Nuclear astrophysics with binary neutron stars
|
|
- Cody Hancock
- 5 years ago
- Views:
Transcription
1 Nuclear astrophysics with binary neutron stars Luciano Rezzolla Institute for Theoretical Physics, Frankfurt Frankfurt Institute for Advanced Studies, Frankfurt Nuclear Astrophysics in Germany: A Community Meeting Darmstadt, 15-1 November 01
2 Plan of the talk EOS information from GW signal Nucleosynthesis: quasi-circular and eccentric binaries Electromagnetic counterparts
3 The two-body problem in GR For BHs we know what to expect: BH + BH BH + GWs For NSs the question is more subtle: the merger leads to an hyper-massive neutron star (HMNS), ie a metastable equilibrium: NS + NS HMNS +...? BH + torus +...? BH HMNS phase can provide clear information on EOS Abbott+ 01 artist impression (NASA) Wex 01 BH+torus system may tell us on the central engine of GRBs
4 Broadbrush picture proto-magnetar? FRB?
5 merger HMNS BH + torus Quantitative differences are produced by: total mass (prompt vs delayed collapse) mass asymmetries (HMNS and torus) soft/stiff EOS (inspiral and post-merger) magnetic fields (equil. and EM emission) radiative losses (equil. and nucleosynthesis)
6 How to constrain the EOS
7 Anatomy of the GW signal binary black holes
8 Anatomy of the GW signal 8 h+ 10 [50 Mpc] 0 GNH3, M =1.350M t [ms]
9 Anatomy of the GW signal 8 h+ 10 [50 Mpc] 0 GNH3, M =1.350M t [ms] Inspiral: well approximated by PN/EOB; tidal effects important
10 Anatomy of the GW signal 8 h+ 10 [50 Mpc] 0 GNH3, M =1.350M t [ms] Merger: highly nonlinear but analytic description possible
11 Anatomy of the GW signal 8 h+ 10 [50 Mpc] 0 GNH3, M =1.350M t [ms] post-merger: quasi-periodic emission of bar-deformed HMNS
12 Anatomy of the GW signal 8 h+ 10 [50 Mpc] 0 GNH3, M =1.350M t [ms] Collapse-ringdown: signal essentially shuts off.
13 Anatomy of the GW signal 8 clean peak at high freqs Chirp signal (track from low to high frequencies) h+ 10 [50 Mpc] 0 8 transient (messy but short) GNH3, M =1.350M t [ms] Cut off (very high freqs)
14 é 1 1ê and Hf h L SSn nhf fl and f»hf HfL» In frequency space Effects of EOS as neutron stars merge effec O G I L l a i Init tivel y po int-p artic le NS-NS merger tidans-ns NS NS EOS BH HB EOS HB l effebh cts BH-BH merger AdvancedLIGO Mpc post merger Einstein Teles co p e ff HHzL Hz courtesy of Jocelyn Read
15 Extracting information from EOS Takami, LR, Baiotti (01, 015), LR+ (01) 1.0 APR 0 M =1.75M M =1.300M M =1.35M M =1.350M M =1.375M ALF 0 M =1.5M M =1.50M M =1.75M M =1.300M M =1.35M h+ 10 [50 Mpc] SLy M =1.50M M =1.75M M =1.300M M =1.35M M =1.350M H M =1.50M M =1.75M M =1.300M M =1.35M M =1.350M GNH3 M =1.50M M =1.75M M =1.300M M =1.35M M =1.350M t [ms]
16 Extracting information from EOS Takami, LR, Baiotti (01, 015), LR+ (01) APR M =1.75M M =1.300M M =1.35M M =1.350M M =1.375M ALF M =1.5M M =1.50M M =1.75M M =1.300M M =1.35M log [ h(f) f 1/ ] [ Hz 1/, 50 Mpc ] SLy H M =1.50M M =1.75M M =1.300M M =1.35M M =1.350M M =1.50M M =1.75M M =1.300M M =1.35M M =1.350M There are lines! Logically not different from 1.5 M =1.50M M =1.75M M =1.300M M =1.35M M =1.350M.0 GNH3 emission lines from stellar atmospheres..5 adligo 3.0 This is GW spectroscopy! 3.5 ET f [khz]
