Finding Structure in the Speed of Sound of Supranuclear Matter from Binary Love Relations

Tan, Hung; Dexheimer, V.; Noronha-Hostler, Jacquelyn; Yunes, Nicolás

doi:10.1103/physrevlett.128.161101

Cited by 37 publications

(18 citation statements)

References 97 publications

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“…We illustrate this behavior in Figure 3, where we show the l l a s ¯¯correlation for the EoS and binary parameters used in this work. We can clearly see that, in line with Tan et al (2021), there is a range of slopes separating EoSs with backwards-and forwards-bending mass-radius curves. Because the binary-Love relation also depends on the neutron star radius and mass-radius slope, but with a different dependence than our two-parameter, quasi-universal relations for f 2 , combined detections of inspiral and postmerger should enable a reconstruction of the linearized mass-radius curve.…”

Section: Discussionsupporting

confidence: 76%

“…nations of the mass-normalized tidal deformabilities l 1,2 ¯of the inspiraling neutron stars in an EoS-insensitive way (Yagi & Yunes 2016). In a recent work, Tan et al (2021) showed that these relations, previously thought to be fully universal, also receive an effective correction that is linearly proportional to the slope of the mass-radius curve. We illustrate this behavior in Figure 3, where we show the l l a s ¯¯correlation for the EoS and binary parameters used in this work.…”

Section: Discussionmentioning

confidence: 98%

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Characterizing the Breakdown of Quasi-universality in Postmerger Gravitational Waves from Binary Neutron Star Mergers

Raithel

Most

2022

ApJL

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The postmerger gravitational wave (GW) emission from a binary neutron star merger is expected to provide exciting new constraints on the dense-matter equation of state (EoS). Such constraints rely, by and large, on the existence of quasi-universal relations, which relate the peak frequencies of the postmerger GW spectrum to properties of the neutron star structure in a model-independent way. In this work, we report on violations of existing quasi-universal relations between the peak spectral frequency, f 2, and the stellar radius, for EoS models with backwards-bending slopes in their mass–radius relations (such that the radius increases at high masses). The violations are extreme, with variations in f 2 of up to ∼600 Hz between EoSs that predict the same radius for a 1.4 M ⊙ neutron star but that have significantly different radii at higher masses. Quasi-universality can be restored by adding in a second parameter to the fitting formulae that depends on the slope of the mass–radius curve. We further find strong evidence that quasi-universality is better maintained for the radii of very massive stars (with masses 2 M ⊙). Both statements imply that f 2 is mainly sensitive to the high-density EoS. Combined with observations of the binary neutron star inspiral, these generalized quasi-universal relations can be used to simultaneously infer the characteristic radius and slope of the neutron star mass–radius relation.

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Section: Discussionsupporting

confidence: 76%

Section: Discussionmentioning

confidence: 98%

Characterizing the Breakdown of Quasi-universality in Postmerger Gravitational Waves from Binary Neutron Star Mergers

Raithel

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2022

ApJL

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“…The symmetric mass ratio and chirp mass may overlap with that of SM NS binaries. Tidal deformabilities would break universal relations and may appear similar to twin stars [86]. The remnant will be a black hole in most scenarios, unless the dark matter core is extremely small.…”

Section: Observational Prospectsmentioning

confidence: 99%

Dark Matter or Regular Matter in Neutron Stars? How to tell the difference from the coalescence of compact objects

Hippert¹,

Emily²,

Tan³

et al. 2022

Preprint

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The mirror twin Higgs model is a candidate for (strongly-interacting) complex dark matter, which mirrors SM interactions with heavier quark masses. A consequence of this model are mirror neutron stars -exotic stars made entirely of mirror matter, which are significantly smaller than neutron stars and electromagnetically dark. This makes mergers of two mirror neutron stars detectable and distinguishable in gravitational wave observations, but can we observationally distinguish between regular neutron stars and those that may contain some mirror matter? This is the question we study in this paper, focusing on two possible realizations of mirror matter coupled to standard model matter within a compact object: (i) mirror matter captured by a neutron star and (ii) mirror neutron star-neutron star coalescences. Regarding (i), we find that (non-rotating) mirror-matter-admixed neutron stars no longer have a single mass-radius sequence, but rather exist in a two-dimensional mass-radius plane. Regarding (ii), we find that binary systems with mirror neutron stars would span a much wider range of chirp masses and completely different binary Love relations, allowing merger remnants to be very light black holes. The implications of this are that gravitational wave observations with advanced LIGO and Virgo, and X-ray observations with NICER, could detect or constrain the existence of mirror matter through searches with wider model and parameter priors.

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“…At 500 MeV fm −3 , the speed of sound plateaus if only astrophysical data are considered, while it decreases significantly if pQCD (at larger X values) is added. Such non-monotonous behaviour of the sound speed is expected to be indicative of the appearance of exotic, non-nucleonic degrees of freedom [42,52,53], such as for instance quarkyonic matter as suggested in Ref. [54].…”

mentioning

confidence: 92%

Perturbative QCD and the Neutron Star Equation of State

Somasundaram¹,

Tews²,

Margueron³

2022

Preprint

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We construct a physics-agnostic approach based on the sound speed model, which connects both low-density information from nuclear theory and high-density constraints from perturbative QCD (pQCD). Using this approach, we study the impact of pQCD constraints on neutron star (NS) equations of state (EoS) that have been constrained by astrophysical observations. We find that the pQCD constraints affect the EoS mainly beyond the densities realized in NS. Furthermore, we observe an interesting interplay between pQCD and astrophysical constraints, with pQCD preferring softer EoS for the heaviest NS while recent NICER observations suggest the EoS to be stiffer. We explore the sensitivity of our findings to pQCD uncertainties and we study the constraining power of pQCD if future observations of heavy NS were to suggest radii larger than 13 km for heavy stars.

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Finding Structure in the Speed of Sound of Supranuclear Matter from Binary Love Relations

Cited by 37 publications

References 97 publications

Characterizing the Breakdown of Quasi-universality in Postmerger Gravitational Waves from Binary Neutron Star Mergers

Characterizing the Breakdown of Quasi-universality in Postmerger Gravitational Waves from Binary Neutron Star Mergers

Dark Matter or Regular Matter in Neutron Stars? How to tell the difference from the coalescence of compact objects

Perturbative QCD and the Neutron Star Equation of State

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