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Carullo G, Albanesi S, Nagar A, Gamba R, Bernuzzi S, Andrade T, Trenado J. Unveiling the Merger Structure of Black Hole Binaries in Generic Planar Orbits. PHYSICAL REVIEW LETTERS 2024; 132:101401. [PMID: 38518333 DOI: 10.1103/physrevlett.132.101401] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/18/2023] [Revised: 12/24/2023] [Accepted: 02/09/2024] [Indexed: 03/24/2024]
Abstract
The precise modeling of binary black hole coalescences in generic planar orbits is a crucial step to disentangle dynamical and isolated binary formation channels through gravitational-wave observations. The merger regime of such coalescences exhibits a significantly higher complexity compared to the quasicircular case, and cannot be readily described through standard parametrizations in terms of eccentricity and anomaly. In the spirit of the effective one body formalism, we build on the study of the test-mass limit, and introduce a new modeling strategy to describe the general-relativistic dynamics of two-body systems in generic orbits. This is achieved through gauge-invariant combinations of the binary energy and angular momentum, such as a dynamical "impact parameter" at merger. These variables reveal simple "quasi-universal" structures of the pivotal merger parameters, allowing us to build an accurate analytical representation of generic (bounded and dynamically bounded) orbital configurations. We demonstrate the validity of these analytical relations using 311 numerical simulations of bounded noncircular binaries with progenitors from the RIT and SXS catalogs, together with a custom dataset of dynamical captures generated using the Einstein Toolkit, and test-mass data in bound orbits. Our modeling strategy lays the foundations of accurate and complete waveform models for systems in arbitrary orbits, bolstering observational explorations of dynamical formation scenarios and the discovery of new classes of gravitational wave sources.
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Affiliation(s)
- Gregorio Carullo
- Niels Bohr International Academy, Niels Bohr Institute, Blegdamsvej 17, 2100 Copenhagen, Denmark
| | - Simone Albanesi
- INFN sezione di Torino, Torino 10125, Italy
- Dipartimento di Fisica, Università di Torino, Torino 10125, Italy
| | - Alessandro Nagar
- INFN sezione di Torino, Torino 10125, Italy
- Institut des Hautes Etudes Scientifiques, 35 Route de Chartres, Bures-sur-Yvette 91440, France
| | - Rossella Gamba
- Theoretisch-Physikalisches Institut, Friedrich-Schiller-Universität Jena, 07743 Jena, Germany
| | - Sebastiano Bernuzzi
- Theoretisch-Physikalisches Institut, Friedrich-Schiller-Universität Jena, 07743 Jena, Germany
| | - Tomas Andrade
- Departament de Física Quàntica i Astrofísica, Institut de Ciències del Cosmos, Universitat de Barcelona, Martí i Franquès 1, E-08028 Barcelona, Spain
| | - Juan Trenado
- Departament de Física Quàntica i Astrofísica, Institut de Ciències del Cosmos, Universitat de Barcelona, Martí i Franquès 1, E-08028 Barcelona, Spain
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2
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Baumgarte TW, Brügmann B, Cors D, Gundlach C, Hilditch D, Khirnov A, Ledvinka T, Renkhoff S, Fernández IS. Critical Phenomena in the Collapse of Gravitational Waves. PHYSICAL REVIEW LETTERS 2023; 131:181401. [PMID: 37977635 DOI: 10.1103/physrevlett.131.181401] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/26/2023] [Revised: 09/04/2023] [Accepted: 09/22/2023] [Indexed: 11/19/2023]
Abstract
Fine-tuning generic but smooth spherically symmetric initial data for general relativity to the threshold of dynamical black hole formation creates arbitrarily large curvatures, mediated by a universal self-similar solution that acts as an intermediate attractor. For vacuum gravitational waves, however, these critical phenomena have been elusive. We present, for the first time, excellent agreement among three independent numerical simulations of this collapse. Surprisingly, we find no universality, and observe approximate self-similarity for some families of initial data but not for others.
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Affiliation(s)
- Thomas W Baumgarte
- Department of Physics and Astronomy, Bowdoin College, Brunswick, Maine 04011, USA
| | - Bernd Brügmann
- Friedrich-Schiller-Universität, Jena, 07743 Jena, Germany
| | - Daniela Cors
- Friedrich-Schiller-Universität, Jena, 07743 Jena, Germany
| | - Carsten Gundlach
- School of Mathematical Sciences, University of Southampton, Southampton SO17 1BJ, United Kingdom
| | - David Hilditch
- Centro de Astrofísica e Gravitação-CENTRA, Departamento de Física, Instituto Superior Técnico-IST, Universidade de Lisboa-UL, Avenida Rovisco Pais 1, 1049-001 Lisboa, Portugal
| | - Anton Khirnov
- Institute of Theoretical Physics, Faculty of Mathematics and Physics, Charles University, CZ-180 00 Prague, Czech Republic
| | - Tomáš Ledvinka
- Institute of Theoretical Physics, Faculty of Mathematics and Physics, Charles University, CZ-180 00 Prague, Czech Republic
| | - Sarah Renkhoff
- Friedrich-Schiller-Universität, Jena, 07743 Jena, Germany
| | - Isabel Suárez Fernández
- Departament de Física, Universitat de les Illes Balears, IAC3-IEEC, Carretera Valldemossa km 7.5, E-07122 Palma, Spain
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3
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Healy J, Lousto CO. Ultimate Black Hole Recoil: What is the Maximum High-Energy Collision Kick? PHYSICAL REVIEW LETTERS 2023; 131:071401. [PMID: 37656861 DOI: 10.1103/physrevlett.131.071401] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/30/2022] [Accepted: 07/13/2023] [Indexed: 09/03/2023]
Abstract
We performed a series of 1381 full numerical simulations of high energy collision of black holes to search for the maximum recoil velocity after their merger. We consider equal mass binaries with opposite spins pointing along their orbital plane and perform a search of spin orientations, impact parameters, and initial linear momenta to find the maximum recoil for a given spin magnitude s. This spin sequence for s=0.4, 0.7, 0.8, 0.85, 0.9 is then extrapolated to the extreme case, s=1, to obtain an estimated maximum recoil velocity of 28,562±342 km/s, thus approximately bounded by 10% of the speed of light.