17 A new approach to constrain the EOS Oechslin+007, Baiotti+008, Bauswein+ 011, 01, Stergioulas+ 011, Hotokezaka+ 013, Takami 01, 015, Bernuzzi 01, 015, Bauswein+ 015, LR+01 merger frequency
18 A new approach to constrain the EOS Oechslin+007, Baiotti+008, Bauswein+ 011, 01, Stergioulas+ 011, Hotokezaka+ 013, Takami 01, 015, Bernuzzi 01, 015, Bauswein+ 015, LR+01
19 Quasi-universal behaviour: inspiral log 10 [ ( M/M )(fmax/hz) ] APR ALF SLy H GNH3 LS0 Eq. (), Takami et al. (01) Eq. (15) Eq. (), Read et al. (013) Read et al. (013) Bernuzzi et al. (01) apple T surprising result: quasiuniversal behaviour of GW frequency at amplitude peak (Read+013) Many other simulations have confirmed this (Bernuzzi+, 01, Takami+, 015, LR+01). Quasi-universal behaviour in the inspiral implies that once fmax is measured, so is tidal deformability, hence I, Q, M/R = M 5 = 1 3 applet tidal deformability or Love number
20 Quasi-universal behaviour: post-merger We have found quasi- Eq. (5) in Takami et al. 015 universal behaviour: i.e., f1 [khz].5.0 APR ALF SLy H GNH3 LS0 the properties of the spectra are only weakly dependent on the EOS. This has profound implications for the 1.5 Dietrich et al. 015 Foucart et al. 015 analytical modelling of the GW emission: what we M/ R do for one EOS can be extended to all EOSs.
21 Quasi-universal behaviour: post-merger 3.0 f,i [khz] Eq. () Correlations with Love number found also for high frequency peak f f [khz].5 APR ALF SLy H GNH3 LS0 Eq. (3) apple T apple T Correlations also with compactness These other correlations are weaker but equally useful.
22 An example: start from equilibria Assume that the GW signal from a binary NS is detected and with a SNR high enough that the two peaks are clearly measurable. Consider your best choices as candidate EOSs
23 An example: use the M(R,f1) relation The measure of the f1 peak will fix a M(R,f1) relation and hence a single line in the (M, R) plane. All EOSs will have one constraint (crossing).
24 An example: use the M(R,f) relations The measure of the f peak will fix a relation M(R,f,EOS) for each EOS and hence a number of lines in the (M, R) plane. The right EOS will have three different constraints (APR, GNH3, SLy excluded)
25 An example: use measure of the mass If the mass of the binary is measured from the inspiral, an additional constraint can be imposed. The right EOS will have four different constraints. Ideally, a single detection would be sufficient.
26 This works for all EOSs considered In reality things will be more complicated. The lines will be stripes; Bayesian probability to get precision on M, R. Some numbers: at 50 Mpc, freq. uncertainty from Fisher matrix is 100 Hz at SNR=, the event rate is 0.- yr -1 for different EOSs.
