Gravitational waves and mass ejecta from binary neutron star mergers: Effect of the spin orientation

Chaurasia, Swami Vivekanandji; Dietrich, Tim; Ujevic, Maximiliano; Hendriks, Kai; Dudi, Reetika; Fabbri, Francesco Maria; Tichy, Wolfgang; Brügmann, Bernd

doi:10.1103/physrevd.102.024087

Cited by 20 publications

(24 citation statements)

References 79 publications

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“…Studying the energetics during the postmerger, one finds that spin aligned systems can create merger remnants with larger angular momentum than non-spinning systems. Consequently, collapse to a BH happens at later times [125]. We note that simulations also indicate that characteristic frequencies in the postmerger, which generally also follow quasi-universal relations [57,58,64,133,470,509,510], might shift under the presence of spin.…”

Section: Spinmentioning

confidence: 61%

“…The main advantage of NR simulations is that the Einstein Equations can be solved directly by numerical discretization of the equations. Over the last years, the NR community has made tremendous progress on several fronts: (i) the exploration of the BNS parameter space by systematically varying the EOSs, total mass, mass ratio, spin, and eccentricity, e.g., [65,66,71,125,174,177,180,183,[191][192][193][194]226,242,275,287,288,295,333,389,425,453,475,487,507,530,532]; (ii) the development of numerical schemes allowing many-orbits simulations with high-accuracy GWs, e.g., [63,72,175,274,277,294,455]; (iii) the increasing realism of microphysical schemes that incorporate magnetic effects, finite-temperature EOSs, composition effects, and neutrino transport, e.g., [26,130,224,228,229,231,235,240,296,297,…”

Section: Numerical Relativity Simulationsmentioning

confidence: 99%

“…In the past, consistently evolved spinning BNS simulations have been presented in Refs. [65,173,177,180,193,390,533] and precessing NR simulations are presented only in [125,174,180,507].…”

Section: Spinmentioning

confidence: 99%

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Interpreting binary neutron star mergers: describing the binary neutron star dynamics, modelling gravitational waveforms, and analyzing detections

2021

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Gravitational waves emitted from the coalescence of neutron star binaries open a new window to probe matter and fundamental physics in unexplored, extreme regimes. To extract information about the supranuclear matter inside neutron stars and the properties of the compact binary systems, robust theoretical prescriptions are required. We give an overview about general features of the dynamics and the gravitational wave signal during the binary neutron star coalescence. We briefly describe existing analytical and numerical approaches to investigate the highly dynamical, strong-field region during the merger. We review existing waveform approximants and discuss properties and possible advantages and shortcomings of individual waveform models, and their application for real gravitational-wave data analysis.

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Section: Spinmentioning

confidence: 61%

Section: Numerical Relativity Simulationsmentioning

confidence: 99%

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Interpreting binary neutron star mergers: describing the binary neutron star dynamics, modelling gravitational waveforms, and analyzing detections

2021

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“…This assumption is based on the spin distribution of Galactic BNSs, which indicates that the magnitude of the dimensionless spin parameter χ = cIω/(GM 2 ) 0.05 (Zhu et al 2018). In general, however, the spin of the neutron star may have a significant effect on the outflows (see, e.g., East et al 2019;Most et al 2019;Chaurasia et al 2020). For a BHNS system, the parameters of interest for the neutron star are again the mass and the tidal deformability.…”

Section: Connecting Binary Progenitor To Outflow Propertiesmentioning

confidence: 99%

The Challenges Ahead for Multimessenger Analyses of Gravitational Waves and Kilonova: A Case Study on GW190425

Raaijmakers

Nissanke

Foucart

et al. 2021

ApJ

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In recent years, there have been significant advances in multimessenger astronomy due to the discovery of the first, and so far only confirmed, gravitational wave event with a simultaneous electromagnetic (EM) counterpart, as well as improvements in numerical simulations, gravitational wave (GW) detectors, and transient astronomy. This has led to the exciting possibility of performing joint analyses of the GW and EM data, providing additional constraints on fundamental properties of the binary progenitor and merger remnant. Here, we present a new Bayesian framework that allows inference of these properties, while taking into account the systematic modeling uncertainties that arise when mapping from GW binary progenitor properties to photometric light curves. We extend the relative binning method presented in Zackay et al. to include extrinsic GW parameters for fast analysis of the GW signal. The focus of our EM framework is on light curves arising from r-process nucleosynthesis in the ejected material during and after merger, the so-called kilonova, and particularly on black hole−neutron star systems. As a case study, we examine the recent detection of GW190425, where the primary object is consistent with being either a black hole or a neutron star. We show quantitatively how improved mapping between binary progenitor and outflow properties, and/or an increase in EM data quantity and quality are required in order to break degeneracies in the fundamental source parameters.

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“…They are characterized as having a mass greater than the maximum value for a uniformly rotating neutron star, but are supported against gravitational collapse by the differential motion of their interior fluids. Numerical simulations (for recent examples, see Kastaun & Galeazzi (2015); Kastaun et al (2017); Dietrich et al (2017); Radice et al (2018); Most et al (2019); Hanauske et al (2019); Ruiz et al (2020); Chaurasia et al (2020)) show that after a period of ∼ 10 ms of nonlinear evolution, post-merger objects settle into equilibria supported against collapse by differential rotation. These equilibria can be highly eccentric and emit gravitational radiation that could be detected by gravitational wave interferometers (Abbott et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Unstable modes of hypermassive compact stars driven by viscosity and gravitational radiation

Rau,

Sedrakian

2021

Preprint

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We study the oscillations modes of differential rotating remnants of binary neutron star inspirals by modeling them as incompressible Riemann ellipsoids parametrized by the ratio 𝑓 of their internal circulation to the rotation frequency. The effects of viscosity and gravitational wave radiation on the modes are studied and it is shown that these bodies exhibit generic instabilities towards gravitational wave radiation akin to the Chandrasekhar-Friedman-Schutz instabilities for uniformly rotating stars. The odd-parity modes are unstable for all values of 𝑓 (except for the spherical model) and deformations, whereas the even parity unstable modes appear only in highly eccentric ellipsoids. We quantify the modification of the modes with varying mass of the model and the magnitude of the viscosity. The modes are weakly dependent on the range of the masses relevant to the binary neutron star mergers. Large turbulent viscosity can lead to a suppression of the gravitational wave instabilities, whereas kinematical viscosity has a negligible influence on the modes and their damping timescales.

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Gravitational waves and mass ejecta from binary neutron star mergers: Effect of the spin orientation

Cited by 20 publications

References 79 publications

Interpreting binary neutron star mergers: describing the binary neutron star dynamics, modelling gravitational waveforms, and analyzing detections

Interpreting binary neutron star mergers: describing the binary neutron star dynamics, modelling gravitational waveforms, and analyzing detections

The Challenges Ahead for Multimessenger Analyses of Gravitational Waves and Kilonova: A Case Study on GW190425

Unstable modes of hypermassive compact stars driven by viscosity and gravitational radiation

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