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Affiliation(s)
- James Healy
- Center for Computational Relativity and Gravitation (CCRG), School of Mathematical Sciences, Rochester Institute of Technology, 85 Lomb Memorial Drive, Rochester, New York 14623, USA
| | - Carlos O Lousto
- Center for Computational Relativity and Gravitation (CCRG), School of Mathematical Sciences, Rochester Institute of Technology, 85 Lomb Memorial Drive, Rochester, New York 14623, USA
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4
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Kiuchi K, Fujibayashi S, Hayashi K, Kyutoku K, Sekiguchi Y, Shibata M. Self-Consistent Picture of the Mass Ejection from a One Second Long Binary Neutron Star Merger Leaving a Short-Lived Remnant in a General-Relativistic Neutrino-Radiation Magnetohydrodynamic Simulation. PHYSICAL REVIEW LETTERS 2023; 131:011401. [PMID: 37478426 DOI: 10.1103/physrevlett.131.011401] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/21/2022] [Revised: 05/22/2023] [Accepted: 06/02/2023] [Indexed: 07/23/2023]
Abstract
We perform a general-relativistic neutrino-radiation magnetohydrodynamic simulation of a one second-long binary neutron star merger on the Japanese supercomputer Fugaku using about 85 million CPU hours with 20 736 CPUs. We consider an asymmetric binary neutron star merger with masses of 1.2M_{⊙} and 1.5M_{⊙} and a "soft" equation of state SFHo. It results in a short-lived remnant with the lifetime of ≈0.017 s, and subsequent massive torus formation with the mass of ≈0.05M_{⊙} after the remnant collapses to a black hole. For the first time, we find that after the dynamical mass ejection, which drives the fast tail and mildly relativistic components, the postmerger mass ejection from the massive torus takes place due to the magnetorotational instability-driven turbulent viscosity in a single simulation and the two ejecta components are seen in the distributions of the electron fraction and velocity with distinct features.
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Affiliation(s)
- Kenta Kiuchi
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg, Potsdam-Golm 14476, Germany
- Center for Gravitational Physics and Quantum Information, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, Japan
| | - Sho Fujibayashi
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg, Potsdam-Golm 14476, Germany
| | - Kota Hayashi
- Center for Gravitational Physics and Quantum Information, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, Japan
| | - Koutarou Kyutoku
- Center for Gravitational Physics and Quantum Information, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, Japan
- Department of Physics, Kyoto University, Kyoto 606-8502, Japan
- Interdisciplinary Theoretical and Mathematical Science Program (iTHEMS), RIKEN, Wako, Saitama 351-0198, Japan
| | - Yuichiro Sekiguchi
- Center for Gravitational Physics and Quantum Information, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, Japan
- Department of Physics, Toho University, Funabashi, Chiba 274-8510, Japan
| | - Masaru Shibata
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg, Potsdam-Golm 14476, Germany
- Center for Gravitational Physics and Quantum Information, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, Japan
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5
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Saló LA, Clough K, Figueras P. Well-Posedness of the Four-Derivative Scalar-Tensor Theory of Gravity in Singularity Avoiding Coordinates. PHYSICAL REVIEW LETTERS 2022; 129:261104. [PMID: 36608187 DOI: 10.1103/physrevlett.129.261104] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/26/2022] [Accepted: 11/21/2022] [Indexed: 06/17/2023]
Abstract
We show that the most general scalar-tensor theory of gravity up to four derivatives in 3+1 dimensions is well-posed in a modified version of the CCZ4 formulation of the Einstein equations in singularity-avoiding coordinates. We demonstrate the robustness of our new formulation in practice by studying equal mass black hole binary mergers for different values of the coupling constants. Although our analysis of well-posedness is restricted to cases in which the couplings are small, we find that in simulations we are able to push the couplings to larger values, so that a certain weak coupling condition is order one, without instabilities developing. Our Letter provides the means for such simulations to be undertaken by the many numerical relativity codes that rely on the moving puncture gauge to evolve black hole singularities.
