE L. SCHECK H.-TH. JANKA, E. MÜLLER, K. KIFONIDIS, T. PLEWA
PULSAR RECOIL BY LARGE-SCALE ANISOTROPIES IN SUPERNOVAE L. SCHECK H.-TH. JANKA, E. MÜLLER, K. KIFONIDIS, T. PLEWA MAX-PLANCK-INSTITUTE FOR ASTROPHYSICS, GARCHING OUTLINE INTRODUCTION Observations Anisotropy
Comparing a Supergiant to the Sun
The Lifetime of Stars Once a star has reached the main sequence stage of it life, it derives its energy from the fusion of hydrogen to helium Stars remain on the main sequence for a long time and most
Wolfgang Hillebrandt. Garching. DEISA PRACE Symposium Barcelona May 10 12, 2010
Modelling Cosmic Explosions Wolfgang Hillebrandt MPI für Astrophysik Garching DEISA PRACE Symposium Barcelona May 10 12, 2010 Outline of the talk Supernova types and phenomenology (in brief) Models of
A Simple Approach to the Supernova Progenitor-Explosion Connection
A Simple Approach to the Supernova Progenitor-Explosion Connection Bernhard Müller Queen's University Belfast Monash Alexander Heger, David Liptai, Joshua Cameron (Monash University) Many potential/indirect
How supernova simulations are affected by input physics. Tomoya Takiwaki (RIKEN) Kei Kotake(Fukuoka) Yudai Suwa(Kyoto/MPA)
2015/08/18 MICRA2015 How supernova simulations are affected by input physics Tomoya Takiwaki (RIKEN) Kei Kotake(Fukuoka) Yudai Suwa(Kyoto/MPA) 1 Supernovae: the death of the star? Q:How does the explosion
Lecture 16: Iron Core Collapse, Neutron Stars, and Nucleosynthesis * 235. Nuclear Binding Energy.
Nuclear Binding Energy Lecture 16: Iron Core Collapse, Neutron Stars, and Nucleosynthesis http://apod.nasa.gov/apod/astropix.html Below iron can repack the nucleons into heavier nuclei and gain energy
New Results from 3-D supernova models with spectral neutrino diffusion
New Results from 3-D supernova models with spectral neutrino diffusion Stuart C. Whitehouse and Matthias Liebendörfer Department of Physics, University of Basel, Switzerland Overview Introduction The Isotropic
Stars and their properties: (Chapters 11 and 12)
Stars and their properties: (Chapters 11 and 12) To classify stars we determine the following properties for stars: 1. Distance : Needed to determine how much energy stars produce and radiate away by using
Nuclear Astrophysics
Nuclear Astrophysics II. Core-collapse supernovae Karlheinz Langanke GSI & TU Darmstadt Aarhus, October 6-10, 2008 Karlheinz Langanke ( GSI & TU Darmstadt) Nuclear Astrophysics Aarhus, October 6-10, 2008
Nuclear Astrophysics
Nuclear Astrophysics IV: Novae, x-ray bursts and thermonuclear supernovae Karlheinz Langanke GSI & TU Darmstadt Aarhus, October 6-10, 2008 Karlheinz Langanke ( GSI & TU Darmstadt) Nuclear Astrophysics
The r-process of nucleosynthesis: overview of current status. Gail McLaughlin North Carolina State University
The r-process of nucleosynthesis: overview of current status Gail McLaughlin North Carolina State University The popular press says that the gold and platinum in wedding bands is made in neutron star mergers
Einführung in die Astronomie II
Einführung in die Astronomie II Teil 10 Peter Hauschildt yeti@hs.uni-hamburg.de Hamburger Sternwarte Gojenbergsweg 112 21029 Hamburg 15. Juni 2017 1 / 47 Overview part 10 Death of stars AGB stars PNe SNe
Nuclear Physics. of Core Collapse Supernova
Subaru and Keck (NAOJ) (SST/HST/CXO/NASA) Integral (ESA) Nuclear Physics of Core Collapse Supernova W.R. Hix (ORNL/UTK) SNO W.R. Hix (ORNL/ U. Tenn.) CNS Summer Stardust School, (JPL-Caltech/NASA) August
Is strong SASI activity the key to successful neutrino-driven supernova explosions?
