Spectral analysis of gravitational waves from binary neutron star merger remnants

Maione, Francesco; Pietri, R. De; Feo, Alessandra; Löffler, Frank

doi:10.1103/physrevd.96.063011

Cited by 44 publications

(55 citation statements)

References 93 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…InFig.1, we show the emitted energy-density in the gravitational waves channel, on the right side, in order to allow a comparison of results with the EoS displayed on the left side. In such a demonstrative case, we have assumed the mass of the two Neutron Stars to be equal to each other 2 .Our numerical results are in agreement with the large numerical GR literature dedicated on Neutron Stars Merging -see e.g [69,70,71,72,73,74,75,76,77,78,79,80,81,82,83,84,85,86,87,88,89,90,91,92,93,94,95,96,97]…”

supporting

confidence: 77%

Testing merging of dark exotic stars from gravitational waves in the multi-messenger approach

Addazi

Marcianò

2018

Int. J. Mod. Phys. A

View full text Add to dashboard Cite

We discuss possible implications of the recent detection by the LIGO and VIRGO collaboration of the gravitational-wave event GW170817, the signal of which is consistent with predictions in general relativity on the merging of neutron stars. A near-simultaneous and spatially correlated observation of a gamma-ray burst, the GRB 170817A signal, was achieved independently by the Fermi Gamma-ray Burst Monitor, and by the Anti-coincidence Shield for the Spectrometer of the International Gamma-Ray Astrophysics Laboratory. Motivated by this near temporal and spatial concomitance of events, which can occur by chance only with the probability 5.0 × 10 −8 , we speculate on the possibility that new dark stars signals could be detected from the LIGO/VIRGO detectors. This proposal, which aims at providing a test for some models of dark matter, relies on the recent achievement of detecting, for visible ordinary matter, the merging of neutron stars both in the gravitational and the electromagnetic channel. A lack of correlation between the two expected signals would suggest a deviation from the properties of ordinary matter. Specifically, we focus on models of invisible dark matter, and in particular we study the case of mirror dark matter, within the framework of which a large amount of mirror neutron stars are naturally envisaged to occupy our dark matter halo. The observation of an electromagnetically hidden event inside the dark matter halo of our galaxy should provide a hint of new physics. There would be indeed no satisfactorily complete explanation accounting for the lack of electromagnetic signal, if only standard neutron star merging were considered to describe events that happen so close to us.

show abstract

supporting

confidence: 77%

Testing merging of dark exotic stars from gravitational waves in the multi-messenger approach

Addazi

Marcianò

2018

Int. J. Mod. Phys. A

View full text Add to dashboard Cite

show abstract

“…We also plot the f peak −R 1.6 fit obtained in [70], confirming that our simulations follow the empirical (EoS-insensitive) relation. Regarding subdominant peaks in the spectrum, we note that they can be generated by different physical mechanisms and that the strength of these different peaks can vary with the binary masses and the EoS [33,41,42,44,48,67,68,95] (see [44,68] for a unified picture of the postmerger dynamics and GW emission). In what follows and for the purposes on this study we do not distinguish between the different origin of subdominant features and define f sub as the frequency of the second highest peak with a frequency at least 400Hz below f peak .…”

Section: Simulated Post-merger Signalsmentioning

confidence: 99%

Observing the post-merger signal of GW170817-like events with improved gravitational-wave detectors

et al. 2019

View full text Add to dashboard Cite

The recent detection of a neutron star binary through gravitational waves, GW170817, has offered another source of information about the properties of cold supranuclear matter. Information from the signal emitted before the neutron stars merged has been used to study the equation of state of these bodies, however, any complementary information included in the signal emitted after the merger has been lost in the detector noise. In this paper we investigate the prospects of studying GW170817-like post-merger signals with future gravitational-wave detectors. We first compute the expected properties of the possible GW170817 post-merger signal using information from premerger analyses. We then quantify the required improvement in detector sensitivity in order to extract key features of the post-merger signal. We find that if we observe a signal of similar strength to GW170817 when the aLIGO detectors have been improved by ∼ 2 − 3 times over their design sensitivity in the kHz regime, we will be able to extract the dominant frequency component of the post-merger. With further improvements and next-generation detectors we will also be able to extract subdominant frequencies. We conclude that post-merger signals could be brought within our reach in the coming years given planned detector upgrades, such as A+, Voyager, and the next-generation detectors. arXiv:1811.08931v3 [gr-qc]

show abstract

“…The time of merging and the time of the collapse to a black hole are indicated by vertical, dotted red lines. For details on the numerical extraction of the GW signal see [59,65,79].…”

Section: A Matter Dynamics and Waveformsmentioning

confidence: 99%

Numerical-relativity simulations of long-lived remnants of binary neutron star mergers

et al. 2020

Self Cite

View full text Add to dashboard Cite

We analyze the properties of the gravitational wave signal emitted after the merger of a binary neutron star system when the remnant survives for more than a 80 ms (and up to 140 ms). We employ four different piecewise polytropic equations of state supplemented by an ideal fluid thermal component. We find that the post-merger phase can be subdivided into three phases: an early post-merger phase (where the quadrupole mode and a few subdominant features are active), the intermediate post-merger phase (where only the quadrupole mode is active) and the late post-merger phase (where convective instabilities trigger inertial modes). The inertial modes have frequencies somewhat smaller than the quadrupole modes. In one model, we find an interesting association of a corotation of the quadrupole mode in parts of the star with a revival of its amplitude. The gravitational wave emission of inertial modes in the late post-merger phase is concentrated in a narrow frequency region and is potentially detectable by the planned third-generation detectors. This allows for the possibility of probing not only the cold part of the equation of state, but also its dependence on finite temperature. In view of these results, it will be important to investigate the impact of various type of viscosities on the potential excitation of inertial modes in binary neutron star merger remnants.PACS numbers: 04.25.D-, 04.40. Dg, 95.30.Lz, 97.60.Jd

show abstract

Spectral analysis of gravitational waves from binary neutron star merger remnants

Cited by 44 publications

References 93 publications

Testing merging of dark exotic stars from gravitational waves in the multi-messenger approach

Testing merging of dark exotic stars from gravitational waves in the multi-messenger approach

Observing the post-merger signal of GW170817-like events with improved gravitational-wave detectors

Numerical-relativity simulations of long-lived remnants of binary neutron star mergers

Contact Info

Product

Resources

About