Constraining the equation of state of nuclear matter with gravitational wave observations: Tidal deformability and tidal disruption

Maselli, Andrea; Gualtieri, Leonardo; Ferrari, Valeria

doi:10.1103/physrevd.88.104040

Cited by 57 publications

(50 citation statements)

References 57 publications

(127 reference statements)

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“…Understanding the magnitude of these two sources of error is the core motivator of this work. Several studies have used the Fisher information matrix (FM), which is only valid in the large signal-to-noise ratio (SNR) limit, to estimate the measurability of tidal effects on the CBC gravitational waveform [10][11][12][15][16][17][18]. Flanagan and Hinderer [10] were among the first to show that advanced detectors can constrain the tidal influence of NSs on the early inspiral portion of the CBC waveform.…”

Section: Background and Motivationmentioning

confidence: 99%

Systematic and statistical errors in a Bayesian approach to the estimation of the neutron-star equation of state using advanced gravitational wave detectors

et al. 2014

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Advanced ground-based gravitational-wave detectors are capable of measuring tidal influences in binary neutron-star systems. In this work, we report on the statistical uncertainties in measuring tidal deformability with a full Bayesian parameter estimation implementation. We show how simultaneous measurements of chirp mass and tidal deformability can be used to constrain the neutron-star equation of state. We also study the effects of waveform modeling bias and individual instances of detector noise on these measurements. We notably find that systematic error between post-Newtonian waveform families can significantly bias the estimation of tidal parameters, thus motivating the continued development of waveform models that are more reliable at high frequencies. DOI: 10.1103/PhysRevD.89.103012 PACS numbers: 95.85.Sz, 26.60.Kp I. BACKGROUND AND MOTIVATIONAdvanced interferometric gravitational-wave (GW) detectors currently under construction are expected to begin operating in the next few years. Advanced LIGO [1] is expected to achieve its design sensitivity c. 2019 [2], at which time the detection rate of binary neutron-star (BNS) events in a single detector is expected to be ∼40 yr −1 , though this value is quite uncertain and ranges from 0.4 − 400 yr −1 [3]. When a compact binary coalescence (CBC) signal is detected [4,5], the corresponding interferometer data stream segment is sent through a parameter estimation pipeline to determine the source parameters of the system. Some of these source parameters include the binary component masses and spins, the sky location, distance, and orientation of the system. Bayesian inference is used to explore the probability distribution of the CBC's source parameters by comparing model waveform templates, whose form depends on these source parameters, to the data stream segment containing the GW. For this work, we use LALINFERENCE_MCMC, which is included in the LALINFERENCE LSC Algorithm Library [6], as our parameter estimation pipeline. It is a Markov Chain Monte Carlo (MCMC) sampler designed to efficiently explore the full waveform parameter space in order to make reliable and meaningful statements about CBC source parameters [7][8][9]. This paper's focus is on measuring the effect of tidal influence on BNS GW signals with advanced detectors. Neutron stars (NSs) in merging CBC systems will be tidally deformed by the gravitational gradient of their companion across their finite diameter. This effect is insignificant at large separations but becomes increasingly significant as the NSs near each other [10]. The internal structure of a NS, which is characterized by its equation of state (EOS), determines how much each star will deform. The amount that a NS deforms will affect the orbital decay rate, which is encoded in the observed gravitational waveform. Therefore, if a gravitational signal from a BNS system is detected, then such a detection could provide insight into the NS EOS [10][11][12][13].In order to make meaningful statements regarding the recoverability of tidal param...

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Section: Background and Motivationmentioning

confidence: 99%

Systematic and statistical errors in a Bayesian approach to the estimation of the neutron-star equation of state using advanced gravitational wave detectors

et al. 2014

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“…What level of numerical approximation and how many macroscopic observable data points are needed to achieve reasonable levels of accuracy for "realistic" neutron-star equations of state? A number of researchers have studied various observational and data-analysis questions associated with the inverse stellar structure problem, both in the context of using mass and radius observations [15][16][17][18][19], and in the context of using mass and tidal deformability measurements from gravitational-wave observations [3][4][5][6][7][8][9][10][11][12][13][14]. To our knowledge, our studies of the more fundamental questions about solving the inverse stellar structure problem described in our papers are unique.…”