27 Dynamically captured binaries and nucleosynthesis
28 animations by J. Papenfort, L. Bovard, LR
29 Mass ejection Mej [M ] LK RP5 LK RP7.5 LK RP10 LK QC t [ms] Mass ejected depends on impact parameter and takes place at each encounter. Quasi-circular binaries have smaller ejected masses (1- orders of magnitude) HY QC LK QC M0 QC Mass ejected depends on whether neutrino losses are taken into account (less ejected mass if neutrinos are taken into account) Mej [M ] HY RPX LK RPX M0 RPX r p /M
30 r < ( ) [10 3 M 1 ] 0 Waveforms have complex morphology: oscillations triggered after first encounter and typical HMNS signal after merger LK RP t r? [ms] 10 8 Improved neutrino treatment (M0) LK QC [g cm 3 ] Ye leads to larger values of Ye at high latitudes M0 QC [g cm 3 ] Ye t [ms]
31 Distributions in electron fraction, entropy, velocity HY RP10 LK RP10 M0 RP10 HY QC LK QC M0 QC Broad distribution in Ye when neutrino losses are taken into account Y e Y e HY RP10 LK RP10 M0 RP10 HY QC LK QC M0 QC Mass ejected at all latitudes but predominantly at low elevations HY RP10 LK RP10 M0 RP10 HY QC LK QC M0 QC Broad distribution in asymptotic velocities independent of initial conditions v 1 [c] v 1 [c]
32 Nucleosynthesis 10 1 Relative abundances Solar HY RP7.5 LK RP7.5 M0 RP7.5 Solar HY RP10 LK RP10 M0 RP10 Solar HY QC LK QC M0 QC A A A Ejected matter undergoes nucleosynthesis as expands and cools. Abundance pattern for A>10 is robust and good agreement with solar (nd and 3rd peak well reproduced) Abundances very robust: essentially the same for eccentric or quasi-circular binaries
33 Macronova emission Energy via radioactive decay of r-process nuclei powers transients in optical/near-infrared with peak emission after (Grossman+ 1) t peak =.9 Mej 10 M 1/ apple 10 cm g 1 1/ hv1 i 0.1 c 1/ days, The peak bolometric luminosity is estimated to be ( ectonova ) L = Mej 10 M 1 / apple 10 cm g 1 / hv1 i 0.1 c / erg s 1. with radioactive energy release a power law = 0 (t/t 0 ), ' 1.3 Eccentric binaries: ~ times more luminous than quasi-circular; delayed peak emission: ~ 8 days (cf. 1.5 days)
34 Conclusions Modelling of binary NSs in full GR is mature: GWs from the inspiral can be computed with precision of binary BHs Spectra of post-merger shows clear peaks, some of which are quasi-universal. If observed, will set tight constraints on EOS Eccentric binaries are rare but with larger ejected matter and macronova emission. high-a nucleosynthesis very robust
Simulations 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 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 informationGravitational waves from NS-NS/BH-NS binaries
Gravitational waves from NS-NS/BH-NS binaries Numerical-relativity simulation Masaru Shibata Yukawa Institute for Theoretical Physics, Kyoto University Y. Sekiguchi, K. Kiuchi, K. Kyutoku,,H. Okawa, K.
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 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 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 informationGRMHD SIMULATIONS OF NS-NS MERGERS. Bruno Giacomazzo University of Trento and INFN-TIFPA, Italy
GRMHD SIMULATIONS OF NS-NS MERGERS 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 sources for
More informationNeutron-star mergers:
Neutron-star mergers: Predictions by numerical relativity Masaru Shibata Center for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto University Many people are exploring NS binaries
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 informationGR SIMULATIONS OF BNS MERGERS: GWs AND SHORT GRBs. Bruno Giacomazzo University of Trento and INFN-TIFPA, Italy
GR SIMULATIONS OF BNS MERGERS: GWs AND SHORT GRBs Bruno Giacomazzo University of Trento and INFN-TIFPA, Italy Result of the explosion of stars larger than ~8 solar masses (but less than ~20-30 M ).! They
More informationGW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral Lazzaro Claudia for the LIGO Scientific Collaboration and the Virgo Collaboration 25 October 2017 GW170817 PhysRevLett.119.161101
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 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 informationApplications of Neutron-Star Universal Relations to Gravitational Wave Observations
Applications of Neutron-Star Universal Relations to Gravitational Wave Observations Department of Physics, Montana State University INT, Univ. of Washington, Seattle July 3rd 2014 Universal Relations:
More informationGravitational Wave Astronomy and the Internal Properties of Hypermassive Neutron Stars
