Comparison of Neutrino Transport Approximations in Core-Collapse Supernova Simulations
|
|
- Edwina York
- 5 years ago
- Views:
Transcription
1 Comparison of Neutrino Transport Approximations in Core-Collapse Supernova Simulations Sherwood Richers 1 Evan O Connor 2 Christian Ott 1 1 TAPIR, California Institute of Technology 2 CITA, University of Toronto November 9, 12 Sherwood Richers Neutrino Transport Approximations November 9, 12 1/13
2 Outline Introduction: What are core-collapse supernovae? Methods: How are neutrinos approximated? Results: How do the resulting explosions differ? Conclusions: Which method is right? Sherwood Richers Neutrino Transport Approximations November 9, 12 2/13
3 Core-Collapse Supernovae Star collapses and core rebounds. Shock propagates out through infalling star. Neutrinos emitted from core heat, pressurize, and leptonize the gain region. Sherwood Richers Neutrino Transport Approximations November 9, 12 3/13
4 Core Collapse Supernovae Dominant Neutrino Processes in the core: electron capture e + p ν e + n positron capture e + + n ν e + p scattering ν l + l ν l + l in the gain region: neutrino capture ν e + n e + p anti-neutrino capture ν e + p e + + n scattering ν l + l ν l + l Neutrinos carry away energy and lepton number. Neutrinos heat, pressurize, and leptonize the gain region. Sherwood Richers Neutrino Transport Approximations November 9, 12 4/13
5 Neutrino Approximations 3-D Boltzmann Equation 1 I c t + Ω I = C(I) Neutrino Intensity Distribution I(x, Ω, ɛ, t) Full Boltzmann transport is prohibitively expensive. Study effects of individual parameters. 1-D simulations can be used to: better understand approximation effects before doing 3-D simulations. assess the predictive power of an approximation. Sherwood Richers Neutrino Transport Approximations November 9, 12 5/13
6 Neutrino Approximations Lightbulb Fixed neutrino properties Lνe = Lν e = erg/s Tνe = Tν e = 4 MeV Analytic heating, cooling, and electron fraction h i H Lνe r 2 Tν2e erg g s h i erg 6 C T g s Ye = Ye (ρ) only consider νe and ν e Sherwood Richers Neutrino Transport Approximations November 9, 12 6/13
7 Neutrino Approximations Leakage Calculate optical depth τ (r) neutrino energy and number loss rate Energy-averaged neutrino heating based on above net neutrino luminosity and neutrinosphere temperature. Considers νe, ν e, and νx Sherwood Richers Neutrino Transport Approximations November 9, 12 7/13
8 Neutrino Approximations Two-Moment Evolves the 0th (energy) and 1st (flux) moments of the neutrino distribution function with an analytic closure relation. 24 energy bins for each species νe, ν e, and νx. Currently no dependence on fluid velocity or coupling between energy groups. Sherwood Richers Neutrino Transport Approximations November 9, 12 8/13
9 Results - Neutrino Energies Eνe [MeV] E νe [MeV] Eνx [MeV] Two-Moment GR 10 Leakage Newtonian 5 Lightbulb t t bounce [ms] Lightbulb scheme does not emit ν x and assumes constant energy. Leakage energies are unreliable due to different definition of energy. Sherwood Richers Neutrino Transport Approximations November 9, 12 9/13
10 Results - Neutrino Luminosities Newt. ν-luminosity [ B s ] GR ν-luminosity [B s ] Two-Moment Leakage Lightbulb ν e ν e ν x t t bounce [ms] Lightbulb scheme does not emit ν x. Lightbulb scheme heating can be unphysical. Sherwood Richers Neutrino Transport Approximations November 9, 12 10/13
11 Results - Supernova Structure Ye T [MeV] log 10 ( ρ g cm 3 ) Two-Moment Leakage Lightbulb Radius [km] GR Newtonian Lightbulb scheme temperature differs within PNS. Lightbulb scheme electron fraction large due to Y e (ρ) prescription. Density profiles remain similar. Sherwood Richers Neutrino Transport Approximations November 9, 12 11/13
12 Results - Shock and PNS Radius R ρ=10 11 g/cm 3 [km] R shock [km] Two-Moment Leakage Lightbulb GR Newtonian t t bounce [ms] Constant input luminosity causes lightbulb scheme s shock to be larger. Lightbulb scheme s PNS is large because Y e (ρ) prescription keeps core pressure high. Sherwood Richers Neutrino Transport Approximations November 9, 12 12/13
