Multimessenger parameter estimation of GW170817

Radice, David; Dai, Liang

doi:10.1140/epja/i2019-12716-4

Cited by 222 publications

(218 citation statements)

References 96 publications

(113 reference statements)

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“…The upper limitΛ = 720 was set by the analysis of GW170817 event (more precisely, this is the lowest value for this limit at 90% confidence [41]). The lower limitΛ ≈ 250 was deduced from the analysis of the electromagnetic counterpart of GW170817, e.g., AT2017gfo [44][45][46][47]. This lower limit onΛ indicates approximately that the radius for a canonical neutron star must be larger than ∼ 10.5 km [46,47] It is expected that more neutron star binary mergers will be observed within the coming years.…”

Section: Comparison With the Data From Gw170817 Eventmentioning

confidence: 96%

“…The lower limitΛ ≈ 250 was deduced from the analysis of the electromagnetic counterpart of GW170817, e.g., AT2017gfo [44][45][46][47]. This lower limit onΛ indicates approximately that the radius for a canonical neutron star must be larger than ∼ 10.5 km [46,47] It is expected that more neutron star binary mergers will be observed within the coming years. Now, imagine comparing two such events in which the observed values of Λ 1 are close but the Λ 2 values are different.…”

Section: Comparison With the Data From Gw170817 Eventmentioning

confidence: 96%

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Relativistic hybrid stars with sequential first-order phase transitions and heavy-baryon envelopes

Sedrakian

Alford

2020

Phys. Rev. D

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We compute the mass, radius and tidal deformability of stars containing phase transitions from hadronic to quark phase(s). These quantities are computed for three types of hadronic envelopes: purely nuclear, hyperonic, and ∆-resonance-hyperon admixed matter. We consider either a single first-order phase transition to a quark phase with a maximally stiff equation of state (EoS) or two sequential first-order phase transitions mimicking a transition from hadronic (H) to a quark matter phase followed by a second phase transition to another quark phase. Such a construct emulates the results of the computations of the EoS which include 2SC and CFL color superconducting phases at low and high density. We explore the parameter space which produces low mass twin and triplet configurations where equal mass stars have substantially different radii and tidal deformabilities. We demonstrate that while for purely hadronic stiff EoS the obtained maximum mass is inconsistent with the upper limit on this quantity placed by GW170817, the inclusion of the hyperonic and ∆-resonance degrees of freedom, as well as the deconfinement phase transition at sufficiently low density, produce configuration of stars consistent with this limit. The obtained hybrid star configurations are in the mass range relevant for the interpretation of the GW170817 event. We compare our results for the tidal deformability with the limits inferred from GW170817 showing that the onset of non-nucleonic phases, such as ∆-resonance-hyperon admixed phase or/and the quark phase(s) is favored by this data if the nuclear EoS is stiff. Also, we show that low-mass twins and especially triplets proliferate the number of combinations of possible types of star that can undergo a merger event, the maximal number being six in the case of triplets. The prospects for uncovering the first-order phase transition(s) to and in quark matter via measurements of tidal deformabilities in merger events are discussed.

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Section: Comparison With the Data From Gw170817 Eventmentioning

confidence: 96%

Section: Comparison With the Data From Gw170817 Eventmentioning

confidence: 96%

Relativistic hybrid stars with sequential first-order phase transitions and heavy-baryon envelopes

Sedrakian

Alford

2020

Phys. Rev. D

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“…In this work, we use an equation of state describing the neutron star crust with a nuclear interaction Hamiltonian; in particular, we use analytical representations of P (ρ) known as the Brussels-Montreal equations of state [55,122,123]. Among its versions, we have used "BsK21" as our standard equation of state -some other versions are disfavored by observations [124,125]. Later, we also employ a few other "BsK" models to show that our results are robust when this choice is varied.…”

Section: Overall Structurementioning

confidence: 99%

Warming nuclear pasta with dark matter: kinetic and annihilation heating of neutron star crusts

