GR SIMULATIONS OF BNS MERGERS: GWs AND SHORT GRBs. Bruno Giacomazzo University of Trento and INFN-TIFPA, Italy
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1 GR SIMULATIONS OF BNS MERGERS: GWs AND SHORT GRBs Bruno Giacomazzo University of Trento and INFN-TIFPA, Italy
2 Result of the explosion of stars larger than ~8 solar masses (but less than ~20-30 M ).! They may appear as isolated objects or in binaries.! Often observed as pulsars (discovered in 1967 by graduate student Jocelyn Bell Burnell). NEUTRON STARS Crab Pulsar Credit: NASA/CXC/ASU/J. Hester et al
3 WHY SO INTERESTING? Due to their duration and dynamics, NS-NS and NS-BH binaries are very good sources for gravitational wave detectors such as Virgo (Italy) and Ligo (USA) Virgo (Pisa, Italy) They are also possible sources for short gamma-ray bursts. Tori formed after the merger could power GRBs via neutrino or magnetic fields. Credit: NASA/SkyWorks Digital
4 GRAVITATIONAL WAVES Predicted by the theory of General Relativity! Distortions of the space-time that propagate unperturbed like a wave! Most powerful sources are compact object binaries! Carry detailed information about the source (NS, BH,...) Credit: NASA Gws will provide a new way to listen to the Universe and open a new frontier.! They are the only way to detect BH directly!! To be detected yet...
5 GW: DO THEY EXIST? GWs carry away energy and angular momentum from orbiting systems! Binary pulsars have been used to verify such predictions! Very good agreement with observations: Nobel prize given in 1993! B Weisberg et al 2010, ApJ 722, 1030
6 GW SPECTRUM AND DETECTORS Several possible sources to study! To detect them and verify theoretical models we need GW templates! Necessary to predict the GWs that we will detect Source:
7 GR NS-NS SIMULATIONS: STATE OF THE ART (for a recent review see: Faber & Rasio 2012, arxiv: ) GRHD (only most recent papers listed) Read et al 2009: investigated cold realistic EOS and GW inspiral signals Baiotti et al 2009: first study of the accuracy of GR computed GWs Kiuchi et al 2009: long-term inspiral, APR EOS Rezzolla et al 2010: studied tori and long HMNS evolutions Kiuchi et al 2010: connection between short-grbs and GWs Baiotti et al 2010, 2011: long-term inspiral and comparison with EOB Sekiguchi et al 2011: first study of neutrino emission in full GR Thierfelder et al 2011: AMR, ideal-fluid EOS, accurate convergence study Gold et al 2012: first study of the merger of eccentric equal-mass neutron stars Bernuzzi et al 2012: study of tidal effects and EOB during inpsiral Barausse et al 2013: BNS mergers in scalar tensor theories of gravity Kastaun et al 2013: study of spin of BH produced by mergers Hotokezaka et al 2013a,b: study of mass ejection and HMNS evolution Read et al 2013: multicode study of EOS effects on GWs Reisswig et al 2013: first BNS merger using multipatch grids Radice et al 2013: first high order simulations of BNS inspiral Bernuzzi et al : BNS simulations with spinning NSs Shibata et al 2014: BNS in scalar tensor theories with spontaneous scalarization Takami et al 2014: relation between post-merger GWs and EOS
8 GR NS-NS SIMULATIONS: STATE OF THE ART (for a recent review see: Faber & Rasio 2012, arxiv: ) GRMHD (all the papers listed) Anderson et al 2008: first run of magnetized BNS (B~10 16 G) Liu et al 2008: magnetized BNS (B~10 16 G), followed collapse to BH Giacomazzo et al 2009: first study of amplification of magnetic field Giacomazzo et al 2011: first study of realistic configurations (B~ G) Rezzolla, Giacomazzo et al 2011: first evidence of jet formation Palenzuela et al 2013: study of EM precursors via resistive GRMHD simulations Giacomazzo and Perna 2013: first study of possible magnetar formation Neilsen et al 2014: first GRMHD code including also neutrino emission Ponce et al 2014: EM precursors for arbitrary magnetic field orientations Kiuchi et al 2014: very high-res simulations (~70 m), no jet observed Giacomazzo et al 2014: magnetic field amplification via a subgrid model
