Neutron star post-merger simulations: origin of kilonovae and the heavy elements
|
|
- Carmella Jackson
- 6 years ago
- Views:
Transcription
1 4-color Process 100% Cyan 72% Magenta logo can also be rendered in black, grey (60% black), Pantone 280, or Pantone 286; on a darker color background, the logo can be rendered in Pantone 290, 291, or 284, depending on which color works best with the overall design of your product, the media in which it will be reproduced, and its intended use. Neutron star post-merger simulations: origin of kilonovae and the heavy elements White or Pantone 290 (Columbia Blue) Background: Pantone 286 Daniel M. Siegel Center for Theoretical Physics & Columbia Astrophysics Columbia University For photographs, use the logo in white against a darker area, positioning it either at top left/right or Laboratory bottom left/right. Einstein Fellows Symposium, Harvard-Smithsonian Center for Astrophysics, Oct 12-13,
2 1/10 NS post-merger accretion disks: formation Movie: long-term evolution of post-merger accretion disk, MBH=3Msun (spin: 0.8), Mdisk=0.02Msun Movie: BNS merger and formation of post-merger accretion disk Radice+ 2016
3 NS post-merger accretion disks: numerical setup First self-consistent simulations modeling r-process nucleosynthesis from disk outflows from first principles: GRMHD: magnetic instabilities (MRI) mediating turbulence (transport of angular momentum) in the disk weak interactions in GRMHD approximate neutrino transport (leakage scheme) realistic EOS (Helmholtz EOS) valid at low temperatures and densities, capturing nuclear binding energy release from alpha-particle formation full r-process network calculations on disk outflows using 104 tracer particles (SkyNet; Lippuner & Roberts 2015) Previous Newtonian alpha-disk simulations: Fig.: disk properties; contours: optical depth for electron neutrinos Fernandez & Metzger 2013 Metzger & Fernandez 2014 Fernandez Fernandez Just /10
4 MHD turbulence Fig.: disk properties; contours: optical depth for electron neutrinos Fig.: magnetic fields in the disk; contours: rest-mass density magnetic properties very similar to Ciolfi /10
5 MHD turbulence average radially for space-time diagram Fig.: disk properties; contours: optical depth for electron neutrinos Fig.: magnetic fields in the disk; contours: rest-mass density magnetic properties very similar to Ciolfi /10
6 Accretion disk dynamo: butterfly diagram magnetic energy is generated in the mid-plane migrates to higher latitudes dissipates into heat off the mid-plane hot corona hot corona launches thermal outflows (neutron-rich wind) NS post-merger accretion disk are cooled from the mid-plane by neutrinos (rather than from the EM photosphere)! 4/10
7 Self-regulation neutrinos Neutrino-cooled accretion disks self-regulate themselves to mild degeneracy (low Ye matter): Beloborodov 2003, Chen & Beloborodov 2007, Metzger viscous heating via magnetic turbulence neutrino cooling charged-current processes: e + p! n + e e+ + n! p + e pair annihilation: e + e+! e + e e + e+! µ, + µ, plasmon decay:! e + e! µ, + µ, Fig.: disk properties; contours: rest-mass density 5/10
8 Self-regulation neutrinos Neutrino-cooled accretion disks self-regulate themselves to mild degeneracy (low Ye matter): Beloborodov 2003, Chen & Beloborodov 2007, Metzger viscous heating via magnetic turbulence neutrino cooling balance with feedback mechanism: higher degeneracy µe /kt fewer e-, e+ (lower Ye) less neutrino emission, i.e., cooling higher temperatures lower degeneracy µe /kt Fig.: disk properties; contours: rest-mass density direct evidence of self-regulation 5/10
9 6/10 The origin of the elements r-process s-process How are the heavy elements formed?
10 The origin of heavy nuclei: r-process nucleosynthesis Movie: r-process nucleosynthesis from NS merger remnant disks 7/10
11 8/10 r-process nucleosynthesis 1st peak 2nd peak 3rd peak 2nd peak rare-earth peak 3rd peak rare-earth peak neutrino absorption robust 2nd and 3rd peak r-process! including neutrino absorption: additional good fit to 1st & 2nd peak elements production of all r-process elements!