13 Conclusions There are clear qualitative differences between the schemes. The two-moment scheme makes the fewest approximations. The leakage scheme appears to fit qualitatively with the two-moment results, but differs quantitatively. The lightbulb scheme differs qualitatively from more sophisticated schemes in many areas. Must compare to full Boltzmann or Monte Carlo transport. Sherwood Richers Neutrino Transport Approximations November 9, 12 13/13
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
More informationIs 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,
More informationIntroduction Core-collapse SN1987A Prospects Conclusions. Supernova neutrinos. Ane Anema. November 12, 2010
Supernova neutrinos Ane Anema November 12, 2010 Outline 1 Introduction 2 Core-collapse 3 SN1987A 4 Prospects 5 Conclusions Types of supernovae Figure: Classification (figure 15.1, Giunti) Supernova rates
More informationUser s Guide for Supernova Neutrino Database
User s Guide for Supernova Neutrino Database Ken ichiro Nakazato (Tokyo Univ. of Sci.) August 27, 2013 Abstract This is a guide for users of Supernova Neutrino Database for neutrino astronomy. 1 Introduction
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 informationarxiv: v1 [astro-ph.he] 23 Nov 2015
SUBMITTED TO APJ ON 15 NOVEMBER 23 Preprint typeset using LATEX style emulateapj v. 01/23/15 TWO DIMENSIONAL CORE-COLLAPSE SUPERNOVA EXPLOSIONS AIDED BY GENERAL RELATIVITY WITH MULTIDIMENSIONAL NEUTRINO
More informationSupernovae SN1987A OPERA Constraints on neutrino parameters. Supernova neutrinos. Ly Duong. January 25, 2012
January 25, 2012 Overview Supernovae Supernovae Supernova types Core collapse model Neutrino properties Detection of neutrinos Data and analysis Experiment results Comparison with results Possible neutrino
More informationNeutrinos 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
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 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 informationNeutrinos from Black Hole Accretion Disks
Neutrinos from Black Hole Accretion Disks Gail McLaughlin North Carolina State University General remarks about black hole accretion disks Neutrinos and nucleosynthesis - winds Neutrino flavor transformation
More informationEquation of State Dependence of Gravitational Waves from Core-Collapse Supernovae
Equation of State Dependence of Gravitational Waves from Core-Collapse Supernovae Sherwood Richers California Institute of Technology NSF Blue Waters Graduate Fellow Christian Ott, Ernazar Abdikamalov
More informationDetection of Gravitational Waves and Neutrinos from Astronomical Events
Detection of Gravitational Waves and Neutrinos from Astronomical Events Jia-Shu Lu IHEP,CAS April 18, 216 JUNO Neutrino Astronomy and Astrophysics Seminar 1 / 24 Outline Sources of both GW and neutrinos.
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 informationNeutrino 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
More informationNeutrinos Probe Supernova Dynamics
Neutrinos Probe Supernova Dynamics Irene Tamborra GRAPPA Institute, University of Amsterdam Rencontres de Moriond, EW Interactions and Unified Theories La Thuile, March 18, 2014 Outline Supernova explosion
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 informationImproving gradient evaluation in Smoothed Particle Hydrodynamics
Improving gradient evaluation in Smoothed Particle Hydrodynamics Domingo García Senz José A. Escartín Antonio Relaño Ruén M. Caezón Alino Perego Matthias Lieendörfer Gradients in SPH < f r > = f r W r
More informationNuclear 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
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 informationSpectrum 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
More informationSupernova neutrinos and their implications for supernova physics
Supernova neutrinos and their implications for supernova physics Ken ichiro Nakazato (Tokyo University of Science) in collaboration with H. Suzuki(Tokyo U of Sci.), T. Totani, H. Umeda(U of Tokyo), K.
More informationGravitational Waves from Supernova Core Collapse: What could the Signal tell us?
Outline Harald Dimmelmeier harrydee@mpa-garching.mpg.de Gravitational Waves from Supernova Core Collapse: What could the Signal tell us? Work done at the MPA in Garching Dimmelmeier, Font, Müller, Astron.
