Gravitational SIGNATURE of Core-Collapse Supernovae

Slides:

Advertisements

Similar presentations

Neutron Stars: Insights into their Formation, Evolution & Structure from their Masses and Radii Feryal Ozel University of Arizona In collaboration with.

Advertisements

Inspiraling Compact Objects: Detection Expectations

Numerical Relativity & Gravitational waves I.Introduction II.Status III.Latest results IV.Summary M. Shibata (U. Tokyo)

Compact remnant mass function: dependence on the explosion mechanism and metallicity Reporter: Chen Wang 06/03/2014 Fryer et al. 2012, ApJ, 749, 91.

Neutrino oscillations in oxygen-neon-magnesium supernovae Cecilia Lunardini Arizona State University And RIKEN-BNL Research Center C.L., B. Mueller and.

The evolution and collapse of BH forming stars Chris Fryer (LANL/UA)  Formation scenarios – If we form them, they will form BHs.  Stellar evolution:

Current status of numerical relativity Gravitational waves from coalescing compact binaries Masaru Shibata (Yukawa Institute, Kyoto University)

Brendan Krueger CEA Saclay 2013 October 18 THE ONSET OF NEUTRINO- DRIVEN CONVECTION IN CORE-COLLAPSE SUPERNOVAE.

Neutron Star Formation and the Supernova Engine Bounce Masses Mass at Explosion Fallback.

Neutrinos from Stellar Collapse Chris Fryer (LANL/UNM) “Normal” Core Collapse: Collapse and Bounce, Fallback and Cooling More massive Stars Low Mass Stars.

The Death of Massive Stars and the Birth of the Elements Stan Woosley Cornell, June 2, 2006.

Core-collapse SN neutrinos and GW bursts We are developing a proposal to the LSC-Virgo to search for associated bursts of low-energy neutrinos and GW bursts.

Günter Sigl, Astroparticules et Cosmologie, ParisILIAS/N5-N6 meeting, Paris, January 23-24, 2006  Supernovae as neutrino and gravitational wave sources.

1 07/10/ Séminaire du LUTh - Jérôme Guilet Asymmetric explosions of Core collapse supernovae Jérôme Guilet En collaboration avec Thierry Foglizzo,

The Astrophysics of Gravitational Wave Sources Conference Summary: Ground-Based Detectors ( Hz) Kimberly New, LANL.

From Supernovae to Neutron Stars

SUPERNOVA NEUTRINOS AT ICARUS

Massive star evolution convection semiconvection overshoot angular momentum transport with and without B-field torques nucleosynthesis presupernova models.

Collapse of rapidly rotating massive stellar core to a black hole in full GR Tokyo institute of technology Yu-ichirou Sekiguchi University of Tokyo Masaru.

Gravitational waves and neutrino emission from the merger of binary neutron stars Kenta Kiuchi Collaboration with Y. Sekiguchi, K. Kyutoku, M. Shibata.

Targeted Supernova Search with Coherent Wave Burst M. Zanolin (ERAU), L. Corpuz (ERAU), and the cWB Team LSC Burst Face to Face – Krakow, Poland 2010.

Frontiers of GW predictions from CCSN Model Takami Kuroda (Basel Univ.) Kei Kotake(Fukuoka Univ.), Tomoya Takiwaki(NAOJ), Ko Nakamura (Waseda Univ.), Kazuhiro.

THERMAL EVOLUION OF NEUTRON STARS: Theory and observations D.G. Yakovlev Ioffe Physical Technical Institute, St.-Petersburg, Russia Catania, October 2012,

Exploding Massive Stars: The Perfect ‘App’ for Computational Physics SESAPS 2003 John M. Blondin North Carolina State University.

Collapsar Accretion and the Gamma-Ray Burst X-Ray Light Curve Chris Lindner Milos Milosavljevic, Sean M. Couch, Pawan Kumar.

June 29 San FranciscoSciDAC 2005 Terascale Supernova Initiative Discovering New Dynamics of Core-Collapse Supernova Shock Waves John M. Blondin NC State.

Lecture 14 Neutrino-Powered Explosions Mixing, Rotation, and Making Black Holes.