12 /mnras.oxfordjournals.org/ at Columbia University on October 8, 2016 r-process nucleosynthesis from NS mergers ach panel) of the ejecta for the LK_QC (upper panel) and M0_QC at radius r = 200 M 295 km and only considers the unbound ch we do not measure any outflow of unbound matter (i.e. where road 60 angle from the equator. The material at low altitudes is ms for the different componentsradice+ of the outflow dynamical ejecta: Fig.:normalized production elements from with early e yields are withof ther-process total abundance of elements escriptiona (pure HY or leakage only cooling, BNS hydrodynamics, merger (dynamical ejecta,with neutrino-driven! 120 is very robust and in overall good agreement with the Solar ejecta of winds) Post-merger accretion disk outflows: 1st peak 2nd peak 3rd peak rare-earth peak Fig.: production of all r-process elements from outflows of post-merger accretion disk Overall ejecta mass per event: Radice h three different levels of microphysical description (HY,Sekiguchi M0). The dynamical ejecta 3from all our simulations ispalenzuela+2015 disk rich with mass-averaged electron fractions Ye! 0.2 (seelehner+2016 strongly depends on EOS entropy perciolfi+2017 We show the joint distribution of Ye and specific robust lower for simulation QC_M0 inand Fig.mass 10. There is an approximate ratio! shock heated on between Ye and s, due to the fact NSthat post-merger simulations: origin of kilonovae and the heavy elements M & 0.4 M & 10 2 M limit 9/10
13 Conclusions Simulations of NS post-merger accretion disks Siegel & Metzger 2017b, i. prep. GRMHD with weak interactions and approx. neutrino transport first fully self-consistent study of its kind evidence for hot coronae that launch thermal outflows first identification of self-regulation in neutrino-cooled accretion disks, implying conditions of neutron richness disk ejecta can be higher than dynamical ejecta from the merger main fuel to power kilonova main site of the r-process suggest NS post-merger systems are robust site of the r-process can produce all r-process elements NS post-merger Short gamma-ray simulations: bursts origin in of thekilonovae time-reversal and thescenario heavy elements 10/10
GRMHD simulations of remnant accretion disks from neutron star mergers
4-color Process 0% Cyan 72% Magenta logo can also be rendered in black, grey (60% black), Pantone 280, or Pantone 286; on a darker color background, the logo can be rendered in Pantone 290, 291, or 284,
More informationProbing the Creation of the Heavy Elements in Neutron Star Mergers
Probing the Creation of the Heavy Elements in Neutron Star Mergers Daniel Kasen UC Berkeley/LBNL r. fernandez, j. barnes, s. richers, f. foucart, d. desai, b. metzger, n. badnell, j. lippuner, l. roberts
More informationGeneral Relativistic MHD Simulations of Neutron Star Mergers
General Relativistic MHD Simulations of Neutron Star Mergers Luca Baiotti Osaka University with Luciano Rezzolla, Bruno Giacomazzo, Kentaro Takami Plan of the talk Brief overview of the status of BNS simulations
More informationDelayed Outflows from BH Accretion Tori Following Neutron Star Binary Coalescence. Brian Metzger
Delayed Outflows from BH Accretion Tori Following Neutron Star Binary Coalescence Brian Metzger (Columbia University) In Collaboration with Rodrigo Fernandez (IAS) Almudena Arcones, Gabriel Martinez-Pinedo
More informationMass ejection from neutron-star mergers in numerical relativity
Mass ejection from neutron-star mergers in numerical relativity Masaru Shibata Center for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto University I. Brief introduction Outline
More informationExtreme Transients in the Multimessenger Era
Extreme Transients in the Multimessenger Era Philipp Mösta Einstein fellow @ UC Berkeley pmoesta@berkeley.edu BlueWBlueWaters Symposium 2018 Sunriver Resort Core-collapse supernovae neutrinos turbulence
More informationGravitational Waves and Electromagnetic Signals from a Neutron Star Merger
Gravitational Waves and Electromagnetic Signals from a Neutron Star Merger end-to-end physics of NS mergers GRB + afterflow binary stellar evolution (10 6-10 9 years) Final inspiral (minutes) gravitational
More informationShort GRB and kilonova: did observations meet our theoretical predictions?