More informationHow 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
More informationIdentifying the neutrino mass hierarchy with supernova neutrinos
Identifying the neutrino mass hierarchy with supernova neutrinos Ricard Tomàs AHEP Group - Institut de Física Corpuscular (CSIC - Universitat de València) IPM School & Conference on Lepton & Hadron Physics
More informationThe Ledoux Criterion for Convection in a Star
The Ledoux Criterion for Convection in a Star Marina von Steinkirch, steinkirch@gmail.com State University of New York at Stony Brook August 2, 2012 Contents 1 Mass Distribution and Gravitational Fields
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 informationSupernova 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
More informationCore- Collapse Supernova Neutrinos. Evan O Connor with Chris7an O8 INT 12-2A Workshop 1 July 2-6, 2012
Core- Collapse Supernova Neutrinos Evan O Connor with Chris7an O8 INT 12-2A Workshop 1 July 2-6, 2012 Overview NuLib! Mo7va7on Current Status Core- Collapse Supernovae: Models and Observable Signals: From
More informationGravitational waves from proto-neutron star evolution
Gravitational waves from proto-neutron star evolution Giovanni Camelio in collaboration with: Leonardo Gualtieri, Alessandro Lovato, Jose A. Pons, Omar Benhar, Morgane Fortin & Valeria Ferrari PhD student
More informationNeutrino Signature from Multi-D Supernova Models
Neutrino Signature from Multi-D Supernova Models David Radice 1,2 A. Burrows, J. C. Dolence, S. Seadrow, M. A. Skinner, D. Vartanyan, J. Wallace 1 Research Associate, Princeton University 2 Schmidt Fellow,
More informationNeutrinos in Supernova Evolution and Nucleosynthesis
Neutrinos in Supernova Evolution and Nucleosynthesis Gabriel Martínez Pinedo The origin of cosmic elements: Past and Present Achievements, Future Challenges, Barcelona, June 12 15, 2013 M.-R. Wu, T. Fischer,
More informationRe-research on the size of proto-neutron star in core-collapse supernova
Vol 17 No 3, March 2008 c 2008 Chin. Phys. Soc. 1674-1056/2008/17(03)/1147-05 Chinese Physics B and IOP Publishing Ltd Re-research on the size of proto-neutron star in core-collapse supernova Luo Zhi-Quan(
More informationNeutrinos and Supernovae
Neutrinos and Supernovae Introduction, basic characteristics of a SN. Detection of SN neutrinos: How to determine, for all three flavors, the flux and temperatures. Other issues: Oscillations, neutronization
More informationNew 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
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 informationGeneral-Relativistic Simulations of Stellar Collapse and The Formation of Stellar-Mass Black Holes
General-Relativistic Simulations of Stellar Collapse and The Formation of Stellar-Mass Black Holes Christian D. Ott, TAPIR, Caltech cott@tapir.caltech.edu Work in Collaboration with: Evan O Connor, Fang
More informationAstroparticle physics
Timo Enqvist University of Oulu Oulu Southern institute lecture cource on Astroparticle physics 15.09.2009 15.12.2009 Supernovae and supernova neutrinos 4.1 4 Supernovae and supernova neutrinos 4.1 Supernova
More informationMulti-Dimensional Core-Collapse Supernova Simulations with the IDSA for Neutrino Transport
F.O.E Conference June 3rd, 2015 Raleigh NC Multi-Dimensional Core-Collapse Supernova Simulations with the IDSA for Neutrino Transport Kuo-Chuan Pan Universität Basel, Switzerland (arxiv:1505.02513) The
More informationNeutrino Emission from Nearby Supernova Progenitors
Neutrino Emission from Nearby Supernova Progenitors Takashi Yoshida Yukawa Institute for Theoretical Physics, Kyoto University Koh Takahashi, Hideyuki Umeda Department of Astronomy, University of Tokyo
More informationGalactic Supernova for neutrino mixing and SN astrophysics
Galactic Supernova for neutrino mixing and SN astrophysics Amol Dighe Tata Institute of Fundamental Research Mumbai NNN05, Aussois, France, April 7-9, 2005 Galactic Supernova forneutrino mixing and SN
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 informationCore-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
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 informationSovan Chakraborty. MPI for Physics, Munich
Neutrino Mass Hierarchy from Supernova Neutrinos Sovan Chakraborty MPI for Physics, Munich Outline Supernova (SN) as Neutrino Source Oscillation of SN Neutrinos Signatures of Neutrino Mass Hierarchy Conclusions
More informationNeutrino-Driven Convection and Neutrino-Driven Explosions