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Affiliation(s)
- Llibert Aresté Saló
- School of Mathematical Sciences, Queen Mary University of London, Mile End Road, London E1 4NS, United Kingdom
| | - Katy Clough
- School of Mathematical Sciences, Queen Mary University of London, Mile End Road, London E1 4NS, United Kingdom
| | - Pau Figueras
- School of Mathematical Sciences, Queen Mary University of London, Mile End Road, London E1 4NS, United Kingdom
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6
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Doneva DD, Vañó-Viñuales A, Yazadjiev SS. Dynamical descalarization with a jump during a black hole merger. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.l061502] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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7
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Sanchis-Gual N, Zilhão M, Cardoso V. Electromagnetic emission from axionic boson star collisions. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.064034] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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8
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Jiménez-Vázquez E, Alcubierre M. Critical gravitational collapse of a massive complex scalar field. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.044071] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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9
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Elley M, Silva HO, Witek H, Yunes N. Spin-induced dynamical scalarization, descalarization, and stealthness in scalar-Gauss-Bonnet gravity during a black hole coalescence. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.044018] [Citation(s) in RCA: 2] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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10
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Hayashi K, Fujibayashi S, Kiuchi K, Kyutoku K, Sekiguchi Y, Shibata M. General-relativistic neutrino-radiation magnetohydrodynamic simulation of seconds-long black hole-neutron star mergers. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.023008] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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11
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Joana C. Gravitational dynamics in Higgs inflation: Preinflation and preheating with an auxiliary field. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.023504] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/06/2022]
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12
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Thinking Outside the Box: Numerical Relativity with Particles. Symmetry (Basel) 2022. [DOI: 10.3390/sym14061280] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/16/2022] Open
Abstract
The observation of gravitational waves from compact objects has now become an active part of observational astronomy. For a sound interpretation, one needs to compare such observations against detailed Numerical Relativity simulations, which are essential tools to explore the dynamics and physics of compact binary mergers. To date, essentially all simulation codes that solve the full set of Einstein’s equations are performed in the framework of Eulerian hydrodynamics. The exception is our recently developed Numerical Relativity code SPHINCS_BSSN which solves the commonly used BSSN formulation of the Einstein equations on a structured mesh and the matter equations via Lagrangian particles. We show here, for the first time, SPHINCS_BSSN neutron star merger simulations with piecewise polytropic approximations to four nuclear matter equations of state. In this set of neutron star merger simulations, we focus on perfectly symmetric binary systems that are irrotational and have 1.3 M⊙ masses. We introduce some further methodological refinements (a new way of steering dissipation, an improved particle–mesh mapping), and we explore the impact of the exponent that enters in the calculation of the thermal pressure contribution. We find that it leaves a noticeable imprint on the gravitational wave amplitude (calculated via both quadrupole approximation and the Ψ4 formalism) and has a noticeable impact on the amount of dynamic ejecta. Consistent with earlier findings, we only find a few times 10−3M⊙ as dynamic ejecta in the studied equal mass binary systems, with softer equations of state (which are more prone to shock formation) ejecting larger amounts of matter. In all of the cases, we see a credible high-velocity (∼0.5…0.7c) ejecta component of ∼10−4M⊙ that is launched at contact from the interface between the two neutron stars. Such a high-velocity component has been suggested to produce an early, blue precursor to the main kilonova emission, and it could also potentially cause a kilonova afterglow.
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13
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Sanchis-Gual N, Izquierdo P. Ultralight bosonic dark matter in white dwarfs and potential observational consequences. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.105.084023] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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14
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Bozzola G. Does Charge Matter in High-Energy Collisions of Black Holes? PHYSICAL REVIEW LETTERS 2022; 128:071101. [PMID: 35244443 DOI: 10.1103/physrevlett.128.071101] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/04/2021] [Revised: 12/07/2021] [Accepted: 01/13/2022] [Indexed: 06/14/2023]
Abstract
We perform numerical-relativity simulations of high-energy head-on collisions of charged black holes with the same charge-to-mass ratio λ. We find that electromagnetic interactions have subdominant effects already at low Lorentz factors γ, supporting the conjecture that the details of the properties of black holes (e.g., their spin or charge) play a secondary role in these phenomena. Using this result and conservation of energy, we argue these events cannot violate cosmic censorship.
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Affiliation(s)
- Gabriele Bozzola
- Department of Astronomy, University of Arizona, Tucson, Arizona 85721, USA
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15
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Tsokaros A, Ruiz M, Shapiro SL, Uryū K. Magnetohydrodynamic Simulations of Self-Consistent Rotating Neutron Stars with Mixed Poloidal and Toroidal Magnetic Fields. PHYSICAL REVIEW LETTERS 2022; 128:061101. [PMID: 35213191 DOI: 10.1103/physrevlett.128.061101] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/29/2021] [Revised: 12/21/2021] [Accepted: 01/10/2022] [Indexed: 06/14/2023]
Abstract
We perform the first magnetohydrodynamic simulations in full general relativity of self-consistent rotating neutron stars (NSs) with ultrastrong mixed poloidal and toroidal magnetic fields. The initial uniformly rotating NS models are computed assuming perfect conductivity, stationarity, and axisymmetry. Although the specific geometry of the mixed field configuration can delay or accelerate the development of various instabilities known from analytic perturbative studies, all our models finally succumb to them. Differential rotation is developed spontaneously in the cores of our magnetars which, after sufficient time, is converted back to uniform rotation. The rapidly rotating magnetars show a significant amount of ejecta, which can be responsible for transient kilonova signatures. However, no highly collimated, helical magnetic fields or incipient jets, which are necessary for γ-ray bursts, arise at the poles of these magnetars by the time our simulations are terminated.
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Affiliation(s)
- Antonios Tsokaros
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Milton Ruiz
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Stuart L Shapiro
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
- Department of Astronomy and NCSA, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Kōji Uryū
- Department of Physics, University of the Ryukyus, Senbaru, Nishihara, Okinawa 903-0213, Japan
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16
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Mathews GJ, Kedia A, Kim HI, Suh IS. Neutron Star Mergers and the Quark Matter Equation of State. EPJ WEB OF CONFERENCES 2022. [DOI: 10.1051/epjconf/202227401013] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 12/24/2022] Open
Abstract
As neutron stars merge they can approach very high nuclear density. Here, we summarized recent results for the evolution and gravitational wave emission from binary-neutron star mergers using a a variety of nuclear equations of state with and without a crossover transition to quark matter. We discuss how the late time gravitational wave emission from binary neutron star mergers may possibly reveal the existence of a crossover transition to quark matter.