Short GRB and kilonova: did observations meet our theoretical predictions? Riccardo Ciolfi INAF - Astronomical Observatory of Padova INFN - Trento Institute for Fundamental Physics and Applications GW170817
More informationNobuya Nishimura Keele University, UK
7. Aug. 2014 @INT Studies of r-process nucleosynthesis based on recent hydrodynamical models of NS-NS mergers Nobuya Nishimura Keele University, UK The r-process: observational request - many r-rich Galactic
More informationNucleosynthesis in Jets from A Collapsar before The Formation of A Black Hole
before The Formation of A Black Hole Kumamoto National College of Technology, Kumamoto 861-1102, Japan E-mail: fujimoto@ec.knct.ac.jp Nobuya Nishimura, Masa-aki Hashimoto, Department of Physics, School
More informationNuclear 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
More informationNS+NS/BH mergers: GW and em counterparts Models and observations needed
NS+NS/BH mergers: GW and em counterparts Models and observations needed Kandinksy Ccomposition 8-1923 Kandinksy Curves and sharp angles - 1923 Frédéric Daigne (Institut d Astrophysique de Paris Sorbonne
More informationSimulations of neutron star mergers: Status and prospects
Simulations of neutron star mergers: Status and prospects David Radice 1,2 1 Research Associate, Princeton University 2 Taplin Member, Institute for Advanced Study First multi-messenger observations of
More informationNUCLEOSYNTHESIS INSIDE GAMMA-RAY BURST ACCRETION DISKS AND ASSOCIATED OUTFLOWS
NUCLEOSYNTHESIS INSIDE GAMMA-RAY BURST ACCRETION DISKS AND ASSOCIATED OUTFLOWS Indrani Banerjee Indian Institute of Science Bangalore The work has been done in collaboration with Banibrata Mukhopadhyay
More informationBrian Metzger Princeton University NASA Einstein Fellow
EM Counterparts of Neutron Star Binary Mergers and their Detection in the Era of Advanced LIGO Brian Metzger Princeton University NASA Einstein Fellow In Collaboration with: Edo Berger (Harvard CfA) Eliot
More informationNuclear robustness of the r process in neutron-star mergers
Nuclear robustness of the r process in neutron-star mergers Gabriel Martínez Pinedo International Nuclear Physics Conference Adelaide, Australia, September 11-16, 2016 Nuclear Astrophysics Virtual Institute
More informationMHD simulation for merger of binary neutron stars in numerical relativity
MHD simulation for merger of binary neutron stars in numerical relativity M. SHIBATA (Yukawa Institute for Theoretical Physics, Kyoto University) In collaboration with K. Kiuchi, L. Baiotti, & Y. Sekiguchi
More informationNucleosynthesis 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
More informationNeutrinos 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
More informationTomoya 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
More information14 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 ~
More informationThe 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
More informationr-process nucleosynthesis in neutron star mergers and associated macronovae events
r-process nucleosynthesis in neutron star mergers and associated macronovae events Oleg Korobkin Stockholm University, Oskar Klein Centre, Sweden March 14, 2014 O. Korobkin () r-process in neutron star
More informationNucleosynthesis in core-collapse supernovae. Almudena Arcones
Nucleosynthesis in core-collapse supernovae Almudena Arcones Nucleosynthesis in core-collapse supernovae Explosive nucleosynthesis: O, Mg, Si, S, Ca, Ti, Fe, p-process shock wave heats falling matter shock
More informationLow 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
More informationNucleosynthesis from Black Hole Accretion Disks. Gail McLaughlin North Carolina State University Rebecca Surman Union College
Nucleosynthesis from Black Hole Accretion Disks Gail McLaughlin North Carolina State University Rebecca Surman Union College 1 Three Relevant Nucleosynthesis Processes Explosive Burning e. g. shock moves
More informationHPC in Physics. (particularly astrophysics) Reuben D. Budiardja Scientific Computing National Institute for Computational Sciences