Abel, Bryan, and Norman, (2002), Science, 295, 5552 density molecular cloud analog (200 K) shock 600 pc.

Numerical relativity simulation with Microphysics National Astronomical Observatory of Japan Yuichiro Sekiguchi Masaru Shibata (YITP) Kenta Kiuchi (YITP)

Phase transition induced collapse of Neutron stars Kim, Hee Il Astronomy Program, SNU 13th Haengdang Symposium, 11/30/2007.

Supernova neutrino challenges Christian Y. Cardall Oak Ridge National Laboratory Physics Division University of Tennessee, Knoxville Department of Physics.

TeraScale Supernova Initiative: A Networker’s Challenge 11 Institution, 21 Investigator, 34 Person, Interdisciplinary Effort.

11/01/2016 Variable Galactic Gamma-Ray Sources, Heidelberg, Germany 1 Maxim Barkov MPI-K, Heidelberg, Germany Space Research Institute, Russia, University.

Core Collapse Supernovae: Power Beyond Imagination

Neutron Star Kicks Chris Fryer Aimee Hungerford Frank Timmes  Observational Evidence and constraints on kicks  Theoretical kick mechanisms.

LIGO- G Z August 17, 2005August LSC Meeting – ASIS Session 1 Recovering Hardware Injection Waveforms with Maximum Entropy Tiffany Summerscales.

Magneto-hydrodynamic Simulations of Collapsars Shin-ichiro Fujimoto (Kumamoto National College of Technology), Collaborators: Kei Kotake(NAOJ), Sho-ichi.

Oct. 30, 2002Source Simulation & Data Analysis1 Gravitational-Wave Observations of Galactic Populations of Compact Binaries M. Benacquista Montana State.

LIGO- G Z March 23, 2005March LSC Meeting – ASIS Session 1 Extracting Supernova Information from a LIGO Detection Tiffany Summerscales Penn State.

Formation of BH-Disk system via PopIII core collapse in full GR National Astronomical Observatory of Japan Yuichiro Sekiguchi.

Neutrino Studies at the Spallation Neutron Source, ORNL, 8/29/03W.R. Hix (UTenn./ORNL) Neutrino-Nucleus Interactions and the Core Collapse Supernova Mechanism.

Christian Y. Cardall Oak Ridge National Laboratory Physics Division University of Tennessee, Knoxville Department of Physics and Astronomy Terascale Supernova.

January 12, 2006Sources & Simulations 1 LIGO Supernova Astronomy with Maximum Entropy Tiffany Summerscales Penn State University.

January 9, 2007AAS/AAPT John M. Blondin NC State University Discovering the Complexity of Supernovae through 3D Simulations.

A Model for GW Emission from CCSN Explosions by Jeremiah W. Murphy NSF AAP Fellow (University of Washington) Collaborators: Christian Ott (Caltech), Adam.

The Critical Neutrino Luminosity and its Observational Signatures Ondřej Pejcha with Todd Thompson, Christopher Kochanek, Basudeb Dasgupta Department of.

Regression Testing for CHIMERA Jessica Travierso Austin Peay State University Bronson Messer National Center for Computational Sciences August 2009.

Waseda univ. Yamada lab. D1 Chinami Kato

Supernova Neutrinos Physics Opportunities with Flavor Oscillations

Detecting a Galactic Supernova with H2 or GEO

Detecting a Galactic Supernova with H2 or GEO

Core Collapse Supernovae and Neutron Star Kicks

International School of Nuclear Physics 39th Course, Erice-Sicily, Sep

Stellar core collapse with QCD phase transition

Rebecca Surman Union College

A New Type of Thermonuclear Supernova, and How the Pulsar Got his Spin

Short-Duration Gamma-Ray Burst Central Engines

Anthony Mezzacappa (ORNL) Computational Methods in Transport

Non-Standard Interactions and Neutrino Oscillations in Core-Collapse Supernovae Brandon Shapiro.