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17
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Schnauck SC, Baumgarte TW, Shapiro SL. Accretion onto black holes inside neutron stars with piecewise-polytropic equations of state: Analytic and numerical treatments. Int J Clin Exp Med 2021. [DOI: 10.1103/physrevd.104.123021] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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18
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Bozzola G, Paschalidis V. Numerical-relativity simulations of the quasicircular inspiral and merger of nonspinning, charged black holes: Methods and comparison with approximate approaches. Int J Clin Exp Med 2021. [DOI: 10.1103/physrevd.104.044004] [Citation(s) in RCA: 9] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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19
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Silva HO, Witek H, Elley M, Yunes N. Dynamical Descalarization in Binary Black Hole Mergers. PHYSICAL REVIEW LETTERS 2021; 127:031101. [PMID: 34328770 DOI: 10.1103/physrevlett.127.031101] [Citation(s) in RCA: 12] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/23/2020] [Revised: 03/16/2021] [Accepted: 06/17/2021] [Indexed: 06/13/2023]
Abstract
Scalar fields coupled to the Gauss-Bonnet invariant can undergo a tachyonic instability, leading to spontaneous scalarization of black holes. Studies of this effect have so far been restricted to single black hole spacetimes. We present the first results on dynamical scalarization in head-on collisions and quasicircular inspirals of black hole binaries with numerical relativity simulations. We show that black hole binaries can either form a scalarized remnant or dynamically descalarize by shedding off its initial scalar hair. The observational implications of these findings are discussed.
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Affiliation(s)
- Hector O Silva
- Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut), Am Mühlenberg 1, D-14476 Potsdam, Germany
- Illinois Center for Advanced Studies of the Universe and Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Helvi Witek
- Illinois Center for Advanced Studies of the Universe and Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Matthew Elley
- Department of Physics, King's College London, Strand, London WC2R 2LS, United Kingdom
| | - Nicolás Yunes
- Illinois Center for Advanced Studies of the Universe and Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
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20
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Ledvinka T, Khirnov A. Universality of Curvature Invariants in Critical Vacuum Gravitational Collapse. PHYSICAL REVIEW LETTERS 2021; 127:011104. [PMID: 34270303 DOI: 10.1103/physrevlett.127.011104] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/18/2021] [Accepted: 06/08/2021] [Indexed: 06/13/2023]
Abstract
We report on a numerical study of gravitational waves undergoing gravitational collapse due to their self-interaction. We consider several families of asymptotically flat initial data which, similar to the well-known Choptuik's discovery, can be fine-tuned between dispersal into empty space and collapse into a black hole. We find that near-critical spacetimes exhibit behavior similar to scalar-field collapse: For different families of initial data, we observe universal "echoes" in the form of irregularly repeating, approximate, scaled copies of the same piece of spacetime.
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Affiliation(s)
- Tomáš Ledvinka
- Institute of Theoretical Physics, Faculty of Mathematics and Physics, Charles University, CZ-180 00 Prague, Czech Republic
| | - Anton Khirnov
- Institute of Theoretical Physics, Faculty of Mathematics and Physics, Charles University, CZ-180 00 Prague, Czech Republic
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21
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Rosato N, Healy J, Lousto CO. Adapted gauge to small mass ratio binary black hole evolutions. Int J Clin Exp Med 2021. [DOI: 10.1103/physrevd.103.104068] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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22
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Richards CB, Baumgarte TW, Shapiro SL. Accretion onto a small black hole at the center of a neutron star. PHYSICAL REVIEW. D. (2016) 2021; 103:104009. [PMID: 34651092 PMCID: PMC8507166 DOI: 10.1103/physrevd.103.104009] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/13/2023]
Abstract
We revisit the system consisting of a neutron star that harbors a small, possibly primordial, black hole at its center, focusing on a nonspinning black hole embedded in a nonrotating neutron star. Extending earlier treatments, we provide an analytical treatment describing the rate of secular accretion of the neutron star matter onto the black hole, adopting the relativistic Bondi accretion formalism for stiff equations of state that we presented elsewhere. We use these accretion rates to sketch the evolution of the system analytically until the neutron star is completely consumed. We also perform numerical simulations in full general relativity for black holes with masses up to nine orders of magnitude smaller than the neutron star mass, including a simulation of the entire evolution through collapse for the largest black hole mass. We construct relativistic initial data for these simulations by generalizing the black hole puncture method to allow for the presence of matter, and evolve these data with a code that is optimally designed to resolve the vastly different length scales present in this problem. We compare our analytic and numerical results, and provide expressions for the lifetime of neutron stars harboring such endoparasitic black holes.
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Affiliation(s)
- Chloe B Richards
- Department of Physics and Astronomy, Bowdoin College, Brunswick, Maine 04011, USA
| | - Thomas W Baumgarte
- Department of Physics and Astronomy, Bowdoin College, Brunswick, Maine 04011, USA
| | - Stuart L Shapiro
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
- Department of Astronomy and NCSA, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
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23
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Wessel E, Paschalidis V, Tsokaros A, Ruiz M, Shapiro SL. Gravitational waves from disks around spinning black holes: Simulations in full general relativity. PHYSICAL REVIEW. D. (2016) 2021; 103:043013. [PMID: 34595363 PMCID: PMC8477220 DOI: 10.1103/physrevd.103.043013] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/13/2023]
Abstract
We present fully general-relativistic numerical evolutions of self-gravitating tori around spinning black holes with dimensionless spin a/M = 0.7 parallel or antiparallel to the disk angular momentum. The initial disks are unstable to the hydrodynamic Papaloizou-Pringle instability which causes them to grow persistent orbiting matter clumps. The effect of black hole spin on the growth and saturation of the instability is assessed. We find that the instability behaves similarly to prior simulations with nonspinning black holes, with a shift in frequency due to spin-induced changes in disk orbital period. Copious gravitational waves are generated by these systems, and we analyze their detectability by current and future gravitational wave observatories for a large range of masses. We find that systems of 10 M ⊙-relevant for black hole-neutron star mergers-are detectable by Cosmic Explorer out to ~300 Mpc, while DECIGO (LISA) will be able to detect systems of 1000 M ⊙ (105 M ⊙)-relevant for disks forming in collapsing supermassive stars-out to cosmological redshift of z ~ 5 (z ~ 1). Computing the accretion rate of these systems we find that these systems may also be promising sources of coincident electromagnetic signals.