Is strong SASI activity the key to successful neutrino-driven supernova explosions? Florian Hanke Max-Planck-Institut für Astrophysik INT-12-2a program Core-Collapse Supernovae: Models and observable Signals,
Low Energy Neutrinos from Black Hole - Accretion Disks
Low Energy Neutrinos from Black Hole - Accretion Disks Gail McLaughlin North Carolina State University General remarks about neutrinos from hot dense environments Detection of accretion disk neutrinos
Core-Collapse Supernovae and Neutrino Transport
Core-Collapse Supernovae and Neutrino Transport SFB TR7 Gravitational Wave Astronomy Video Seminar B.Müller 5.7.2010 Core Collapse Supernovae, General Relativity & Gravitational Waves Core collapse supernova
Chapter 15. Supernovae Classification of Supernovae
Chapter 15 Supernovae Supernovae represent the catastrophic death of certain stars. They are among the most violent events in the Universe, typically producing about 10 53 erg, with a large fraction of
High Mass Stars. Dr Ken Rice. Discovering Astronomy G
High Mass Stars Dr Ken Rice High mass star formation High mass star formation is controversial! May form in the same way as low-mass stars Gravitational collapse in molecular clouds. May form via competitive
Neutrinos and explosive nucleosynthesis
Neutrinos and explosive nucleosynthesis Gabriel Martínez-Pinedo Microphysics in computational relativistic astrophysics June 22, 2011 Outline 1 Introduction 2 Neutrino-matter interactions 3 Nucleosynthesis
Integrated nucleosynthesis in neutrino-driven winds
Integrated nucleosynthesis in neutrino-driven winds L. Huther 1, T. Fischer 1, G. Martínez-Pindeo 1,2 & K. Langanke 2,3 1 TU Darmstadt, 2 GSI Helmholtzzentrum für Schwerionenforschung, 3 Frankfurt Institute
Chapter 6: Stellar Evolution (part 2): Stellar end-products
Chapter 6: Stellar Evolution (part 2): Stellar end-products Final evolution stages of high-mass stars Stellar end-products White dwarfs Neutron stars and black holes Supernovae Core-collapsed SNe Pair-Instability
Observable constraints on nucleosynthesis conditions in Type Ia supernovae
Observable constraints on nucleosynthesis conditions in Type Ia supernovae MPE Eurogenesis Garching, March 26, 2013 Ivo Rolf Seitenzahl Institut für Theoretische Physik und Astrophysik Julius-Maximilians-Universität
Excavation or Accretion from Classical Novae (or related objects) Sumner Starrfield
Excavation or Accretion from Classical Novae (or related objects) Sumner Starrfield School of Earth and Space Exploration Arizona State University KITP March 20, 2007 Collaborators: Peter Hauschildt: Hamburg
Konstantin Yakunin Joint Institute for Computational Sciences Oak Ridge National Laboratory. 3/29/17 Particle Physics and Astro-Cosmology Seminar, UTK
Konstantin Yakunin Joint Institute for Computational Sciences Oak Ridge National Laboratory 3/29/17 Particle Physics and Astro-Cosmology Seminar, UTK 1 Credit: NASA/Dana Berry, Sky Works Digital Credit:
Stars with Mⵙ go through two Red Giant Stages
Astronomy A. Dayle Hancock adhancock@wm.edu Small 239 Office hours: MTWR 10-11am Death of Stars Nuclear reactions in small stars How stars disperse carbon How low mass stars die The nature of white dwarfs
Progress of supernova simulations with the Shen equation of state
Progress of supernova simulations with the Shen equation of state Nuclei K. Sumi yoshi Supernovae Numazu College of Technology & Theory Center, KEK, Japan Crab nebula hubblesite.org Applications of nuclear
The role of neutrinos in the formation of heavy elements. Gail McLaughlin North Carolina State University
The role of neutrinos in the formation of heavy elements Gail McLaughlin North Carolina State University 1 Neutrino Astrophysics What are the fundamental properties of neutrinos? What do they do in astrophysical
The evolution of supernova progenitors
The evolution of supernova progenitors NuGrid (p,n) (γ,α) (n,α) (α,γ) (γ,p) (n,p) Samuel Jones University of Victoria In collaboration with: R. Hirschi (Keele U), K. Nomoto (Kavli IPMU), F. Herwig (UVic),
Compschool, Copenhagen Core-Collapse Supernovae. Large cancellation effects in the total energy budget:
Compschool, Copenhagen 2009 Core-Collapse Supernovae M. Liebendörfer University of Basel Collapse phase: Dynamics & ν-interactions Postbounce phase: ν-transport & explosion mechanisms Models: Approximations
Electron Flavor Neutrinos in Stellar Core Collapse and Postbounce Evolution
Electron Flavor Neutrinos in Stellar Core Collapse and Postbounce Evolution M. Liebendörfer, O. E. B. Messer, A. Mezzacappa, G. Martinez-Pinedo, W. R. Hix, F.-K. Thielemann University of Tennessee, Oak
Stellar Evolution. Stars are chemical factories The Earth and all life on the Earth are made of elements forged in stars
Lecture 11 Stellar Evolution Stars are chemical factories The Earth and all life on the Earth are made of elements forged in stars A Spiral Galaxy (Milky Way Type) 120,000 ly A few hundred billion stars
The Evolution of Low Mass Stars
The Evolution of Low Mass Stars Key Ideas: Low Mass = M < 4 M sun Stages of Evolution of a Low Mass star: Main Sequence star star star Asymptotic Giant Branch star Planetary Nebula phase White Dwarf star
Stellar Evolution. The lives of low-mass stars. And the lives of massive stars
Stellar Evolution The lives of low-mass stars And the lives of massive stars Stars of High Mass High mass stars fuse H He, but do so in a different reaction: the CNO cycle Carbon is a catalyst, speeding
Core-collapse supernovae are thermonuclear explosions
Core-collapse supernovae are thermonuclear explosions Doron Kushnir Collaborators: Boaz Katz (WIS), Kfir Blum (WIS), Roni Waldman (HUJI) 17.9.2017 The progenitors are massive stars SN2008bk - Red Super
How is the supernova shock wave revived?