Gravitational Wave Astronomy and the Internal Properties of Hypermassive Neutron Stars N E U TRON STA R S IN FUTURE RESEARCH, 1 1. D E CEMBER 2017 MAX- P L A NCK- INSTITUT F Ü R R A D I OASTRONOMIE B ONN,
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 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 informationarxiv: v1 [gr-qc] 21 Jan 2019
Spectral classification of gravitational-wave emission and equation of state constraints in binary neutron star mergers arxiv:1901.06969v1 [gr-qc] 21 Jan 2019 A. Bauswein 1,2 & N. Stergioulas 3 1 GSI Helmholtzzentrum
More informationDYNAMICS OF MIXED BINARIES
DYNAMICS OF MIXED BINARIES Luciano Rezzolla Albert Einstein Institute, Golm, Germany In collaboration with Frank Löffler & Marcus Ansorg [Phys. Rev. D 74 104018 (2006)] SISSA (Trieste, Italy), AEI (Golm,
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 informationMerger of binary neutron stars: Gravitational waves and electromagnetic counterparts Numerical-relativity study
Merger of binary neutron stars: Gravitational waves and electromagnetic counterparts Numerical-relativity study Masaru Shibata Yukawa Institute for Theoretical Physics, Kyoto University In collaboration
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 informationElectromagne,c Counterparts of Gravita,onal Wave Events
Electromagne,c Counterparts of Gravita,onal Wave Events Bing Zhang University of Nevada Las Vegas Jul. 21, 2014, INT Program14-2a, Binary Neutron Star Coalescence as a Fundamental Physics Laboratory Collaborators:
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 informationHow to simulate the most catastrophic events in the universe
How to simulate the most catastrophic events in the universe Luciano Rezzolla Max-Planck-Institut für Gravitationsphysik, Albert Einstein Institut, Potsdam, Germany NYC, 25/06/13 2013 International Summer
More information, G RAVITATIONAL-WAVE. Kent Yagi. with N. Yunes. Montana State University. YKIS2013, Kyoto
UNIVERSAL I-LOVE OVE-Q Q RELATIONSR IN Q R NEUTRON STARS AND THEIR APPLICATIONS TO ASTROPHYSICS STROPHYSICS,, GRAVITATIONAL G RAVITATIONAL-WAVE AVE, G AND FUNDAMENTAL PHYSICS Kent Yagi with N. Yunes Montana
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 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 informationGravitational waves from neutron-star binaries
Gravitational waves from neutron-star binaries - Constraining Neutron Star EOS - Masaru Shibata Center for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto University Outline 0. Brief
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 informationStudying the Effects of Tidal Corrections on Parameter Estimation
Studying the Effects of Tidal Corrections on Parameter Estimation Leslie Wade Jolien Creighton, Benjamin Lackey, Evan Ochsner Center for Gravitation and Cosmology 1 Outline Background: Physical description
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 informationSources of Gravitational Waves
1 Sources of Gravitational Waves Joan Centrella Laboratory for High Energy Astrophysics NASA/GSFC Gravitational Interaction of Compact Objects KITP May 12-14, 2003 A Different Type of Astronomical Messenger
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 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 informationMeasuring the Neutron-Star EOS with Gravitational Waves from Binary Inspiral
Measuring the Neutron-Star EOS with Gravitational Waves from Binary Inspiral I. Astrophysical Constraints Jocelyn Read, Ben Lackey, Ben Owen, JF II. NRDA NS-NS Jocelyn Read, Charalampos Markakis, Masaru
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 informationGravitational Waves & Intermediate Mass Black Holes. Lee Samuel Finn Center for Gravitational Wave Physics
Gravitational Waves & Intermediate Mass Black Holes Lee Samuel Finn Center for Gravitational Wave Physics Outline What are gravitational waves? How are they produced? How are they detected? Gravitational
More informationGRAVITATIONAL WAVE ASTRONOMY
GRAVITATIONAL WAVE ASTRONOMY A. Melatos (Melbourne) 1. GW: physics & astronomy 2. Current- & next-gen detectors & searches 3. Burst sources: CBC, SN GR, cosmology 4. Periodic sources: NS subatomic physics
More informationFundamental Physics, Astrophysics and Cosmology with ET
Fundamental Physics, Astrophysics and Cosmology with ET B.S. Sathyaprakash (CU) and Bernard Schutz (CU, AEI) based on a Living Review article with a similar title (in preparation) ET Science Summary Fundamental