Neutrino-Driven Convection and Neutrino-Driven Explosions by Jeremiah W. Murphy (Princeton U.) Collaborators: Adam Burrows (Princeton U.), Josh Dolence (Princeton U.) & Casey Meakin (U. Arizona) 1D simulations
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 informationLife 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
More informationNeutrinos Must be Tachyons
Neutrinos Must be Tachyons Eue Jin Jeong Department of Physics, The University of Texas at Austin, Austin, TX 78712 Abstract The negative mass squared problem of the recent neutrino experiments[1-6] prompts
More informationNeutrino-Driven Convection and Neutrino-Driven Explosions
Neutrino-Driven Convection and Neutrino-Driven Explosions by Jeremiah W. Murphy (Princeton U.) Collaborators: Adam Burrows (Princeton U.), Josh Dolence (Princeton U.) & Casey Meakin (LANL) 1D simulations
More informationTheory of core-collapse supernovae
Theory of core-collapse supernovae H.-Th. Janka 1, K. Langanke 2,3, A. Marek 1, G. Martínez-Pinedo 2, B. Müller 1 1 Max-Planck Institut für Astrophysik, Garching, Germany 2 Gesellschaft für Schwerionenforschung,
More informationProgress 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
More informationarxiv:astro-ph/ v1 20 Sep 2006
Formation of Neutrino Stars from Cosmological Background Neutrinos M. H. Chan, M.-C. Chu Department of Physics, The Chinese University of Hong Kong, Shatin, New Territories, Hong Kong, China arxiv:astro-ph/0609564v1
More informationNumerical 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
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 informationRelativistic Mean Field Model for finite nuclei and infinite matter
Relativistic Mean Field Model for finite nuclei and infinite matter Hiroshi Toki (RCNP/Osaka) in collaboration with H. Shen (Nankai/China) L. Geng (Beijing/China) K. Sumiyoshi (Numazu) Supernova explosion
More informationGENERALIZED DENSITY FUNCTIONAL EQUATION OF STATE FOR SUPERNOVA & NEUTRON STAR SIMULATIONS MacKenzie Warren J.P. Olson, M. Meixner, & G.
GENERALIZED DENSITY FUNCTIONAL EQUATION OF STATE FOR SUPERNOVA & NEUTRON STAR SIMULATIONS MacKenzie Warren J.P. Olson, M. Meixner, & G. Mathews Symposium on Neutron Stars in the Multimessenger Era Ohio
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 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 informationExplosion 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
More informationStars AS4023: Stellar Atmospheres (13) Stellar Structure & Interiors (11)
Stars AS4023: Stellar Atmospheres (13) Stellar Structure & Interiors (11) Kenneth Wood, Room 316 kw25@st-andrews.ac.uk http://www-star.st-and.ac.uk/~kw25 What is a Stellar Atmosphere? Transition from dense
More informationProton decay and neutrino astrophysics with the future LENA detector
Proton decay and neutrino astrophysics with the future LENA detector Teresa Marrodán Undagoitia tmarroda@ph.tum.de Institut E15 Physik-Department Technische Universität München Paris, 11.09.08 Outline
More informationEnergy and momentum losses in the process of neutrino scattering on plasma electrons with the presence of a magnetic field.
Energy and momentum losses in the process of neutrino scattering on plasma electrons with the presence of a magnetic field. Nickolay V. Mikheev and Elena N. Narynskaya Division of Theoretical Physics,
More informationNeutrino 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
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 information3D Simulations of Core-collapse Supernovae. Tomoya Takiwaki(NAOJ) Kei Kotake(Fukuoka U) Yudai Suwa(YITP) Tomohide Wada(vis) And many collaborators
2013/12/3 MMCOCOS@Fukuoka University 3D Simulations of Core-collapse Supernovae Tomoya Takiwaki(NAOJ) Kei Kotake(Fukuoka U) Yudai Suwa(YITP) Tomohide Wada(vis) And many collaborators Plan 1. Brief summary
More informationNeutrinos, nonzero rest mass particles, and production of high energy photons Particle interactions
Neutrinos, nonzero rest mass particles, and production of high energy photons Particle interactions Previously we considered interactions from the standpoint of photons: a photon travels along, what happens
More informationSupernova theory: simulation and neutrino fluxes
Supernova theory: simulation and neutrino fluxes K G Budge 1, C L Fryer and A L Hungerford CCS-2, Los Alamos National Laboratory 2 M.S. D409, Los Alamos National Laboratory, Los Alamos, New Mexico, 87545,
More informationNeutrinos and Nucleosynthesis
Neutrinos and Nucleosynthesis The effect of neutrinos on nucleosynthesis in core-collapse supernovae Franziska Treffert (Matrikelnummer: 2044556) Seminar zur Kernstruktur und nuklearen Astrophysik Prof.