9 THE ET AND WHISKY CODES The E i n s t e i n T o o l k i t (einsteintoolkit.org) is a set of open source codes for computational relativity. It provides infrastructures for parallelization, I/O, AMR, space-time evolution routines,... Whisky ( is a numerical code, initially developed at the AEI and SISSA, for the solution of the general relativistic hydrodynamics and ideal magnetohydrodynamics equations in arbitrary curved spacetimes. ET Whisky
10 GRMHD EQUATIONS The evolution equations of the matter are given as usual by the conservation of the baryon number and energy-momentum: µ T µ = 0 µ J µ = 0 J µ u µ T µ = ( + + p + b 2 )u µ u + plus an Equation of State P=P(ρ,ε) p b2 g µ b µ b The evolution of the magnetic field obeys Maxwell s equations (assuming infinite conductivity): t B = v B = 0 B
11 GRMHD EQUATIONS The evolution equations are then rewritten in a conservative form: 1 ( p U)+@ i ( p gf i ) = S g HRSC schemes are used to solve them (HLLE, PPM) and the divergence free character of the magnetic field is guarantee by evolving the vector potential (Giacomazzo and Rezzolla 2007, Giacomazzo et al 2011, Giacomazzo and Perna 2013)
12 GW EMISSION FROM NS-NS MERGERS
13 NEUTRON STARS Discovered in 1967, NSs are one of the most fascinating objects! Have been observed for several years! Their internal structure is still a mystery... Credit: Dany Page (
14 NS MASS Several observation of NS masses are available! NS masses observed up to M~2 (Demorest et al 2010, Antoniadis et al 2013)! Radius not well constrained (~10 to ~15 km?) Figure by Jim Lattimer
15 NS EOS: MASS vs RADIUS S e v e r a l different EOSs a l l o w f o r s i m i l a r N S masses. Lattimer & Prakash 2007 Only contemporary measure of Mass and Radius can constrain EOS.
16 IDEAL-FLUID EOS: HIGH-MASS BINARY Visualization by Giacomazzo, Kaehler, Rezzolla
17
18 GRAVITATIONAL WAVES FROM BINARY NEUTRON STARS contribution from the inspiral contribution from the HMNS
19 MATTER EFFECTS ON BNS GWs (Read et al 2013, PRD 88, ) We used the Whisky and SACRA codes to perform the first multicode study of EOS effects on merger waveforms! Used an extended set of piecewise polytropic EOSs! Estimated numerical errors by comparing between the codes and using different resolutions.
20 MATTER EFFECTS ON BNS GWs (Read et al 2013, PRD 88, ) GW frequency at merger is well correlated with tidal deformability and NS compactness (see also Bernuzzi et al 2014).
21 MATTER EFFECTS ON BNS GWs (Read et al 2013, PRD 88, ) HB Hybrid GWs: EOSs distinguishable at 300 Mpc if NS radii differ of ~1.3km Only numrel GWs: EOSs distinguishable at 100 Mpc if NS radii differ of ~1.3km
22 POST-MERGER GRAVITATIONAL WAVES Simulation by L. Baiotti (Rezzolla et al 2010)
23 EOS EFFECTS IN THE POSTMERGER Andersson et al 2013 Rezzolla et al 2010: for smaller NS masses, HMNS can survive for more than 100ms. Bauswein & Janka 2012 Bauswein et al , Hotokezaka et al 2013, Takami et al 2014: frequency peak in GWs emitted after merger can constrain EOS Is the EOS the only unknown to affect the post-merger?
24 POST-MERGER: MAGNETIC FIELD EFFECTS Giacomazzo, Rezzolla, Baiotti 2011, PRD 83, We considered equal-mass BNSs with different masses and with a p o l o i d a l magnetic field with different amplitudes (B~ G). First time this study was done in full GR Studied impact on dynamics, disk formation, and GW emission
25 Model M1.62-B10 Visualization by Koppitz, Giacomazzo, Rezzolla
26 GW: MAGNETIC FIELD EFFECTS IN THE HMNS Giacomazzo et al 2011 Magnetic field may have an impact on the post-merger GWs and even accelerate collapse to BH.