More informationMeasuring the Neutron-Star EOS with Gravitational Waves from Binary Inspiral
Measuring the Neutron-Star EOS with Gravitational Waves from Binary Inspiral John L Friedman Leonard E. Parker Center for Gravitation, Cosmology, and Asrtrophysics Measuring the Neutron-Star EOS with Gravitational
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 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 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 informationGravitational Waves. Masaru Shibata U. Tokyo
Gravitational Waves Masaru Shibata U. Tokyo 1. Gravitational wave theory briefly 2. Sources of gravitational waves 2A: High frequency (f > 10 Hz) 2B: Low frequency (f < 10 Hz) (talk 2B only in the case
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 informationMergers Involving Black Holes and Neutron Stars in an ADM Landscape
Mergers Involving Black Holes and Neutron Stars in an ADM Landscape Bernard Schutz Albert Einstein Institute (AEI), Potsdam, Germany and Cardiff University, Wales with input from Luciano Rezzolla (AEI)
More informationMagnetized Binary Neutron Stars with Whisky
Magnetized Binary Neutron Stars with Whisky Bruno Giacomazzo (AEI, Potsdam, Germany) in collaboration with Luca Baiotti (Tokyo) and Luciano Rezzolla (AEI) Plan of the Talk Introduction The Whisky(MHD)
More informationConstraints from the GW merger event on the nuclear matter EoS
COST Action CA16214 Constraints from the GW170817 merger event on the nuclear matter EoS Fiorella Burgio INFN Sezione di Catania CRIS18, Portopalo di Capo Passero, June 18-22, 2018 1 Schematic view of
More informationLight curves and spectra of kilonovae
Light curves and spectra of kilonovae Current expectations and possibilities Tanaka 2016 Anders Jerkstrand, MPA Ingredients to predict observables 1. Mass, velocity and Ye of ejecta 2. Radioactivity and
More informationA Relativistic Toy Model for Black Hole-Neutron Star Mergers
A Relativistic Toy Model for Francesco Pannarale A.Tonita, L.Rezzolla, F.Ohme, J.Read Max-Planck-Institute für Gravitationsphysik (Albert-Einstein-Institut) SFB Videoseminars, Golm - January 17, 2011 Introduction
More informationMultimessenger Probes of Neutron Star Physics. David Tsang (U. Southampton)
Resonant Shattering Flares: Multimessenger Probes of Neutron Star Physics David Tsang (U. Southampton) GW/EM170817 - A Golden Binary Kasliwal+ 2017 Flux density (mjy) 10 1 10 2 10 3 10 4 10 5 10 6 10 7
More informationNeutron-star mergers in scalartensor theories of gravity
Neutron-star mergers in scalartensor theories of gravity Enrico Barausse (Institut d'astrophysique de Paris, France) in collaboration with Carlos Palenzuela (CITA, Canada), Luis Lehner (Perimeter Institute,
More informationGRMHD 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 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 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 informationGW Observation of Gravitational Waves from a Binary Black Hole Merger
GW150914 Observation of Gravitational Waves from a Binary Black Hole Merger F. Marion for the LIGO Scientific Collaboration and the Virgo Collaboration Seminar at CPPM, 2016 March 3 Introduction Sources
More informationOverview of Gravitational Wave Physics [PHYS879]
Overview of Gravitational Wave Physics [PHYS879] Alessandra Buonanno Maryland Center for Fundamental Physics Joint Space-Science Institute Department of Physics University of Maryland Content: What are
More informationConstraints on Neutron Star Sttructure and Equation of State from GW170817
Constraints on Neutron Star Sttructure and Equation of State from GW170817 J. M. Lattimer Department of Physics & Astronomy Stony Brook University March 12, 2018 INT-JINA GW170817 12 March, 2018 GW170817
More informationKey Results from Dynamical Spacetime GRMHD Simulations. Zachariah Etienne
Key Results from Dynamical Spacetime GRMHD Simulations Zachariah Etienne Outline Lecture 1: The mathematical underpinnings of GRMHD, astrophysical importance Lecture 2: Solving GRMHD equations numerically
More informationSynergy with Gravitational Waves
Synergy with Gravitational Waves Alexandre Le Tiec and Jérôme Novak Laboratoire Univers et Théories Observatoire de Paris / CNRS LIGO, Virgo, ( elisa, ET,... ( What is a gravitational wave? A gravitational
More informationSearching for Intermediate Mass Black Holes mergers