HPC in Physics (particularly astrophysics) Reuben D. Budiardja Scientific Computing National Institute for Computational Sciences 1 Gravitational Wave Einstein s Unfinished Symphony Marcia Bartuciak Predicted
More informationParametrization 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
More informationFormation and evolution of BH and accretion disk in Collapsar
Formation and evolution of BH and accretion disk in Collapsar Yuichiro Sekiguchi National Astronomical Observatory of Japan arxiv : 1009.5303 Motivation Collapsar model of GRB Central engine : Black hole
More information14/11/2018. L Aquila - Multi-messenger studies of NS mergers, GRBs and magnetars. Simone Dall Osso
L Aquila - 14/11/2018 Multi-messenger studies of NS mergers, GRBs and magnetars Simone Dall Osso OUTLINE 1. Overview of GW/EM discoveries since 2015 binary black hole mergers binary neutron star mergers
More informationIdentifying the Remnants of Neutron Star Mergers. Wen-fai Fong University of Arizona
Identifying the Remnants of Neutron Star Mergers Wen-fai Fong University of Arizona Einstein Fellows Symposium, Harvard-Smithsonian Center for Astrophysics, 10.27.2015 What s left after two neutron stars
More informationGR SIMULATIONS OF COMPACT BINARY MERGERS. Bruno Giacomazzo JILA, University of Colorado, USA
GR SIMULATIONS OF COMPACT BINARY MERGERS Bruno Giacomazzo JILA, University of Colorado, USA WHY SO INTERESTING? Due to their duration and dynamics, NS-NS and NS-BH binaries are very good sources for gravitational
More informationNeutron skin measurements and its constraints for neutron matter. C. J. Horowitz, Indiana University INT, Seattle, 2016
Neutron skin measurements and its constraints for neutron matter C. J. Horowitz, Indiana University INT, Seattle, 2016 1 Neutron Rich Matter Compress almost anything to 10 11 + g/cm 3 and electrons react
More informationMagnetorotational Instability: Plans at MPA, IPP and TU Berlin
Magnetorotational Instability: Plans at MPA, IPP and TU Berlin Wolf-Christian Müller 1, Ewald Müller 2, Thomas Janka 2, Frank Jenko 3 1 Max-Planck-Institut für Plasmaphysik, Garching 2 Max-Planck-Institut
More informationNuclear physics impact on kilonova light curves
Nuclear physics impact on kilonova light curves Gabriel Martínez Pinedo INT-JINA symposium: First multi-messenger observations of a neutron star merger and its implications for nuclear physics, INT, Seattle,
More informationNumerical modeling of binary neutron star mergers
Numerical modeling of binary neutron star mergers Kenta Kiuchi (YITP) Masaru Shibata (YITP), Yuichiro Sekiguchi (Toho Univ.), Koutarou Kyutoku (KEK), Kyohei Kawaguchi (AEI) Dawn of the GW astronomy 2016-2017~
More informationCore 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
More informationCompschool, 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
More informationImportant (!) Effects of Nucleosynthesis on the EM Signatures of Neutron Star Mergers. Brian Metzger
Important (!) Effects of Nucleosynthesis on the EM Signatures of Neutron Star Mergers Brian Metzger Princeton University NASA Einstein Fellow In Collaboration with Almudena Arcones (U Basel) & Gabriel
More informationRadiative MHD. in Massive Star Formation and Accretion Disks. Rolf Kuiper, Hubert Klahr, Mario Flock, Henrik Beuther, Thomas Henning
Radiative MHD in Massive Star Formation and Accretion Disks, Hubert Klahr, Mario Flock, Henrik Beuther, Thomas Henning, Radiative MHD with Makemake and Pluto : We developed a fast 3D frequency-dependent
More informationGravitational waves (...and GRB central engines...) from neutron star mergers
Gravitational waves (...and GRB central engines...) from neutron star mergers Roland Oechslin MPA Garching, SFB/TR 7 Ringberg Workshop, 27.3.2007 In this talk: -Intro: -Overview & Motivation -Neutron star
More informationBlack hole accretion with a tilt
Black hole accretion with a tilt Alexander (Sasha) Tchekhovskoy Northwestern University Koushik Chatterjee Matthew Liska M87 Jet: Acceleration and Collimation over 5 Orders in Distance Chandra XRC Relativistic
More informationType 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.
