What Constraints on the Neutron Star Maximum Mass Can One Pose from GW170817 Observations?

Ai, Shunke; Zhang, Bing

doi:10.3847/1538-4357/ab80bd

Cited by 68 publications

(59 citation statements)

References 78 publications

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“…Energetic arguments suggest that the remnant star formed after the merger was initially a hypermassive neutron star which eventually collapsed into a black hole [284], though counterarguments also exist [285][286][287]. A number of studies have used this and different assumptions about the post-merger evolution of the system to suggest an upper limit on the maximum mass of stable, nonrotating neutron stars of 2.3M [201,284,[287][288][289][290][291][292]. Using a similar interpretation, a relation between the radius, the maximum neutron star mass, and the threshold mass for prompt collapse of the merger remnant [293] suggests R 1.6 10.6km [220].…”

Section: Multimessenger Constraintsmentioning

confidence: 99%

Neutron-star tidal deformability and equation-of-state constraints

2020

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Despite their long history and astrophysical importance, some of the key properties of neutron stars are still uncertain. The extreme conditions encountered in their interiors, involving matter of uncertain composition at extreme density and isospin asymmetry, uniquely determine the stars' macroscopic properties within General Relativity. Astrophysical constraints on those macroscopic properties, such as neutron star masses and radii, have long been used to understand the microscopic properties of the matter that forms them. In this article we discuss another astrophysically observable macroscopic property of neutron stars that can be used to study their interiors: their tidal deformation. Neutron stars, much like any other extended object with structure, are tidally deformed when under the influence of an external tidal field. In the context of coalescences of neutron stars observed through their gravitational wave emission, this deformation, quantified through a parameter termed the tidal deformability, can be measured. We discuss the role of the tidal deformability in observations of coalescing neutron stars with gravitational waves and how it can be used to probe the internal structure of Nature's most compact matter objects. Perhaps inevitably, a large portion of the discussion will be dictated by GW170817, the most informative confirmed detection of a binary neutron star coalescence with gravitational waves as of the time of writing.

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Section: Multimessenger Constraintsmentioning

confidence: 99%

Neutron-star tidal deformability and equation-of-state constraints

2020

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“…That information, together with gravitational-wave observations elucidating the nature of the remnant (e.g., Shibata et al 2019) and time it takes for the remnant to collapse to a black hole (Lucca & Sagunski 2020;Easter, Lasky, & Casey 2020), will be as important to our understanding of gamma-ray burst physics as the first multimessenger gravitational-wave observation GW170817/GRB170817A. The precise nature of the remnant of GW170817 is not known (e.g., Ai, Gao, & Zhang 2020), in large part due to the non-detection of post-merger gravitational waves (Abbott et al 2017f;2019c). The joint electromagnetic and gravitational-wave detection of GW170817-like events with the addition of a NEMO will enable significant further insight into gamma-ray burst physics.…”

Section: Other Sciencementioning

confidence: 99%

Neutron Star Extreme Matter Observatory: A kilohertz-band gravitational-wave detector in the global network

Ackley

Adya

Agrawal

et al. 2020

Publ. Astron. Soc. Aust.

187

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Gravitational waves from coalescing neutron stars encode information about nuclear matter at extreme densities, inaccessible by laboratory experiments. The late inspiral is influenced by the presence of tides, which depend on the neutron star equation of state. Neutron star mergers are expected to often produce rapidly rotating remnant neutron stars that emit gravitational waves. These will provide clues to the extremely hot post-merger environment. This signature of nuclear matter in gravitational waves contains most information in the 2–4 kHz frequency band, which is outside of the most sensitive band of current detectors. We present the design concept and science case for a Neutron Star Extreme Matter Observatory (NEMO): a gravitational-wave interferometer optimised to study nuclear physics with merging neutron stars. The concept uses high-circulating laser power, quantum squeezing, and a detector topology specifically designed to achieve the high-frequency sensitivity necessary to probe nuclear matter using gravitational waves. Above 1 kHz, the proposed strain sensitivity is comparable to full third-generation detectors at a fraction of the cost. Such sensitivity changes expected event rates for detection of post-merger remnants from approximately one per few decades with two A+ detectors to a few per year and potentially allow for the first gravitational-wave observations of supernovae, isolated neutron stars, and other exotica.

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“…The lack of detection of such features suggests that the merger product of GW170817 may not be an SMNS. However, we note that the data for GW170817 suggest an M TOV ≤ 2.17 M if the newly formed remnant has been a short-lived HMNS (Margalit & Metzger 2017;Rezzolla et al 2018;Ai et al 2020), while in order to account for X-ray plateaus, M TOV would need to be relatively high, M TOV ∼ 2.3 M (Fan et al 2013a;Gao et al 2016). This difference may be reduced if the remnant formed in GW170817 had quickly or effectively lost its angular momentum through the GW radiation, for which M TOV ≤ 2.3 M is allowed for the general cases (Shibata et al 2019;Shao et al 2020).…”

Section: Conclusion and Discussionmentioning

confidence: 77%

“…Fan et al (2020) showed that the properties of the binary NSs involved in GW170817 are in favor of strong post-merger GW radiation. In addition, as discussed in Ai et al (2020), the merger remnant of GW170817 may also have been a long-lived massive NS or even a stable NS. This question needs further investigation.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Protomagnetar research through an analysis of the X-ray plateau in the multi-messengar era

Ren

Wei

Zhu

et al. 2020

A&A

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The joint detection of the gravitational wave signal and the electromagnetic emission from a binary neutron star merger can place unprecedented constraint on the equation of state of supranuclear matter. Although a variety of electromagnetic counterparts have been observed for GW170817, including a short gamma-ray burst, kilonova, and the afterglow emission, the nature of the merger remnant is still unclear, however. The X-ray plateau is another important characteristics of short gamma-ray bursts. This plateau is probably due to the energy injection from a rapidly rotating magnetar. We investigate what we can learn from the detection of a gravitational wave along with the X-ray plateau. In principle, we can estimate the mass of the merger remnant if the X-ray plateau is caused by the central magnetar. We selected eight equations of state that all satisfy the constraint given by the gravitational wave observation, and then calculated the mass of the merger remnants of four short gamma-ray bursts with a well-measured X-ray plateau. If, on the other hand, the mass of the merger remnant can be obtained by gravitational wave information, then by comparing the masses derived by these two different methods can further constrain the equation of state. We discuss the possibility that the merger product is a quark star. In addition, we estimate the possible mass range for the recently discovered X-ray transient CDF-S XT2 that probably originated from a binary neutron star merger. Finally, under the assumption that the post-merger remnant of GW170817 was a supramassive neutron star, we estimated the allowed parameter space of the supramassive neutron star and find that in this case, the magnetic dipole radiation energy is so high that it may have some effects on the short gamma-ray burst and kilonova emission. The lack of detection of these effects suggests that the merger product of GW170817 may not be a supermassive neutron star.

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What Constraints on the Neutron Star Maximum Mass Can One Pose from GW170817 Observations?

Cited by 68 publications

References 78 publications

Neutron-star tidal deformability and equation-of-state constraints

Neutron-star tidal deformability and equation-of-state constraints

Neutron Star Extreme Matter Observatory: A kilohertz-band gravitational-wave detector in the global network

Protomagnetar research through an analysis of the X-ray plateau in the multi-messengar era

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