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Affiliation(s)
- Erik Wessel
- Department of Physics, University of Arizona, Tucson, Arizona 85721, USA
| | - Vasileios Paschalidis
- Departments of Astronomy and Physics, University of Arizona, Tucson, Arizona 85721, USA
| | - Antonios Tsokaros
- Department of Physics, University of Illinois, Urbana-Champaign, Illinois 61801, USA
| | - Milton Ruiz
- Department of Physics, University of Illinois, Urbana-Champaign, Illinois 61801, USA
| | - Stuart L Shapiro
- Departments of Physics and Astronomy, University of Illinois, Urbana-Champaign, Illinois 61801, USA
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Bozzola G, Paschalidis V. General Relativistic Simulations of the Quasicircular Inspiral and Merger of Charged Black Holes: GW150914 and Fundamental Physics Implications. PHYSICAL REVIEW LETTERS 2021; 126:041103. [PMID: 33576671 DOI: 10.1103/physrevlett.126.041103] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/01/2020] [Revised: 10/02/2020] [Accepted: 01/05/2021] [Indexed: 06/12/2023]
Abstract
We perform general-relativistic simulations of charged black holes targeting GW150914. We show that the inspiral is most efficient for detecting black hole charge through gravitational waves and that GW150914 is compatible with having charge-to-mass ratio as high as 0.3. Our work applies to electric and magnetic charge and to theories with black holes endowed with U(1) (hidden or dark) charges. Using our results, we place an upper bound on the deviation from general relativity in the dynamical strong-filed regime of Moffat's modified gravity.
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Affiliation(s)
- Gabriele Bozzola
- Department of Astronomy, University of Arizona, Tucson, Arizona 85721, USA
| | - Vasileios Paschalidis
- Departments of Astronomy and Physics, University of Arizona, Tucson, Arizona 85721, USA
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25
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Ruiz M, Paschalidis V, Tsokaros A, Shapiro SL. Black hole-neutron star coalescence: Effects of the neutron star spin on jet launching and dynamical ejecta mass. PHYSICAL REVIEW. D. (2016) 2020; 102:124077. [PMID: 34595362 PMCID: PMC8477222 DOI: 10.1103/physrevd.102.124077] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/13/2023]
Abstract
Black hole-neutron star (BHNS) mergers are thought to be sources of gravitational waves (GWs) with coincident electromagnetic (EM) counterparts. To further probe whether these systems are viable progenitors of short gamma-ray bursts (SGRBs) and kilonovas, and how one may use (the lack of) EM counterparts associated with LIGO/Virgo candidate BHNS GW events to sharpen parameter estimation, we study the impact of neutron star spin in BHNS mergers. Using dynamical spacetime magnetohydrodynamic simulations of BHNSs initially on a quasicircular orbit, we survey configurations that differ in the BH spin (a BH/M BH = 0 and 0.75), the NS spin (a NS/M NS = -0.17, 0, 0.23, and 0.33), and the binary mass ratio (q = M BH:M NS = 3:1 and 5:1). The general trend we find is that increasing the NS prograde spin increases both the rest mass of the accretion disk onto the remnant black hole, and the rest mass of dynamically ejected matter. By a time Δt ~ 3500-5500M ~ 88-138(M NS/1.4 M ⊙) ms after the peak gravitational-wave amplitude, a magnetically driven jet is launched only for q = 3:1 regardless of the initial NS spin. The lifetime of the jets [Δt ~ 0.5-0.8(M NS/1.4 M ⊙) s] and their outgoing Poynting luminosity [L Poyn ~ 1051.5±0.5 erg/s] are consistent with typical SGRBs' luminosities and expectations from the Blandford-Znajek mechanism. By the time we terminate our simulations, we do not observe either an outflow or a large-scale magnetic-field collimation for the other systems we consider. The mass range of dynamically ejected matter is 10-4.5-10-2(M NS/1.4 M ⊙) M ⊙, which can power kilonovas with peak bolometric luminosities L knova ~ 1040-1041.4 erg/s with rise times ≲6.5 h and potentially detectable by the LSST.
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Affiliation(s)
- Milton Ruiz
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Vasileios Paschalidis
- Departments of Astronomy and Physics, University of Arizona, Tucson, Arizona 85719, USA
| | - Antonios Tsokaros
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Stuart L Shapiro
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
- Department of Astronomy and NCSA, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
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Bernuzzi S. Neutron star merger remnants. GENERAL RELATIVITY AND GRAVITATION 2020; 52:108. [PMID: 39247669 PMCID: PMC11377492 DOI: 10.1007/s10714-020-02752-5] [Citation(s) in RCA: 9] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 04/21/2020] [Accepted: 10/09/2020] [Indexed: 09/10/2024]
Abstract
Binary neutron star mergers observations are a unique way to constrain fundamental physics and astrophysics at the extreme. The interpretation of gravitational-wave events and their electromagnetic counterparts crucially relies on general-relativistic models of the merger remnants. Quantitative models can be obtained only by means of numerical relativity simulations in 3 + 1 dimensions including detailed input physics for the nuclear matter, electromagnetic and weak interactions. This review summarizes the current understanding of merger remnants focusing on some of the aspects that are relevant for multimessenger observations.