More informationExploring Astrophysical Magnetohydrodynamics Using High-power Laser Facilities
Exploring Astrophysical Magnetohydrodynamics Using High-power Laser Facilities Mario Manuel Einstein Fellows Symposium Harvard-Smithsonian Center for Astrophysics October 28 th, 2014 Ø Collimation and
More informationAstronomy 1504 Section 002 Astronomy 1514 Section 10 Midterm 2, Version 1 October 19, 2012
Astronomy 1504 Section 002 Astronomy 1514 Section 10 Midterm 2, Version 1 October 19, 2012 Choose the answer that best completes the question. Read each problem carefully and read through all the answers.
More informationCore-collapse supernova simulations in three dimensions
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),
More informationExplosive nucleosynthesis of heavy elements:
Explosive nucleosynthesis of heavy elements: an astrophysical and nuclear physics challenge Gabriel Martínez Pinedo NUSPIN 2017 GSI, Darmstadt, June 26-29, 2017 32 30 28 34 36 38 40 42 46 44 48 26 28 60
More informationACTIVE GALACTIC NUCLEI: FROM THE CENTRAL BLACK HOLE TO THE GALACTIC ENVIRONMENT
Julian H. Krolik ACTIVE GALACTIC NUCLEI: FROM THE CENTRAL BLACK HOLE TO THE GALACTIC ENVIRONMENT PRINCETON UNIVERSITY PRESS Princeton, New Jersey Preface Guide for Readers xv xix 1. What Are Active Galactic
More informationHigh-Energy Plasma Astrophysics and Next Generation Gamma-Ray Observatory Cherenkov Telescope Array
High-Energy Plasma Astrophysics and Next Generation Gamma-Ray Observatory Cherenkov Telescope Array FAPESP CUNY Week, New York, November 2018 M82 Star Formation- Clouds-SNRturbulence connection Sun & Stars
More informationNeutrinos in supernova evolution and nucleosynthesis
Neutrinos in supernova evolution and nucleosynthesis Gabriel Martínez Pinedo International School of Nuclear Physics 39th Course Neutrinos in Cosmology, in Astro-, Particle- and Nuclear Physics Erice,
More informationA Turbulent Dynamo in Rotating Magnetized Core-Collapse Supernovae
A Turbulent Dynamo in Rotating Magnetized Core-Collapse Supernovae David Radice R. Haas, P. Mösta, L. Roberts, C.D. Ott, E. Schnetter Core-Collapse Supernovae Core-Collapse Supernovae in Numbers ~ (50
More informationChapter 18 Reading Quiz Clickers. The Cosmic Perspective Seventh Edition. The Bizarre Stellar Graveyard Pearson Education, Inc.
