Tuning Advanced LIGO to kilohertz signals from neutron-star collisions

Ganapathy, D.; McCuller, L.; Rollins, J. G.; Hall, E. D.; Barsotti, L.; Evans, M.

doi:10.1103/physrevd.103.022002

Cited by 28 publications

(19 citation statements)

References 30 publications

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“…Despite the sensitivity of the advanced LIGO and advanced Virgo detectors, these were not sensitive enough in order to determine the post-merger phase in GW170817 [43,61]. However, this post-merger phase may be revealed in the near future, by several experiments and collaborations, like [45], or by third-generation detectors [62,63], or even with high-frequency detectors [64,65]. The observation of GW in the post-merger phase of a BNS merger would then offer another opportunity to probe the high-density EoS of NSs, see [66][67][68][69][70][71][72][73][74][75][76][77].…”

Section: Introductionmentioning

confidence: 99%

Anisotropic Compact Stars in D → 4 Limit of Gauss–Bonnet Gravity

2022

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In the frame of Gauss–Bonnet gravity and in the limit of D→4, based on the fact that spherically symmetric solution derived using any of regularization schemes will be the same form as the original theory, we derive a new interior spherically symmetric solution assuming specific forms of the metric potentials that have two constants. Using the junction condition we determine these two constants. By using the data of the star EXO 1785-248, whose mass is M=1.3±0.2M⊙ and radius l=8.849±0.4 km, we calculate the numerical values of these constants, in terms of the dimensionful coupling parameter of the Gauss–Bonnet term, and eventually, we get real values for these constants. In this regard, we show that the components of the energy–momentum tensor have a finite value at the center of the star as well as a smaller value to the surface of the star. Moreover, we show that the equations of the state behave in a non-linear way due to the impact of the Gauss–Bonnet term. Using the Tolman–Oppenheimer–Volkoff equation, the adiabatic index, and stability in the static state we show that the model under consideration is always stable. Finally, the solution of this study is matched with observational data of other pulsars showing satisfactory results.

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Section: Introductionmentioning

confidence: 99%

Anisotropic Compact Stars in D → 4 Limit of Gauss–Bonnet Gravity

2022

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“…The sensitivity of the LIGO and Virgo GW detectors was not sufficient to detect the post-merger phase of the BNS merger GW170817 [20,21], or the likely BNS merger GW190425 [22]. However, a post-merger detection is expected to be achieved in the near future, either with upgraded or next-generation detectors [12,[23][24][25][26][27][28][29][30][31][32][33][34][35][36][37][38][39].…”

Section: Introductionmentioning

confidence: 99%

Frequency deviations in universal relations of isolated neutron stars and postmerger remnants

Lioutas,

Bauswein,

Stergioulas

2021

Preprint

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We relate the fundamental quadrupolar fluid mode of isolated non-rotating NSs and the dominant oscillation frequency of neutron star merger remnants. Both frequencies individually are known to correlate with certain stellar parameters like radii or the tidal deformability, which we further investigate by constructing fit formulae and quantifying the scatter of the data points from those relations. Furthermore, we compare how individual data points deviate from the corresponding fit to all data points. Considering this point-to-point scatter we uncover a striking similarity between the frequency deviations of perturbative data for isolated NSs and of oscillation frequencies of rapidly rotating, hot, massive merger remnants. The correspondence of frequency deviations in these very different stellar systems points to an underlying mechanism and EoS information being encoded in the frequency deviation. We trace the frequency scatter back to deviations of the tidal Love number from an average tidal Love number for a given stellar compactness. Our results thus indicate a possibility to break the degeneracy between NS radii, tidal deformability and tidal Love number. We also relate frequency deviations to the derivative of the tidal deformability with respect to mass. Our findings generally highlight a possibility to improve GW asteroseismology relations where the systematic behavior of frequency deviations is employed to reduce the scatter in such relationships and consequently increase the measurement accuracy. In addition, we relate the f −mode frequency of static stars and the dominant GW frequency of merger remnants. We find an analytic mapping to connect the masses of both stellar systems, which yields particularly accurate mass-independent relations between both frequencies and between the postmerger frequency and the tidal deformability.

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“…Significant improvement on these EoS constraints are expected by combining a larger number of detections in the near future [18][19][20][21][22]. Although the sensitivity of the Advanced LIGO and Advanced Virgo detectors was not sufficient to detect the post-merger phase in GW170817 [1,4,23], such detections are likely to be achieved in the future, with upgraded [24], with dedicated high-frequency [25][26][27][28][29] or with third-generation [30,31] detectors. Such observations of GWs in the postmerger phase of BNS mergers would offer a tremendous opportunity to probe the high-density EoS, see [13, and references therein.…”

Section: Introductionmentioning

confidence: 99%

Analytic models of the spectral properties of gravitational waves from neutron star merger remnants

Soultanis,

Bauswein,

Stergioulas

2021

Preprint

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We present a new analytic model describing gravitational wave emission in the post-merger phase of binary neutron star mergers. The model is described by a number of physical parameters that are related to various oscillation modes, quasi-linear combination tones or non-linear features that appear in the post-merger phase. The time evolution of the main post-merger frequency peak is taken into account and it is described by a two-segment linear expression. The effectiveness of the model, in terms of the fitting factor or, equivalently, the reduction in the detection rate, is evaluated along a sequence of equal-mass simulations of varying mass. We find that all parameters of the analytic model correlate with the total binary mass of the system. For high masses, we identify new spectral features originating from the non-linear coupling between the quasi-radial oscillation and the antipodal tidal deformation, the inclusion of which significantly improves the fitting factors achieved by the model. We can thus model the post-merger gravitational-wave emission with an analytic model that achieves high fitting factors for a wide range of total binary masses. Our model can be used for the detection and parameter estimation of the post-merger phase in upcoming searches with upgraded second-generation detectors, such as aLIGO+ and aVirgo+, with future, third-generation detectors (Einstein Telescope and Cosmic Explorer) or with dedicated, high-frequency detectors.

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Tuning Advanced LIGO to kilohertz signals from neutron-star collisions

Cited by 28 publications

References 30 publications

Anisotropic Compact Stars in D → 4 Limit of Gauss–Bonnet Gravity

Anisotropic Compact Stars in D → 4 Limit of Gauss–Bonnet Gravity

Frequency deviations in universal relations of isolated neutron stars and postmerger remnants

Analytic models of the spectral properties of gravitational waves from neutron star merger remnants

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