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Affiliation(s)
- Sebastiano Bernuzzi
- Theoretisch-Physikalisches Institut, Friedrich-Schiller-Universität Jena, Max-Wien-Platz 1, 07743 Jena, Germany
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27
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Healy J, Lousto CO, Rosato N. Adapted gauge to a quasilocal measure of the black holes recoil. Int J Clin Exp Med 2020. [DOI: 10.1103/physrevd.102.024040] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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28
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Fujibayashi S, Shibata M, Wanajo S, Kiuchi K, Kyutoku K, Sekiguchi Y. Mass ejection from disks surrounding a low-mass black hole: Viscous neutrino-radiation hydrodynamics simulation in full general relativity. Int J Clin Exp Med 2020. [DOI: 10.1103/physrevd.101.083029] [Citation(s) in RCA: 45] [Impact Index Per Article: 11.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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29
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Ruiz M, Tsokaros A, Shapiro SL. Magnetohydrodynamic simulations of binary neutron star mergers in general relativity: Effects of magnetic field orientation on jet launching. PHYSICAL REVIEW. D. (2016) 2020; 101:064042. [PMID: 34589635 PMCID: PMC8477221 DOI: 10.1103/physrevd.101.064042] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/13/2023]
Abstract
Binary neutron star mergers can be sources of gravitational waves coincident with electromagnetic counterpart emission across the spectrum. To solidify their role as multimessenger sources, we present fully 3D, general relativistic, magnetohydrodynamic simulations of highly spinning binary neutrons stars initially on quasicircular orbits that merge and undergo delayed collapse to a black hole. The binaries consist of two identical stars modeled as Γ = 2 polytropes with spin χ NS = 0.36 aligned along the direction of the total orbital angular momentum L. Each star is initially threaded by a dynamical unimportant interior dipole magnetic field. The field is extended into the exterior where a nearly force-free magnetosphere resembles that of a pulsar. The magnetic dipole moment μ is either aligned or perpendicular to L and has the same initial magnitude for each orientation. For comparison, we also impose symmetry across the orbital plane in one case where μ in both stars is aligned along L. We find that the lifetime of the transient hypermassive neutron star remnant, the jet launching time, and the ejecta (which can give rise to a detectable kilonova) are very sensitive to the magnetic field orientation. By contrast, the physical properties of the black hole + disk remnant, such as the mass and spin of the black hole, the accretion rate, and the electromagnetic (Poynting) luminosity, are roughly independent of the initial magnetic field orientation. In addition, we find imposing symmetry across the orbital plane does not play a significant role in the final outcome of the mergers. Our results suggest that, as in the black hole-neutron star merger scenario, an incipient jet emerges only when the seed magnetic field has a sufficiently large-scale poloidal component aligned to the initial orbital angular momentum. The lifetime [Δt ≳ 140(M NS/1.625 M ⊙) ms] and Poynting luminosities [L EM ≃ 1052 erg/s] of the jet, when it forms, are consistent with typical short gamma-ray bursts, as well as with the Blandford-Znajek mechanism for launching jets.
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Affiliation(s)
- Milton Ruiz
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, IL 61801
| | - Antonios Tsokaros
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, IL 61801
| | - Stuart L Shapiro
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, IL 61801
- Department of Astronomy & NCSA, University of Illinois at Urbana-Champaign, Urbana, IL 61801
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Tsokaros A, Ruiz M, Shapiro SL, Sun L, Uryū K. Great Impostors: Extremely Compact, Merging Binary Neutron Stars in the Mass Gap Posing as Binary Black Holes. PHYSICAL REVIEW LETTERS 2020; 124:071101. [PMID: 32142310 DOI: 10.1103/physrevlett.124.071101] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/15/2019] [Revised: 12/20/2019] [Accepted: 01/27/2020] [Indexed: 06/10/2023]
Abstract
Can one distinguish a binary black hole undergoing a merger from a binary neutron star if the individual compact companions have masses that fall inside the so-called mass gap of 3-5 M_{⊙}? For neutron stars, achieving such masses typically requires extreme compactness and in this work we present initial data and evolutions of binary neutron stars initially in quasiequilibrium circular orbits having a compactness C=0.336. These are the most compact, nonvacuum, quasiequilibrium binary objects that have been constructed and evolved to date, including boson stars. The compactness achieved is only slightly smaller than the maximum possible imposed by causality, C_{max}=0.355, which requires the sound speed to be less than the speed of light. By comparing the emitted gravitational waveforms from the late inspiral to merger and postmerger phases between such a binary neutron star vs a binary black hole of the same total mass we identify concrete measurements that serve to distinguish them. With that level of compactness, the binary neutron stars exhibit no tidal disruption up until merger, whereupon a prompt collapse is initiated even before a common core forms. Within the accuracy of our simulations the black hole remnants from both binaries exhibit ringdown radiation that is not distinguishable from a perturbed Kerr spacetime. However, their inspiral leads to phase differences of the order of ∼5 rad over an ∼81 km separation (1.7 orbits) while typical neutron stars exhibit phase differences of ≥20 rad. Although a difference of ∼5 rad can be measured by current gravitational wave laser interferometers (e.g., aLIGO/Virgo), uncertainties in the individual masses and spins will likely prevent distinguishing such compact, massive neutron stars from black holes.
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Affiliation(s)
- Antonios Tsokaros
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Milton Ruiz
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Stuart L Shapiro
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
- Department of Astronomy & NCSA, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Lunan Sun
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Kōji Uryū
- Department of Physics, University of the Ryukyus, Senbaru, Nishihara, Okinawa 903-0213, Japan
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Sperhake U, Rosca-Mead R, Gerosa D, Berti E. Amplification of superkicks in black-hole binaries through orbital eccentricity. Int J Clin Exp Med 2020. [DOI: 10.1103/physrevd.101.024044] [Citation(s) in RCA: 9] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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32
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Tsokaros A, Ruiz M, Sun L, Shapiro SL, Uryū K. Dynamically Stable Ergostars Exist: General Relativistic Models and Simulations. PHYSICAL REVIEW LETTERS 2019; 123:231103. [PMID: 31868499 DOI: 10.1103/physrevlett.123.231103] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/08/2019] [Revised: 10/10/2019] [Indexed: 06/10/2023]
Abstract
We construct the first dynamically stable ergostars (equilibrium neutron stars that contain an ergoregion) for a compressible, causal equation of state. We demonstrate their stability by evolving both strict and perturbed equilibrium configurations in full general relativity for over a hundred dynamical timescales (≳30 rotational periods) and observing their stationary behavior. This stability is in contrast to earlier models which prove radially unstable to collapse. Our solutions are highly differentially rotating hypermassive neutron stars with a corresponding spherical compaction of C=0.3. Such ergostars can provide new insights into the geometry of spacetimes around highly compact, rotating objects and on the equation of state at supranuclear densities. Ergostars may form as remnants of extreme binary neutron star mergers and possibly provide another mechanism for powering short gamma-ray bursts.