Theoretical Astrophysics Group

Travis Hansen, Marek Szczepanczyk, Michele Zanolin

Supernova Neutrinos Christian Y. Cardall Oak Ridge National Laboratory

Neutrinos and the deaths of Massive Stars

No BH at the GC and Supernova Explosion Driven by Magnetic Molopoles

Impact of electro-weak processes in Type II Supernovae collapse

The neutrino mass hierarchy and supernova n

ACRES Final Presentation July 25, 2018

Recovering Hardware Injection Waveforms with Maximum Entropy

Equation of State for Hadron-Quark Mixed Phase and Stellar Collapse

Center for Computational Physics

Presentation transcript:

Gravitational SIGNATURE of Core-Collapse Supernovae Konstantin Yakunin (Florida Atlantic University) In collaboration with S. Bruenn (FAU), P. Marronetti (FAU), A. Mezzacappa (ORNL-UTK) and the CHIMERA Team (ORNL-FAU-NCSU) GWPAW, Millowakee November 13, 2018

Funded by Blondin Warren Bruenn Dirk Marronetti Fuller Yakunin Budiardja Cardall Endeve Hix Lentz Messer Mezzacappa Parete-Koon Funded by Collaborators Solvers: D’Azevedo Data Management: Barreto, Canon, Klasky, Podhorszki Networking: Beck, Moore, Rao Visualization: Ahern, Daniel, Ma, Meredith, Pugmire, Toedte Cray Center of Excellence: Levesque, Wichmann GWPAW, Millowakee November 13, 2018

How is the SN shock revived? Known, Potentially Important Ingredients Gravity Neutrino Heating Convection Shock Instability Nuclear Burning Rotation Magnetic Fields Need 3D models with all of the above, treated with sufficient realism. GWPAW, Millowakee November 13, 2018

CHIMERA Bruenn et al., Journ. Phys. Conf. Ser., 180, 012018 (2009) “RbR-Plus” MGFLD Neutrino Transport O(v/c), GR time dilation and redshift, GR aberration (in flux limiter) 2D PPM Hydrodynamics adaptive radial grid Lattimer-Swesty EOS Cooperstein et al. for low densities Nuclear (Alpha) Network 14 alpha nuclei between helium and zinc 2D Effective Gravitational Potential Marek et al. A&A, 445, 273 (2006) GR time dilation, effective gravitational potential, “Ray-by-Ray-Plus” Approximation Radial transport allowed. Lateral transport suppressed. Buras et al. A&A, 447, 1049 (2003) GWPAW, Millowakee November 13, 2018

15 M Progenitor collapse in 2D GWPAW, Millowakee November 13, 2018

GWPAW, Millowakee November 13, 2018

Murphy, Ott, and Burrows, Ap.J. 707, 1173 (2009) CHIMERA simulation for 15 M progenitor GWPAW, Millowakee November 13, 2018

Effective GR potential & LS EoS Gravitational WAVE Murphy, Ott, and Burrows (2009) CHIMERA Newtonian potential & Shen EoS Effective GR potential & LS EoS GWPAW, Millowakee November 13, 2018

Gravitational WAVE Marek and Janka (2009) CHIMERA simulation GWPAW, Millowakee November 13, 2018

Gravitational Wave extraction Neutrinos Epstein-Müller approximation R - distance from the source to the observer θ, φ - direction angles of neutrino emission in observer’s frame dLν/dΩ - direction dependent neutrino luminosity GWPAW, Millowakee November 13, 2018

GW from Neutrino emission GWPAW, Millowakee November 13, 2018

TracER PARTICLE METHOD Heger 15 model: 5000 particles = 40 per row X 125 rows Post-bounce time = 0 ms Post-bounce time = 5 ms Post-bounce time = 157 ms GWPAW, Millowakee November 13, 2018

TRAcER ANALYSIS Low frequency component of early signal (tb<100 ms) produced by deflection of infalling matter through the shock GWPAW, Millowakee November 13, 2018

Detectability by ADV. ligo CHIMERA simulation for 15 M progenitor GWPAW, Millowakee November 13, 2018

Conclusions 2D simulations of core-collapse SN show sustained explosions for a range of non-rotating progenitors There is qualitative agreement between several groups on the main characteristics of the GW signals from 2D Core Collapse Supernovae simulations Galactic event detection by AdvLIGO will provide unique insights of the collapse dynamics and proto-neutron star structure 3D simulations are necessary for the complete realistic GW waveforms GWPAW, Millowakee November 13, 2018