Reading Quiz Clickers The Cosmic Perspective Seventh Edition The Bizarre Stellar Graveyard 18.1 White Dwarfs What is a white dwarf? What can happen to a white dwarf in a close binary system? What supports
More informationShort gamma-ray bursts from binary neutron star mergers: the time-reversal scenario
Short gamma-ray bursts from binary neutron star mergers: the time-reversal scenario Riccardo Ciolfi Physics Department, University of Trento INFN-TIFPA, Trento Institute for Fundamental Physics and Applications
More informationarxiv:astro-ph/ v1 27 Jul 2004
1 Prospects for obtaining an r process from Gamma Ray Burst Disk Winds arxiv:astro-ph/0407555v1 27 Jul 2004 G. C. McLaughlin a, and R. Surman b a Department of Physics, North Carolina State University,
More informationRef. PRL 107, (2011)
Kenta Kiuchi, Y. Sekiguchi, K. Kyutoku, M. Shibata Ref. PRL 107, 051102 (2011) Y TP YUKAWA INSTITUTE FOR THEORETICAL PHYSICS Introduction Coalescence of binary neutron stars Promising source of GWs Verification
More informationWhy study plasma astrophysics?
Why study plasma astrophysics? Nick Murphy and Xuening Bai Harvard-Smithsonian Center for Astrophysics Astronomy 253: Plasma Astrophysics January 25, 2016 Today s plan Definition of a plasma Plasma astrophysics:
More informationNuclear 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
More informationNucleosynthesis Process. Ba: s-process Ag, Eu: r-process
Nucleosynthesis Process Ba: s-process Ag, Eu: r-process Ba Ag Eu Nucleosynthesis Process Ba: s-process Ag, Eu: r-process Ba Ag Eu Nucleosynthesis Process Ba: s-process Ag, Eu: r-process Ba Ag Eu 0 Metal-poor
More informationτ 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
More informationOur sole source of light and heat in the solar system. A very common star: a glowing g ball of gas held together by its own gravity and powered
The Sun Visible Image of the Sun Our sole source of light and heat in the solar system A very common star: a glowing g ball of gas held together by its own gravity and powered by nuclear fusion at its
More informationMAGNETIZED BINARY NEUTRON STAR MERGERS. Bruno Giacomazzo Department of Astronomy, University of Maryland, USA NASA Goddard Space Flight Center, USA
MAGNETIZED BINARY NEUTRON STAR MERGERS Bruno Giacomazzo Department of Astronomy, University of Maryland, USA NASA Goddard Space Flight Center, USA PLAN OF THE TALK Introduction Magnetized Binary Neutron
More informationAdvanced Stellar Astrophysics
v Advanced Stellar Astrophysics William K. Rose University of Maryland College Park CAMBRIDGE UNIVERSITY PRESS Contents Preface xiii Star formation and stellar evolution: an overview 1 1 A short history
More informationAstronomy 404 October 18, 2013
Astronomy 404 October 18, 2013 Parker Wind Model Assumes an isothermal corona, simplified HSE Why does this model fail? Dynamic mass flow of particles from the corona, the system is not closed Re-write
More informationPUSHing 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
More informationGENERAL RELATIVISTIC SIMULATIONS OF NS BINARIES. Bruno Giacomazzo University of Trento and INFN-TIFPA, Italy
GENERAL RELATIVISTIC SIMULATIONS OF NS BINARIES Bruno Giacomazzo University of Trento and INFN-TIFPA, Italy WHY SO INTERESTING? Due to their duration and dynamics, NS-NS and NS-BH binaries are very good
More informationElectromagnetic counterparts to binary neutron star mergers. Koutarou Kyutoku (KEK) Collaborators: Kunihito Ioka (KEK), Masaru Shibata (YITP)
Electromagnetic counterparts to binary neutron star mergers Koutarou Kyutoku (KEK) Collaborators: Kunihito Ioka (KEK), Masaru Shibata (YITP) Summary Electromagnetic counterparts to gravitational waves
More informationStellar 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
More informationScience Olympiad Astronomy C Division Event MIT Invitational