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Affiliation(s)
- Antonios Tsokaros
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Milton Ruiz
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Lunan Sun
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Stuart L Shapiro
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
- Department of Astronomy & NCSA, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Kōji Uryū
- Department of Physics, University of the Ryukyus, Senbaru, Nishihara, Okinawa 903-0213, Japan
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33
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Baumgarte TW, Gundlach C, Hilditch D. Critical Phenomena in the Gravitational Collapse of Electromagnetic Waves. PHYSICAL REVIEW LETTERS 2019; 123:171103. [PMID: 31702276 DOI: 10.1103/physrevlett.123.171103] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/02/2019] [Indexed: 06/10/2023]
Abstract
We numerically investigate the threshold of black-hole formation in the gravitational collapse of electromagnetic waves in axisymmetry. We find approximate power-law scaling ρ_{max}∼(η_{*}-η)^{-2γ} of the maximum density in the time evolution of near-subcritical data with γ≃0.145, where η is the amplitude of the initial data. We directly observe approximate discrete self-similarity in near-critical time evolutions with a log-scale echoing period of Δ≃0.55. The critical solution is approximately the same for two families of initial data, providing some evidence of universality. Neither the discrete self-similarity nor the universality, however, are exact. We speculate that the absence of an exactly discrete self-similarity might be caused by the interplay of electromagnetic and gravitational wave degrees of freedom, or by the presence of higher-order angular multipoles, or both, and discuss implications of our findings for the critical collapse of vacuum gravitational waves.
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Affiliation(s)
- Thomas W Baumgarte
- Department of Physics and Astronomy, Bowdoin College, Brunswick, Maine 04011, USA
| | - Carsten Gundlach
- Mathematical Sciences, University of Southampton, Southampton SO17 1BJ, United Kingdom
| | - David Hilditch
- CENTRA, Departamento de Física, Instituto Superior Técnico IST, Universidade de Lisboa UL, Avenida Rovisco Pais 1, 1049 Lisboa, Portugal
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34
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35
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Tsokaros A, Ruiz M, Paschalidis V, Shapiro SL, Uryū K. Effect of spin on the inspiral of binary neutron stars. Int J Clin Exp Med 2019. [DOI: 10.1103/physrevd.100.024061] [Citation(s) in RCA: 19] [Impact Index Per Article: 3.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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36
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Abstract
The long-awaited detection of a gravitational wave from the merger of a binary neutron star in August 2017 (GW170817) marks the beginning of the new field of multi-messenger gravitational wave astronomy. By exploiting the extracted tidal deformations of the two neutron stars from the late inspiral phase of GW170817, it is now possible to constrain several global properties of the equation of state of neutron star matter. However, the most interesting part of the high density and temperature regime of the equation of state is solely imprinted in the post-merger gravitational wave emission from the remnant hypermassive/supramassive neutron star. This regime was not observed in GW170817, but will possibly be detected in forthcoming events within the current observing run of the LIGO/VIRGO collaboration. Numerous numerical-relativity simulations of merging neutron star binaries have been performed during the last decades, and the emitted gravitational wave profiles and the interior structure of the generated remnants have been analysed in detail. The consequences of a potential appearance of a hadron-quark phase transition in the interior region of the produced hypermassive neutron star and the evolution of its underlying matter in the phase diagram of quantum cromo dynamics will be in the focus of this article. It will be shown that the different density/temperature regions of the equation of state can be severely constrained by a measurement of the spectral properties of the emitted post-merger gravitational wave signal from a future binary compact star merger event.
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37
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Rosofsky SG, Gold R, Chirenti C, Huerta E, Miller MC. Probing neutron star structure via
f
-mode oscillations and damping in dynamical spacetime models. Int J Clin Exp Med 2019. [DOI: 10.1103/physrevd.99.084024] [Citation(s) in RCA: 7] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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38
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Hinder I, Ossokine S, Pfeiffer HP, Buonanno A. Gravitational waveforms for high spin and high mass-ratio binary black holes: A synergistic use of numerical-relativity codes. Int J Clin Exp Med 2019. [DOI: 10.1103/physrevd.99.061501] [Citation(s) in RCA: 5] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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39
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Uchida H, Shibata M, Takahashi K, Yoshida T. Gravitational waves from very massive stars collapsing to a black hole. Int J Clin Exp Med 2019. [DOI: 10.1103/physrevd.99.041302] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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40
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Chakravarti K, Gupta A, Bose S, Duez MD, Caro J, Brege W, Foucart F, Ghosh S, Kyutoku K, Lackey BD, Shibata M, Hemberger DA, Kidder LE, Pfeiffer HP, Scheel MA. Systematic effects from black hole-neutron star waveform model uncertainties on the neutron star equation of state. Int J Clin Exp Med 2019. [DOI: 10.1103/physrevd.99.024049] [Citation(s) in RCA: 7] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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41
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42
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Ramos-Buades A, Husa S, Pratten G. Simple procedures to reduce eccentricity of binary black hole simulations. Int J Clin Exp Med 2019. [DOI: 10.1103/physrevd.99.023003] [Citation(s) in RCA: 12] [Impact Index Per Article: 2.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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43
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Duez MD, Zlochower Y. Numerical relativity of compact binaries in the 21st century. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2019; 82:016902. [PMID: 30117809 DOI: 10.1088/1361-6633/aadb16] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/08/2023]
Abstract
We review the dramatic progress in the simulations of compact objects and compact-object binaries that has taken place in the first two decades of the twenty-first century. This includes simulations of the inspirals and violent mergers of binaries containing black holes and neutron stars, as well as simulations of black-hole formation through failed supernovae and high-mass neutron star-neutron star mergers. Modeling such events requires numerical integration of the field equations of general relativity in three spatial dimensions, coupled, in the case of neutron-star containing binaries, with increasingly sophisticated treatment of fluids, electromagnetic fields, and neutrino radiation. However, it was not until 2005 that accurate long-term evolutions of binaries containing black holes were even possible (Pretorius 2005 Phys. Rev. Lett. 95 121101, Campanelli et al 2006 Phys. Rev. Lett. 96 111101, Baker et al 2006 Phys. Rev. Lett. 96 111102). Since then, there has been an explosion of new results and insights into the physics of strongly-gravitating system. Particular emphasis has been placed on understanding the gravitational wave and electromagnetic signatures from these extreme events. And with the recent dramatic discoveries of gravitational waves from merging black holes by the Laser Interferometric Gravitational Wave Observatory and Virgo, and the subsequent discovery of both electromagnetic and gravitational wave signals from a merging neutron star-neutron star binary, numerical relativity became an indispensable tool for the new field of multimessenger astronomy.