Section: Introductionmentioning

confidence: 97%

“…This may turn out to be the case, but the spectral approach for solving this problem does not (in principle) depend very strongly on exactly which observables are used. Recent work [3][4][5][6][7][8][9][10][11][12][13][14] has shown that gravitational-wave observations of binary neutron-star mergers should provide accurate measurements of the masses and tidal deformabilities of neutron stars once the advanced LIGO-VIRGO network of detectors becomes operational (within the next few years). The possibility of using this type of observational data to solve the inverse stellar structure problem is explored in Sec.…”

Section: Introductionmentioning

confidence: 99%

Spectral approach to the relativistic inverse stellar structure problem II

Lindblom

Indik

2014

Phys. Rev. D

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The inverse stellar structure problem determines the equation of state of the matter in stars from a knowledge of their macroscopic observables (e.g. their masses and radii). This problem was solved in a previous paper by constructing a spectral representation of the equation of state whose stellar models match a prescribed set of macroscopic observables. This paper improves and extends that work in two significant ways. (i) The method is made more robust by accounting for an unexpected feature of the enthalpy-based representations of the equations of state used in this work. After making the appropriate modifications, accurate initial guesses for the spectral parameters are no longer needed, so Monte Carlo techniques can now be used to ensure the best fit to the observables. (ii) The method is extended here to use masses and tidal deformabilities (which will be measured by gravitational wave observations of neutron-star mergers) as the macroscopic observables instead of masses and radii. The accuracy and reliability of this extended and more robust spectral method is evaluated in this paper using mock data for observables from stars based on 34 different theoretical models of the high-density neutron-star equation of state. In qualitative agreement with earlier work, these tests suggest the high-density part of the neutron-star equation of state could be determined at the few-percent accuracy level using high-quality measurements of the masses and radii (or masses and tidal deformabilities) of just two or three neutron stars.

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“…Measuring the NS deformability through GW detections would help to constrain the behavior of matter at ultranuclear density 18,[37][38][39][40] . This has motivated a vast literature on the tidal deformability of nonspinning NSs.…”

Section: Tidal Deformations Of Spinning Nssmentioning

confidence: 99%

“…On the one hand a deeper theoretical understanding of the tidal deformability within general relativity is highly desirable, because the nonlinearities of the theory introduce some subtleties in the definition of the tidal Love numbers 1,2 for relativistic compact objects 3,4 . On the other hand, the first direct detection of gravitational waves (GWs) by aLIGO 5 , the prospects of measuring the tidal Love numbers through GW detections of compact binaries [6][7][8][9][10][11][12][13][14][15][16][17][18] , and the related possibility of constraining the equation of state (EoS) of neutron stars (NSs) through GW astronomy, make it urgent to include spin-tidal effects in the gravitational waveforms. In this work we briefly review some recent results on the deformability and tidal Love numbers of spinning black holes (BHs) and NSs.…”

Section: Introductionmentioning

confidence: 99%

Recent progress on the tidal deformability of spinning compact objects

Pani

Gualtieri

Maselli

et al. 2017

The Fourteenth Marcel Grossmann Meeting

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We give a short review on recent progress in the theory of tidal deformability of a slowly spinning compact object. A rotating object immersed in a quadrupolar, electric tidal field can acquire some induced mass, spin, quadrupole, octupole and hexadecapole moments to second order in the spin. Angular momentum introduces couplings between electric and magnetic distortions and new classes of spin-induced, tidal Love numbers emerge. All tidal Love numbers of a Kerr black hole were proved to be exactly zero to first order in the spin and also to second order in the spin, at least in the axisymmetric case. The tidal Love numbers of a neutron star depend strongly on the equation of state. Spintidal couplings deteriorate some approximate universal relations that exist for neutron stars in the static case. For a binary system close to the merger, various components of the tidal field become relevant. Preliminary results suggest that spin-tidal couplings can introduce important corrections to the gravitational waveforms of spinning neutron-star binaries approaching the merger.

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Constraining the equation of state of nuclear matter with gravitational wave observations: Tidal deformability and tidal disruption

Cited by 57 publications

References 57 publications

Systematic and statistical errors in a Bayesian approach to the estimation of the neutron-star equation of state using advanced gravitational wave detectors

Systematic and statistical errors in a Bayesian approach to the estimation of the neutron-star equation of state using advanced gravitational wave detectors

Spectral approach to the relativistic inverse stellar structure problem II

Recent progress on the tidal deformability of spinning compact objects

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