Searching for Intermediate Mass Black Holes mergers G. A. Prodi, Università di Trento and INFN for the LIGO Scientific collaboration and the Virgo collaboration special credits to Giulio Mazzolo and Chris
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 informationSources of Gravitational Waves
Optical afterglow of GRB 050709 Hubble image 5.6 days after initial gamma-ray burst (Credit: Derek Fox / Penn State University) Sources of Gravitational Waves Peter Shawhan SLAC Summer Institute August
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 informationWhat have we learned from coalescing Black Hole binary GW150914
Stas Babak ( for LIGO and VIRGO collaboration). Albert Einstein Institute (Potsdam-Golm) What have we learned from coalescing Black Hole binary GW150914 LIGO_DCC:G1600346 PRL 116, 061102 (2016) Principles
More informationGravitational Waves from Neutron Stars
Gravitational Waves from Neutron Stars Astronomical Institute Anton Pannekoek Elastic outer crust Neutron star modelling Elastic inner curst with superfluid neutrons Superfluid neutrons and superconducting
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 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 informationLIGO Status and Advanced LIGO Plans. Barry C Barish OSTP 1-Dec-04
LIGO Status and Advanced LIGO Plans Barry C Barish OSTP 1-Dec-04 Science Goals Physics» Direct verification of the most relativistic prediction of general relativity» Detailed tests of properties of gravitational
More informationDynamics of star clusters containing stellar mass black holes: 1. Introduction to Gravitational Waves
Dynamics of star clusters containing stellar mass black holes: 1. Introduction to Gravitational Waves July 25, 2017 Bonn Seoul National University Outline What are the gravitational waves? Generation of
More informationThe Dynamical Strong-Field Regime of General Relativity
The Dynamical Strong-Field Regime of General Relativity Frans Pretorius Princeton University IFT Colloquium Sao Paulo, March 30, 2016 Outline General Relativity @100 the dynamical, strong-field regime
More informationInferring the Nuclear Equation of State Using Gravitational Waves from Binary Neutron Star Mergers
Inferring the Nuclear Equation of State Using Gravitational Waves from Binary Neutron Star Mergers Samantha A. Usman 1 Advisors: Tjonnie Li 2, Alan Weinstein 2 1 Department of Physics, Syracuse University,
More informationNewtonian instantaneous action at a distance General Relativity information carried by gravitational radiation at the speed of light
Modern View of Gravitation Newtonian instantaneous action at a distance G µ = 8 µ # General Relativity information carried by gravitational radiation at the speed of light Gravitational Waves GR predicts
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 informationEINSTEIN TELESCOPE rd. 3 generation GW detector
EINSTEIN TELESCOPE rd 3 generation GW detector http://www.et-gw.eu/ Dorota Gondek-Rosińska University of Zielona Góra w imieniu polskiego ET konsorcjum (UW, UZG, UwB, PW, CAMK, IMPAN ) Gravitational wave
More informationFour ways of doing cosmography with gravitational waves
Four ways of doing cosmography with gravitational waves Chris Van Den Broeck National Institute for Subatomic Physics Amsterdam, The Netherlands StronG BaD Workshop, Oxford, Mississippi, 27 February -
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 informationCosmology with Gravitational Wave Detectors. Maya Fishbach
Cosmology with Gravitational Wave Detectors Maya Fishbach Part I: Cosmography Compact Binary Coalescenses are Standard Sirens The amplitude* of a GW from a CBC is The timescale is Measuring amplitude,
More informationWhat have we learned from the detection of gravitational waves? Hyung Mok Lee Seoul National University
What have we learned from the detection of gravitational waves? Hyung Mok Lee Seoul National University Outline Summary of 1st and 2nd Observing Runs Characteristics of detected sources Astrophysical Implications
More informationGravitational waves from binary neutron stars
Gravitational waves from binary neutron stars Koutarou Kyutoku High Energy Accelerator Research Organization (KEK), Institute of Particle and Nuclear Studies 2018/11/12 QNP2018 satellite at Tokai 1 Plan
More informationAstrophysical Stochastic Gravitational Waves. Jonah Kanner PHYS 798G March 27, 2007
Astrophysical Stochastic Gravitational Waves Jonah Kanner PHYS 798G March 27, 2007 Introduction Gravitational Waves come from space Require acceleration of dense mass (Think black holes and neutron stars!)