Science Olympiad Astronomy C Division Event MIT Invitational Massachusetts Institute of Technology Cambridge, MA January 20, 2018 Team Number: Team Name: Instructions: 1) Please turn in all materials at
More informationAccretion onto the Massive Black Hole in the Galactic Center. Eliot Quataert (UC Berkeley)
Accretion onto the Massive Black Hole in the Galactic Center Eliot Quataert (UC Berkeley) Why focus on the Galactic Center? GR! Best evidence for a BH (stellar orbits) M 4x10 6 M Largest BH on the sky
More informationTransient Events from Neutron Star Mergers
Transient Events from Neutron Star Mergers Li-Xin Li Kavli Institute for Astronomy and Astrophysics Peking University, Beijing Transient Astronomical Events Transient astronomical events include all astronomical
More informationNucleosynthesis in core-collapse supernovae. Almudena Arcones
Nucleosynthesis in core-collapse supernovae Almudena Arcones Solar system abundances Solar photosphere and meteorites: chemical signature of the gas cloud where the Sun formed. Contribution of all nucleosynthesis
More informationPTYS/ASTR 206. The Sun 3/1/07
The Announcements Reading Assignment Review and finish reading Chapter 18 Optional reading March 2006 Scientific American: article by Gene Parker titled Shielding Space Travelers http://en.wikipedia.org/wiki/solar_variability
More informationFriday, 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:
More informationSynergy of GWs and EM signals
Leiden, Feb 04 2015 Synergy of GWs and EM signals Gravitational wave facilities (LIGO, VIRGO ) Transient facilities (PTF, ZTF ) Stephan Rosswog I. Gravitational wave detection LIGO & VIRGO detectors currently
More informationν-driven wind in the Aftermath of Neutron Star Merger
ν-driven wind in the Aftermath of Neutron Star Merger Albino Perego in collaboration with A. Arcones, R. Cabezon, R. Käppeli, O. Korobkin, M. Liebendörfer, D. Martin, S. Rosswog albino.perego@physik.tu-darmstadt.de
More informationTesting GR with Compact Object Binary Mergers
Testing GR with Compact Object Binary Mergers Frans Pretorius Princeton University The Seventh Harvard-Smithsonian Conference on Theoretical Astrophysics : Testing GR with Astrophysical Systems May 16,
More informationGravitational waves and dynamical mass ejection from binary neutron-star mergers
Gravitational waves and dynamical mass ejection from binary neutron-star mergers Masaru Shibata Yukawa Institute for Theoretical Physics, Kyoto University In collaboration with Hotokezaka, Kiuchi, Kyutoku,
More informationThe ECHO code: from classical MHD to GRMHD in dynamical spacetimes
The ECHO code: from classical MHD to GRMHD in dynamical spacetimes Luca Del Zanna Dipartimento di Fisica e Astronomia Università di Firenze Main collaborators: N. Bucciantini, O. Zanotti, S. Landi 09/09/2011
More informationShort GRBs: Progenitors, r-process Nucleosynthesis, and Gravitational Waves. Edo Berger Harvard University
Short GRBs: Progenitors, r-process Nucleosynthesis, and Gravitational Waves Edo Berger Harvard University GWPAW 2015 Osaka, Japan June 2015 Objectives Berger 2014 Annual Reviews of Astronomy & Astrophysics,
More informationGR SIMULATIONS OF BINARY NEUTRON STARS AND BINARY BLACK HOLES WITH WHISKY. Bruno Giacomazzo University of Trento, Italy
GR SIMULATIONS OF BINARY NEUTRON STARS AND BINARY BLACK HOLES WITH WHISKY Bruno Giacomazzo University of Trento, Italy PART I: BINARY NEUTRON STAR MERGERS WHY SO INTERESTING? Due to their duration and
More informationGlobal Simulations of Black Hole Accretion. John F. Hawley Department of Astronomy, University of Virginia
Global Simulations of Black Hole Accretion John F. Hawley Department of Astronomy, University of Virginia Collaborators and Acknowledgements Julian Krolik, Johns Hopkins University Scott Noble, JHU Jeremy
More informationThis is a vast field - here are some references for further reading
This is a vast field - here are some references for further reading Dippers: Smale et al. 1988 MNRAS 232 647 Black hole transient lmxbs: Remillard and McClintock, 2006 ARAA 44, 49 Color-color diagrams