How is the supernova shock wave revived? The most fundamental question in supernova theory Gravity Neutrino Heating Convection Shock Instability Nuclear Burning Rotation Magnetic Fields *New Ingredient
Guiding Questions. The Deaths of Stars. Pathways of Stellar Evolution GOOD TO KNOW. Low-mass stars go through two distinct red-giant stages
The Deaths of Stars 1 Guiding Questions 1. What kinds of nuclear reactions occur within a star like the Sun as it ages? 2. Where did the carbon atoms in our bodies come from? 3. What is a planetary nebula,
The Deaths of Stars 1
The Deaths of Stars 1 Guiding Questions 1. What kinds of nuclear reactions occur within a star like the Sun as it ages? 2. Where did the carbon atoms in our bodies come from? 3. What is a planetary nebula,
Late stages of stellar evolution for high-mass stars
Late stages of stellar evolution for high-mass stars Low-mass stars lead a relatively peaceful life in their old age: although some may gently blow off their outer envelopes to form beautiful planetary
Neutrino emission features from 3D supernova simulations
Neutrino emission features from 3D supernova simulations Irene Tamborra GRAPPA Institute, University of Amsterdam GDR Neutrino 2014 Laboratoire de l Accelérateur Linéaire, Orsay, June 17, 2014 Outline
Stellar Evolution: The Deaths of Stars. Guiding Questions. Pathways of Stellar Evolution. Chapter Twenty-Two
Stellar Evolution: The Deaths of Stars Chapter Twenty-Two Guiding Questions 1. What kinds of nuclear reactions occur within a star like the Sun as it ages? 2. Where did the carbon atoms in our bodies come
Nucleosynthesis in Core Collapse Supernovae: Knowns and Unknown. Friedrich-K. Thielemann Dept. of Physics University of Basel
Nucleosynthesis in Core Collapse Supernovae: Knowns and Unknown Friedrich-K. Thielemann Dept. of Physics University of Basel Radioactivity Diagnostics of SN1987A: 56Ni/Co, 57Ni/Co, 44Ti total/photon decay
Guiding Questions. The Deaths of Stars. Pathways of Stellar Evolution GOOD TO KNOW. Low-mass stars go through two distinct red-giant stages
The Deaths of Stars Guiding Questions 1. What kinds of nuclear reactions occur within a star like the Sun as it ages? 2. Where did the carbon atoms in our bodies come from? 3. What is a planetary nebula,
10/26/ Star Birth. Chapter 13: Star Stuff. How do stars form? Star-Forming Clouds. Mass of a Star-Forming Cloud. Gravity Versus Pressure
10/26/16 Lecture Outline 13.1 Star Birth Chapter 13: Star Stuff How do stars form? Our goals for learning: How do stars form? How massive are newborn stars? Star-Forming Clouds Stars form in dark clouds
Lecture 26. High Mass Post Main Sequence Stages
Lecture 26 Fate of Massive Stars Heavy Element Fusion Core Collapse Supernova Neutrinoes Gaseous Remnants Neutron Stars Mar 27, 2006 Astro 100 Lecture 26 1 High Mass Post Main Sequence Stages For M(main
Ch. 16 & 17: Stellar Evolution and Death
Ch. 16 & 17: Stellar Evolution and Death Stars have lives: born, evolve, die Mass determines stellar evolution: Really Low Mass (0.08 to 0.4 M sun ) Low Mass: (0.4 to 4 M sun ) Long lives High Mass (4
Parametrization of the effect of weak interactions on the production of heavy elements in binary neutron star mergers.