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 informationImplications of GW observations for short GRBs
Implications of GW observations for short GRBs Resmi Lekshmi Indian Institute of Space Science & Technology Trivandrum What are Gamma Ray Bursts? What are short GRBs? Open Questions : Central engine of
More informationGravitational Wave Burst Searches
Gravitational Wave Burst Searches Peter Shawhan For the LIGO Scientific Collaboration and Virgo Collaboration Gravitational Waves 2010 University of Minnesota October 16, 2010 LIGO-G1000998-v3 Worldwide
More informationProbing Cosmology and measuring the peculiar acceleration of binary black holes with LISA
Probing Cosmology and measuring the peculiar acceleration of binary black holes with LISA Institut de Physique Théorique CEA-Saclay CNRS Université Paris-Saclay Probing cosmology with LISA Based on: Tamanini,
More informationProbing the High-Density Behavior of Symmetry Energy with Gravitational Waves
Probing the High-Density Behavior of Symmetry Energy with Gravitational Waves Farrukh J. Fattoyev Bao-An Li, William G. Newton Texas A&M University-Commerce 27 th Texas Symposium on Relativistic Astrophysics
More informationLISA: Probing the Universe with Gravitational Waves. Tom Prince Caltech/JPL. Laser Interferometer Space Antenna LISA
: Probing the Universe with Gravitational Waves Tom Caltech/JPL Laser Interferometer Space Antenna http://lisa.nasa.gov Gravitational Wave Astronomy is Being Born LIGO, VIRGO, GEO, TAMA 4000m, 3000m, 2000m,
More informationGR Simulations of Neutron Star-Neutron Star & Black Hole-Neutron Star Binaries
GR Simulations of Neutron Star-Neutron Star & Black Hole-Neutron Star Binaries Masaru Shibata Yukawa Institute for Theoretical Physics, Kyoto University Introduction: Why NS-NS/BH-NS simulations are important?
More informationGravity. Newtonian gravity: F = G M1 M2/r 2
Gravity Einstein s General theory of relativity : Gravity is a manifestation of curvature of 4- dimensional (3 space + 1 time) space-time produced by matter (metric equation? g μν = η μν ) If the curvature
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 informationSearching for Gravitational Waves from Coalescing Binary Systems
Searching for Gravitational Waves from Coalescing Binary Systems Stephen Fairhurst Cardiff University and LIGO Scientific Collaboration 1 Outline Motivation Searching for Coalescing Binaries Latest Results
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 informationStudies of self-gravitating tori around black holes and of self-gravitating rings
Studies of self-gravitating tori around black holes and of self-gravitating rings Pedro Montero Max Planck Institute for Astrophysics Garching (Germany) Collaborators: Jose Antonio Font (U. Valencia) Masaru
More informationThe Merger of Two Compact Stars: A Tool for Dense Matter Nuclear Physics
Review The Merger of Two Compact Stars: A Tool for Dense Matter Nuclear Physics Alessandro Drago 1 ID, Giuseppe Pagliara 1, Sergei B. Popov 2, Silvia Traversi 1, * and Grzegorz Wiktorowicz 3,4 1 Dipartimento
More informationMulti-Messenger Signatures of the R-Process
Multi-Messenger Signatures of the R-Process Brian Metzger Columbia University In Collaboration with Rodrigo Fernandez, Eliot Quataert, Geoff Bower, Dan Kasen (UC Berkeley) Andrey Vlasov (Columbia), Almudena
More informationFORMATION AND EVOLUTION OF COMPACT BINARY SYSTEMS
FORMATION AND EVOLUTION OF COMPACT BINARY SYSTEMS Main Categories of Compact Systems Formation of Compact Objects Mass and Angular Momentum Loss Evolutionary Links to Classes of Binary Systems Future Work
More informationBlack Holes and Active Galactic Nuclei
Black Holes and Active Galactic Nuclei A black hole is a region of spacetime from which gravity prevents anything, including light, from escaping. The theory of general relativity predicts that a sufficiently
More informationThe effect of f - modes on the gravitational waves during a binary inspiral
The effect of f - modes on the gravitational waves during a binary inspiral Tanja Hinderer (AEI Potsdam) PRL 116, 181101 (2016), arxiv:1602.00599 and arxiv:1608.01907? A. Taracchini F. Foucart K. Hotokezaka
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 information