More informationSupernova Neutrino Directionality
Supernova Neutrino Directionality Fan Zhang April 25, 2016 Subject: Senior Thesis Date Performed: Jan 2015 to Apr 2016 Instructor: Prof. Kate Scholberg Defense Committee: Prof. Kate Scholberg Prof. Roxanne
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 informationStrange nuclear matter in core-collapse supernovae
Strange nuclear matter in core-collapse supernovae I. Sagert Michigan State University, East Lansing, Michigan, USA EMMI Workshop on Dense Baryonic Matter in the Cosmos and the Laboratory Tuebingen, Germany
More informationSterile Neutrinos in Cosmology and Astrophysics
Kalliopi Petraki (UCLA) October 27, 2008 Particle Physics Neutrino Oscillation experiments: neutrinos have mass Cosmology and Astrophysics Plenty of unexplained phenomena Dark Matter Pulsar Kicks Supernova
More informationProf. dr. A. Achterberg, Astronomical Dept., IMAPP, Radboud Universiteit
Prof. dr. A. Achterberg, Astronomical Dept., IMAPP, Radboud Universiteit Shocks occur in supersonic flows; Shocks are sudden jumps in velocity, density and pressure; Shocks satisfy flux in = flux out principle
More informationGravitational Waves from Supernova Core Collapse: Current state and future prospects
Gravitational Waves from Core Collapse Harald Dimmelmeier harrydee@mpa-garching.mpg.de Gravitational Waves from Supernova Core Collapse: Current state and future prospects Work done with E. Müller (MPA)
More informationExplosion Mechanism, Neutrino Burst, and Gravitational Wave in Core-Collapse Supernovae
Explosion Mechanism, Neutrino Burst, and Gravitational Wave in Core-Collapse Supernovae Kei Kotake, Katsuhiko Sato, and Keitaro Takahashi Science & Engineering, Waseda University, 3-4-1 Okubo, Shinjuku,
More informationProf. dr. A. Achterberg, Astronomical Dept., IMAPP, Radboud Universiteit
Prof. dr. A. Achterberg, Astronomical Dept., IMAPP, Radboud Universiteit Shocks occur in supersonic flows; Shocks are sudden jumps in velocity, density and pressure; Shocks satisfy flux in = flux out principle
More informationGalaxies 626. Lecture 5
Galaxies 626 Lecture 5 Galaxies 626 The epoch of reionization After Reionization After reionization, star formation was never the same: the first massive stars produce dust, which catalyzes H2 formation
More information6. Cosmology. (same at all points) probably true on a sufficiently large scale. The present. ~ c. ~ h Mpc (6.1)
6. 6. Cosmology 6. Cosmological Principle Assume Universe is isotropic (same in all directions) and homogeneous (same at all points) probably true on a sufficiently large scale. The present Universe has
More informationNeutrino Oscillations in Core-Collapse Supernovae
Neutrino Oscillations in Core-Collapse Supernovae Meng-Ru Wu, Technische Universität Darmstadt Supernovae and Gamma-Ray Bursts 2013 10/14/2013-11/15/2013 Neutrino Oscillations in Core-Collapse Supernovae
More informationLecture 13. Presupernova Models, Core Collapse and Bounce
Lecture 13 Presupernova Models, Core Collapse and Bounce Generalities When Massive Stars Die, How Do They Explode? Black hole Neutron Star + Neutrinos Neutron Star + Rotation Colgate and White (1966) Arnett
More informationPhase Oscillation between Superfluid and Normal State of Neutrons in Neutron Stars The Origin of Glitches of Pulsars 1
Phase Oscillation between Superfluid and Normal State of Neutrons in Neutron Stars The Origin of Glitches of Pulsars Qiu-he Peng a,b ( qhpeng@nju.edu.cn ) Zhi quan Luo a,c a School of Physics and electronic
More informationQuark Nugget Dark Matter. Kyle Lawson May 15, 2017
Quark Nugget Dark Matter Kyle Lawson May 15, 2017 Outline High density QCD and quark matter Compact composite dark matter Baryogenesis as separation of charges Observational constraints High density QCD
More informationIf light travels past a system faster than the time scale for which the system evolves then t I ν = 0 and we have then
6 LECTURE 2 Equation of Radiative Transfer Condition that I ν is constant along rays means that di ν /dt = 0 = t I ν + ck I ν, (29) where ck = di ν /ds is the ray-path derivative. This is equation is the