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Affiliation(s)
- Matthew D Duez
- Department of Physics and Astronomy, Washington State University, Pullman, WA 99164, United States of America
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44
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Sun L, Ruiz M, Shapiro SL. Simulating the magnetorotational collapse of supermassive stars: Incorporating gas pressure perturbations and different rotation profiles. PHYSICAL REVIEW. D. (2016) 2018; 98:103008. [PMID: 34589637 PMCID: PMC8477203 DOI: 10.1103/physrevd.98.103008] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/13/2023]
Abstract
Collapsing supermassive stars (SMSs) with masses M ≳ 104-6 M ⊙ have long been speculated to be the seeds that can grow and become supermassive black holes (SMBHs). We previously performed general relativistic magnetohydrodynamic (GRMHD) simulations of marginally stable Γ = 4/3 polytropes uniformly rotating at the mass-shedding limit and endowed initially with a dynamically unimportant dipole magnetic field to model the direct collapse of SMSs. These configurations are supported entirely by thermal radiation pressure and reliably model SMSs with M ≳ 106 M ⊙. We found that around 90% of the initial stellar mass forms a spinning black hole (BH) remnant surrounded by a massive, hot, magnetized torus, which eventually launches a magnetically-driven jet. SMSs could be therefore sources of ultra-long gamma-ray bursts (ULGRBs). Here we perform GRMHD simulations of Γ ≳ 4/3, polytropes to account for the perturbative role of gas pressure in SMSs with M ≲ 106 M ⊙. We also consider different initial stellar rotation profiles. The stars are initially seeded with a dynamically weak dipole magnetic field that is either confined to the stellar interior or extended from its interior into the stellar exterior. We calculate the gravitational wave burst signal for the different cases. We find that the mass of the black hole remnant is 90%-99% of the initial stellar mass, depending sharply on Γ - 4/3 as well as on the initial stellar rotation profile. After t ~ 250-550M ≈ 1 - 2 × 103(M/106 M ⊙) s following the appearance of the BH horizon, an incipient jet is launched and it lasts for ~104-105(M/106 M ⊙) s, consistent with the duration of long gamma-ray bursts. Our numerical results suggest that the Blandford-Znajek mechanism powers the incipient jet. They are also in rough agreement with our recently proposed universal model that estimates accretion rates and electromagnetic (Poynting) luminosities that characterize magnetized BH-disk remnant systems that launch a jet. This model helps explain why the outgoing electromagnetic luminosities computed for vastly different BH-disk formation scenarios all reside within a narrow range (~1052±1 erg s-1), roughly independent of M.
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Affiliation(s)
- Lunan Sun
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Milton Ruiz
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Stuart L Shapiro
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
- Department of Astronomy & NCSA, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
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45
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Chaurasia SV, Dietrich T, Johnson-McDaniel NK, Ujevic M, Tichy W, Brügmann B. Gravitational waves and mass ejecta from binary neutron star mergers: Effect of large eccentricities. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.98.104005] [Citation(s) in RCA: 32] [Impact Index Per Article: 5.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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46
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Abstract
Einstein's theory of general relativity affords an enormously successful description of gravity. The theory encodes the gravitational interaction in the metric, a tensor field on spacetime that satisfies partial differential equations known as the Einstein equations. This review introduces some of the fundamental concepts of numerical relativity-solving the Einstein equations on the computer-in simple terms. As a primary example, we consider the solution of the general relativistic two-body problem, which features prominently in the new field of gravitational wave astronomy.
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Affiliation(s)
- Bernd Brügmann
- Theoretical Physics Institute, University of Jena, 07743 Jena, Germany.
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47
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Optimization of Finite-Differencing Kernels for Numerical Relativity Applications. JOURNAL OF LOW POWER ELECTRONICS AND APPLICATIONS 2018. [DOI: 10.3390/jlpea8020015] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/17/2022]
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48
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Dumbser M, Guercilena F, Köppel S, Rezzolla L, Zanotti O. Conformal and covariant Z4 formulation of the Einstein equations: Strongly hyperbolic first-order reduction and solution with discontinuous Galerkin schemes. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.97.084053] [Citation(s) in RCA: 27] [Impact Index Per Article: 4.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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49
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Sadiq J, Zlochower Y, Nakano H. Comparing an analytical spacetime metric for a merging binary to a fully nonlinear numerical evolution using curvature scalars. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.97.084007] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/06/2022]
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50
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Ruchlin I, Etienne ZB, Baumgarte TW. SENR/NRPy+
: Numerical relativity in singular curvilinear coordinate systems. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.97.064036] [Citation(s) in RCA: 26] [Impact Index Per Article: 4.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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