27 BNSs AND THE CENTRAL ENGINE OF SHORT-GRBs
28 MOST POPULAR MODEL FOR SGRB CENTRAL ENGINE Image from Neil Gehrels, Luigi Piro, and Peter J. T. Leonard 2007, Scientific American sp 17, 34! (CREDIT: JUAN VELASCO)
29 UNEQUAL-MASS BNS: M3.4q0.80 Visualization by Giacomazzo, Koppitz, Rezzolla
30 COMPACT BINARY PROGENITORS OF SHORT GAMMA-RAY BURSTS Giacomazzo, Perna, Rezzolla, Troja, Lazzati 2013, ApJL 762, L18 Depending on mass and EOS several post-merger scenarios: NS-BH BH+torus NS-NS HMNS SMNS+torus BH+torus? NS+torus Magnetic fields play fundamental role in post-merger dynamics (jets from BH/NS+torus, NS collapse to BH,...) All these scenarios may lead to SGRBs with different properties
31 JETS FROM BNS MERGERS? Rezzolla, Giacomazzo, Baiotti, Granot, Kouveliotou, Aloy 2011, ApJL 732, L6
32 Rezzolla et al 2011, ApJL 732, L6 Etienne et al 2012, PRD 86, BNS and NS-BH can produce tori around spinning BHs. When NSs are magnetized this can lead to the production of relativistic jets. Energy extraction from the disk can power short GRBs. Can we link SGRBs observations with numerical simulations?
33 We considered the current sample of SGRBs with measured energies We made the following assumptions: SGRBs are powered via magnetic fields SGRBs energy is provided by the disk Efficiency is constant E,iso = M torus c 2 jet jet = 10% = 50% εjet is inferred from disk simulations (Fragile, McKinney, Tchekhovskoy,...) εᵧ is derived from observations (e.g., Zhang et al 2007)
34 From the BNS simulations we computed a fit to relate the mass of the torus to the NS masses and their mass ratio q: M torus =[c 1 (1 q)+c 2 ][c 3 (1 + q) M BNS /M max ] 2.4 M torus /M 0.9 MBNS /Mmax Giacomazzo et al 2013 q Almost all SGRBs are produced by high-mass BNSs. These BNSs produce an HMNS that survive only few ms before collapse to BH.
35 low-energy SGRBs (<~1e51 erg) high-energy SGRBs (>~1e51 erg) high-mass BNSs low-mass BNSs Simultaneous GW/EM detection will help validate this model
36 MAGNETAR FORMATION Giacomazzo & Perna 2013, ApJ Letters, 771, L26 What about the blue path? NS-BH BH+torus NS-NS HMNS SMNS+torus BH+torus? NS+torus Credit: The Matrix (1999)
37 WHY DO WE NEED A MAGNETAR? Rowlinson et al 2013 A stable magnetar could be used to explain X-ray plateaus and extended emissions from SGRBs (e.g., Rowlinson et al 2013).
38 TIME-REVERSAL SGRB MODEL (CIOLFI+SIEGEL 2014, REZZOLLA+KUMAR 2014) X-ray afterglow emitted by magnetar SGRB emitted by BH after magnetar collapse Ciolfi & Siegel 2014
39 MAGNETAR FORMATION Giacomazzo & Perna 2013, ApJ Letters, 771, L26 Investigated merger of two 1.2 M NSs! Used Ideal Fluid, Gamma=2.75, k=30000 (Oechslin et al 2007)!! Produced a stable ultraspinning NS surrounded by a magnetized disk of ~0.1 M.
40 MAGNETAR FORMATION Giacomazzo & Perna 2013, ApJ Letters, 771, L26 Magnetic field amplified of ~2 orders of magnitude. Difference in the GW signal are small and present only in the post-merger phase. GWs publicly available for download at
41 CONCLUSIONS GRMHD simulations of BNSs now able to study all phases of merger Tidal effects at merger may be used to constrain NS EOS Magnetized BNSs may produce jets and power SGRBs BNS mergers can be used both for the standard GRB model and for the magnetar one In the standard scenario most SGRBs may be generated by highmass BNSs: less energetic SGRBs are powered by high-mass BNSs more energetic ones by low-mass BNSs Possible to form stable magnetar+disk from BNS mergers
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