Parametrization of the effect of weak interactions on the production of heavy elements in binary neutron star mergers. S. Ning, H. Gerling-Dunsmore, L. Roberts 1 Abstract. Recent research 1 has shown that
Explosion Models of CoreCollapse Supernovae
SFB-TR7 Hirschegg 2013: Astrophysics and Nuclear Structure Hirschegg, Austria, January 26 February 1, 2013 Explosion Models of CoreCollapse Supernovae Status of Modeling at Garching Hans-Thomas Janka Max
Star Death ( ) High Mass Star. Red Supergiant. Supernova + Remnant. Neutron Star
Star Death High Mass Star Red Supergiant A star with mass between 8 M and 20 M will become a red supergiant and will subsequently experience a supernova explosion. The core of this star will have a mass
Supernova Nucleosynthesis
Supernova Nucleosynthesis Andrea Kulier Princeton University, Department of Astrophysical Sciences November 25, 2009 Outline o Overview o Core-Collapse Supernova Nucleosynthesis o Explosive Nucleosynthesis
Supernovae, Gamma-Ray Bursts, and Stellar Rotation
Supernovae, Gamma-Ray Bursts, and Stellar Rotation When Massive Stars Die, How Do They Explode? Neutron Star + Neutrinos Neutron Star + Rotation Black Hole + Rotation Colgate and White (1966) Arnett Wilson
Stars: Their Life and Afterlife
The 68 th Compton Lecture Series Stars: Their Life and Afterlife Lecture 3: The Life and Times of Low Mass Stars Brian Humensky, lecturer http://kicp.uchicago.edu/~humensky/comptonlectures.htm October
Spectrum of the Supernova Relic Neutrino Background
Spectrum of the Supernova Relic Neutrino Background Ken ichiro Nakazato (Tokyo University of Science) Numazu Workshop 2015, Sep. 1, 2015 Outline 1. Introduction Neutrino signal from supernovae Supernova
ASTRONOMY 220C ADVANCED STAGES OF STELLAR EVOLUTION AND NUCLEOSYNTHESIS. Spring, This is a one quarter course dealing chiefly with:
This is a one quarter course dealing chiefly with: ASTRONOMY 220C ADVANCED STAGES OF STELLAR EVOLUTION AND NUCLEOSYNTHESIS Spring, 2015 http://www.ucolick.org/~woosley a) Nuclear astrophysics and the relevant
Lecture 16: Iron Core Collapse, Neutron Stars, and Nucleosynthesis * 235. Nuclear Binding Energy.
Nuclear Binding Energy Lecture 16: Iron Core Collapse, Neutron Stars, and Nucleosynthesis http://apod.nasa.gov/apod/astropix.html Below iron can repack the nucleons into heavier nuclei and gain energy
15 Post-main sequence stellar evolution
15 Post-main sequence stellar evolution After the MS, the core becomes structured in concentric shells in which H, He, C/O, etc., burn at various times. This happens together with readjustments involving
Nuclear physics input for the r-process
Nuclear physics input for the r-process Gabriel Martínez Pinedo INT Workshop The r-process: status and challenges July 28 - August 1, 2014 Nuclear Astrophysics Virtual Institute Outline 1 Introduction
Supernova Explosion Mechanisms
SFB-TR7 SFB-TR27 International Conference Physics of Neutron Stars 2011 St. Petersburg, Russia, July 11-15, 2011 Supernova Explosion Mechanisms Advancing to the 3rd Dimension: Supernova Models Confronting
Life and Death of a Star. Chapters 20 and 21
Life and Death of a Star Chapters 20 and 21 90 % of a stars life Most stars spend most of their lives on the main sequence. A star like the Sun, for example, after spending a few tens of millions of years
Explosion Models of Massive Stars
SFB-TR7 Fifty-One Ergs NC State University, Raleigh, North Carolina, May 13th 17th, 2013 Explosion Models of Massive Stars Hans-Thomas Janka Max Planck Institute for Astrophysics, Garching Heinzi-Ado Arnolds
This class: Life cycle of high mass stars Supernovae Neutron stars, pulsars, pulsar wind nebulae, magnetars Quark-nova stars Gamma-ray bursts (GRBs)
This class: Life cycle of high mass stars Supernovae Neutron stars, pulsars, pulsar wind nebulae, magnetars Quark-nova stars Gamma-ray bursts (GRBs)!1 Cas$A$ All$Image$&$video$credits:$Chandra$X7ray$ Observatory$
Chapter 19: The Evolution of Stars
Chapter 19: The Evolution of Stars Why do stars evolve? (change from one state to another) Energy Generation fusion requires fuel, fuel is depleted [fig 19.2] at higher temperatures, other nuclear process
Lecture 15. Explosive Nucleosynthesis and the r-process
Lecture 15 Explosive Nucleosynthesis and the r-process As the shock wave passes through the star, matter is briefly heated to temperatures far above what it would have experienced in hydrostatic equilibrium.
Chapter 17 Lecture. The Cosmic Perspective Seventh Edition. Star Stuff Pearson Education, Inc.
Chapter 17 Lecture The Cosmic Perspective Seventh Edition Star Stuff 17.1 Lives in the Balance Our goals for learning: How does a star's mass affect nuclear fusion? How does a star's mass affect nuclear