More informationSupernovae represent the catastrophic death of certain stars. They are among the most violent events in the Universe,
Chapter 20 Supernovae Supernovae represent the catastrophic death of certain stars. They are among the most violent events in the Universe, They typically produce about 10 53 erg, with a large fraction
More informationBlack Holes ASTR 2110 Sarazin. Calculation of Curved Spacetime near Merging Black Holes
Black Holes ASTR 2110 Sarazin Calculation of Curved Spacetime near Merging Black Holes Test #2 Monday, November 13, 11-11:50 am Ruffner G006 (classroom) Bring pencils, paper, calculator You may not consult
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 informationAST 301 Introduction to Astronomy
AST 301 Introduction to Astronomy John Lacy RLM 16.332 471-1469 lacy@astro.as.utexas.edu Myoungwon Jeon RLM 16.216 471-0445 myjeon@astro.as.utexas.edu Bohua Li RLM 16.212 471-8443 bohuali@astro.as.utexas.edu
More informationSupernovae represent the catastrophic death of certain stars. They are among the most violent events in the Universe,
Chapter 14 Supernovae Supernovae represent the catastrophic death of certain stars. They are among the most violent events in the Universe, They typically produce about 10 53 erg, with a large fraction
More informationNew Supernova Constraints on Sterile Neutrino Production
UMD-PP-96-93 SMU-PHYS-96-02 FERMILAB Pub 96-096-A hep-ph/9605350 May, 1996 arxiv:hep-ph/9605350v1 18 May 1996 New Supernova Constraints on Sterile Neutrino Production Edward W. Kolb, a Rabindra N. Mohapatra,
More informationarxiv: v3 [astro-ph.sr] 26 Jun 2014
Draft version June 7, 1 Preprint typeset using L A TEX style emulateapj v. 5//11 A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMICS CODE FOR CORE-COLLAPSE SUPERNOVAE IV. THE NEUTRINO SIGNAL
More informationFast-time variations of supernova neutrino fluxes and detection perspectives
Fast-time variations of supernova neutrino fluxes and detection perspectives Irene Tamborra GRAPPA Institute, University of Amsterdam Xmas Workshop 2013 Bari, December 23, 2013 Outline Supernova explosion
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 informationImplicit Lagrangian method on variable triangular grid for magnetorotational supernova simulations Sergey Moiseenko
Implicit Lagrangian method on variable triangular grid for magnetorotational supernova simulations Sergey Moiseenko Space Research Institute, Moscow, Russia Basic equations: MHD +self-gravitation, infinite
More informationApplications of nuclear physics in neutrino physics
Applications of nuclear physics in neutrino physics Emanuel Ydrefors E. Ydrefors (KTH) Neutrino physics 1 / 16 Outline of lecture Brief introduction to neutrinos Nuclear beta decay Neutrino-nucleus scattering
More informationPULSAR 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
More informationLecture 14. Neutrino-Powered Explosions Mixing, Rotation, and Making Black Holes
Lecture 14 Neutrino-Powered Explosions Mixing, Rotation, and Making Black Holes Baade and Zwicky, Proceedings of the National Academy of Sciences, (1934) With all reserve we advance the view that a supernova
More informationSupernova Evolution and Explosive Nucleosynthesis
Supernova Evolution and Explosive Nucleosynthesis Gabriel Martínez Pinedo 5 th European Summer School On Experimental Nuclear Astrophysics Santa Tecla, September 25, 2009 Outline 1 Introduction 2 Electron
More informationPHAS3135 The Physics of Stars
PHAS3135 The Physics of Stars Exam 2013 (Zane/Howarth) Answer ALL SIX questions from Section A, and ANY TWO questions from Section B The numbers in square brackets in the right-hand margin indicate the
More informationSupernova Neutrinos in Future Liquid-Scintillator Detectors
Supernova Neutrinos in Future Liquid-Scintillator Detectors Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 9, China E-mail: liyufeng@ihep.ac.cn A high-statistics measurement of
More information