More informationThe 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
More informationThree-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
More informationAsymmetric explosion of core-collapse supernovae
Asymmetric explosion of core-collapse supernovae Rémi Kazeroni (CEA) Thierry Foglizzo (CEA), Jérôme Guilet (MPA Garching) Journées des doctorants - IRFU 01/07/2015 About me Rémi Kazeroni (IRFU/SAp) Advisor:
More informationRADIATION FROM ACCRETION ONTO BLACK HOLES
RADIATION FROM ACCRETION ONTO BLACK HOLES Accretion via MHD Turbulence: Themes Replacing dimensional analysis with physics MRI stirs turbulence; correlated by orbital shear; dissipation heats gas; gas
More informationTheoretical 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
More informationInfluence of Mass Flows on the Energy Balance and Structure of the Solar Transition Region
**TITLE** ASP Conference Series, Vol. **VOLUME***, **YEAR OF PUBLICATION** **NAMES OF EDITORS** Influence of Mass Flows on the Energy Balance and Structure of the Solar Transition Region E. H. Avrett and
More informationHow Nature makes gold
How Nature makes gold The role of isotopes for the origin of the elements Karlheinz Langanke GSI Helmholtzzentrum Darmstadt AAAS Symposium, Vancouver, February 20, 2012 Signatures of Nucleosynthesis solar
More informationNucleosynthesis in core-collapse supernovae
INT Program INT-12-2a Core-Collapse Supernovae: Models and Observable Signals Workshop: Nuclear and neutrino physics Nucleosynthesis in core-collapse supernovae Almudena Arcones Z Big Bang: H, He 20 28
More informationHirschegg 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
More informationType 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
More informationInterstellar Medium and Star Birth
Interstellar Medium and Star Birth Interstellar dust Lagoon nebula: dust + gas Interstellar Dust Extinction and scattering responsible for localized patches of darkness (dark clouds), as well as widespread
More informationBinary black-hole mergers in magnetized disks: Simulations in full general relativity
Binary black-hole mergers in magnetized disks: Simulations in full general relativity Brian D. Farris, Roman Gold, Vasileios Paschalidis, Zachariah B. Etienne, and Stuart L. Shapiro arxiv:1207.3354 University
More informationCore-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
More informationJin Matsumoto. Relativistic HD/MHD Flow for GRB Jets. RIKEN Astrophysical Big Bang Laboratory
Relativistic HD/MHD Flow for GRB Jets Jin Matsumoto RIKEN Astrophysical Big Bang Laboratory Collaborators: Nagataki, Ito, Mizuta, Barkov, Dainotti, Teraki (RIKEN), Masada (Kobe University) What a relativistic
More informationSOLAR WIND ION AND ELECTRON DISTRIBUTION FUNCTIONS AND THE TRANSITION FROM FLUID TO KINETIC BEHAVIOR
SOLAR WIND ION AND ELECTRON DISTRIBUTION FUNCTIONS AND THE TRANSITION FROM FLUID TO KINETIC BEHAVIOR JUSTIN C. KASPER HARVARD-SMITHSONIAN CENTER FOR ASTROPHYSICS GYPW01, Isaac Newton Institute, July 2010
More informationNeutron Star Mergers and Nucleosynthesis of Heavy Elements
Neutron Star Mergers and Nucleosynthesis of Heavy Elements arxiv:1710.02142v1 [astro-ph.he] 5 Oct 2017 F.-K. Thielemann 1,2, M. Eichler 3, I.V. Panov 4,5, and B. Wehmeyer 6 1 Department of Physics, University
More informationThe Bizarre Stellar Graveyard
The Bizarre Stellar Graveyard 18.1 White Dwarfs Our goals for learning: What is a white dwarf? What can happen to a white dwarf in a close binary system? What is a white dwarf? White Dwarfs White dwarfs
More informationAstronomy 421. Lecture 23: End states of stars - Neutron stars
Astronomy 421 Lecture 23: End states of stars - Neutron stars 1 Outline Neutron stars Pulsars properties distribution emission mechanism evolution 2 Neutron stars Typical values: M ~ 1.4M R ~ 10 km ρ ~
More information