Acevedo

Bramante

Leane

et al. 2020

J. Cosmol. Astropart. Phys.

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Neutron stars serve as excellent next-generation thermal detectors of dark matter, heated by the scattering and annihilation of dark matter accelerated to relativistic speeds in their deep gravitational wells. However, the dynamics of neutron star cores are uncertain, making it difficult at present to unequivocally compute dark matter scattering in this region. On the other hand, the physics of an outer layer of the neutron star, the crust, is more robustly understood. We show that dark matter scattering solely with the low-density crust still kinetically heats neutron stars to infrared temperatures detectable by forthcoming telescopes. We find that for both spin-independent and spin-dependent scattering on nucleons, the crust-only cross section sensitivity is 10 −43 − 10 −41 cm 2 for dark matter masses of 100 MeV − 1 PeV, with the best sensitivity arising from dark matter scattering with a crust constituent called nuclear pasta (including gnocchi, spaghetti, and lasagna phases). For dark matter masses from 10 eV to 1 MeV, the sensitivity is 10 −39 − 10 −34 cm 2 , arising from exciting collective phonon modes in a neutron superfluid in the inner crust. Furthermore, for any s-wave or p-wave annihilating dark matter, we show that dark matter will efficiently annihilate by thermalizing just with the neutron star crust, regardless of whether the dark matter ever scatters with the neutron star core. This implies efficient annihilation in neutron stars for any electroweakly interacting dark matter with inelastic mass splittings of up to 200 MeV, including Higgsinos. We conclude that neutron star crusts play a key role in dark matter scattering and annihilation in neutron stars. *

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“…Changes in the orbital phasing due to the components' mutual tidal interaction leave a detectable imprint in the GW signal [2][3][4][5][6], and several studies have exploited this fact to infer the tidal deformabilities of the compact objects involved in the coalescence [7][8][9][10]. Additionally, the observations of counterparts across the electromagnetic spectrum provide complementary constraints on tidal effects [11][12][13][14]. As the advanced LIGO [15] and Virgo [16] detectors continue to operate, further observations of NS coalescences (e.g.…”

Section: Introductionmentioning

confidence: 99%

Nonparametric inference of neutron star composition, equation of state, and maximum mass with GW170817

2020

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The detection of GW170817 in gravitational waves provides unprecedented constraints on the equation of state (EOS) of the ultra-dense matter within the cores of neutron stars (NSs). We extend the nonparametric analysis first introduced in Landry & Essick (2019), and confirm that GW170817 favors soft EOSs. We infer macroscopic observables for a canonical 1.4 M NS, including the tidal deformability Λ1.4 = 211 +312 −137 (491 +216 −181 ) and radius R1.4 = 10.86 +2.04 −1.42 (12.51 +1.00 −0.88 ) km, as well as the maximum mass for nonrotating NSs, Mmax = 2.064 +0.260 −0.134 (2.017 +0.238 −0.087 ) M , with nonparametric priors loosely (tightly) constrained to resemble candidate EOSs from the literature. Furthermore, we find weak evidence that GW170817 involved at least one NS based on gravitational-wave data alone (B NS BBH = 3.3 ± 1.4), consistent with the observation of electromagnetic counterparts. We also investigate GW170817's implications for the maximum spin frequency of millisecond pulsars, and find that the fastest known pulsar is spinning at more than 50% of its breakup frequency at 90% confidence. We additionally find modest evidence in favor of quark matter within NSs, and GW170817 favors the presence of at least one disconnected hybrid star branch in the mass-radius relation over a single stable branch by a factor of 2. Assuming there are multiple stable branches, we find a suggestive posterior preference for a sharp softening around nuclear density followed by stiffening around twice nuclear density, consistent with a strong first-order phase transition. While the statistical evidence in favor of new physics within NS cores remains tenuous with GW170817 alone, these tantalizing hints reemphasize the promise of gravitational waves for constraining the supranuclear EOS.

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Multimessenger parameter estimation of GW170817

Cited by 222 publications

References 96 publications

Relativistic hybrid stars with sequential first-order phase transitions and heavy-baryon envelopes

Relativistic hybrid stars with sequential first-order phase transitions and heavy-baryon envelopes

Warming nuclear pasta with dark matter: kinetic and annihilation heating of neutron star crusts

Nonparametric inference of neutron star composition, equation of state, and maximum mass with GW170817

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