$R$-mode Stability of GW190814's Secondary Component as a Supermassive and Superfast Pulsar

Zhou, Xia; Li, Ang; Li, Bao-An

doi:10.48550/arxiv.2011.11934

Cited by 4 publications

(4 citation statements)

References 67 publications

(113 reference statements)

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“…We now turn to examine the nature and properties of several merger events based on our results of the hybrid star maximum mass. Even though there is a wide distribution of M TOV from our results, the peak value ∼ 2.4 M suggests that the possibility that the secondary component of GW190814 with a mass M ∼ 2.6 M (Abbott et al 2020b) could be a spinning supermassive NS is not ruled out, even if one takes into account the limitation of the intrinsic r-mode instability (Zhou et al 2020). Within this scenario, however, the supramassive NS needs to carry a low dipolar magnetic field so that it has not been spun down yet at the time of merger.…”

Section: Hybrid Star Eos and The Maximum Masscontrasting

confidence: 53%

Constraints on the maximum mass of neutron stars with a quark core from GW170817 and NICER PSR J0030+0451 data

Li,

Miao,

Han

et al. 2021

Preprint

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We perform a Bayesian analysis of the maximum mass M TOV of neutron stars with a quark core, incorporating the observational data from tidal deformability of the GW170817 binary neutron star merger as detected by LIGO/Virgo and the mass and radius of PSR J0030+0451 as detected by NICER. The analysis is performed under the assumption that the hadron-quark phase transition is of first order, where the low-density hadronic matter described in a unified manner by the soft QMF or the stiff DD2 equation of state (EOS) transforms into a high-density phase of quark matter modeled by the generic "Constant-sound-speed" (CSS) parameterization. The mass distribution measured for the 2.14 M pulsar, MSP J0740+6620, is used as the lower limit on M TOV . We find the most probable values of the hybrid star maximum mass are M TOV = 2.36 +0.49 −0.26 M (2.39 +0.47 −0.28 M ) for QMF (DD2), with an absolute upper bound around 2.85 M , to the 90% posterior credible level. Such results appear robust with respect to the uncertainties in the hadronic EOS. We also discuss astrophysical implications of this result, especially on the post-merger product of GW170817, short gamma-ray bursts, and other likely binary neutron star mergers.

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Section: Hybrid Star Eos and The Maximum Masscontrasting

confidence: 53%

Constraints on the maximum mass of neutron stars with a quark core from GW170817 and NICER PSR J0030+0451 data

Li,

Miao,

Han

et al. 2021

Preprint

Self Cite

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“…Among them the majority are confirmed to be BH-BH systems and several are suspected to be BH-NS systems, e.g. GW190814 (Huang et al 2020;Zhou et al 2020) and GW190425 (Han et al 2020a;Kyutoku et al 2020). As expected, searches of the electromagnetic counterparts for BH-BH mergers have yielded negative results (e.g., Copperwheat et al 2016;Smartt et al 2016;Racusin et al 2017).…”

Section: Introductionmentioning

confidence: 94%

Population Synthesis of Black Hole Binaries with Normal-star Companions. I. Detached Systems

Shao

2019

ApJ

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Optical observations of normal-stars in binary systems with massive unseen objects have been proposed to search for candidate black holes (BHs) and provide a direct measurement of their dynamical masses. In this paper, we have performed binary population synthesis calculations to simulate the potential population of detached binaries containing BHs and normal-star companions in the Galaxy. We focus on the influence of the BH progenitors. In the traditional model, BHs in binaries evolve from stars more massive than ∼ 25M . However, it is difficult for this model to produce BH low-mass X-ray binaries. Recent investigations on massive star evolution suggest that the BH progenitors may have masses as low as ∼ 15M . Based on this model, we provide the expected distributions of various parameters for detached BH binaries with normal-star companions, including the component masses, the orbital parameters of the binary systems, the radial velocity semi-amplitudes, and the astrometric signatures of the optical companions. Our calculations show that there are more than thousands of such detached binaries in the Galaxy, and hundreds of them are potentially observable systems with luminous companions brighter than 20 mag. In addition, detached BH binaries are dominated by those with main-sequence companions and only a few percent of them are expected to have giant companions.

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“…The condition (18) leads to the critical angular velocity Ω c which is given by (for a detailed analysis see Refs. [17,39,40])…”

Section: B Critical Angular Velocity For R-modesmentioning

confidence: 99%

Crust-core interface and bulk neutron star properties

Margaritis

Koliogiannis²,

Kanakis-Pegios³

et al. 2021

Phys. Rev. C

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The nuclear symmetry energy plays an important role in the description of the properties of finite nuclei as well as neutron stars. Especially, for low values of baryon density, the accurate description of the crust-core interface strongly depends on the symmetry energy. Usually, the well known parabolic approximation is employed for the definition of the symmetry energy without avoiding some drawbacks. In the present work, a class of nuclear models, suitable for the description of the inner and outer core of neutron stars, is applied in studying the effect of higher orders of the expansion of the energy on the location of the crust-core transition. The thermodynamical and dynamical methods are used for the determination of the transition density nt and pressure Pt. The corresponding energy density functional is applied for the study of some relevant properties of both non-rotating and slow rotating neutron stars. We found that the larger the value of the slope parameter L, the slower the convergence of the expansion. In addition, a universal relation is presented between nt and L, by employing the full expression and dynamical approach. The crustal moment of inertia is very sensitive on the location of the transition while the effects are moderated concerning the critical angular velocity of the r-mode instability and minimum mass configuration. The effect on the tidal deformability is less but not negligible. In any case, the use of the parabolic approximation leads to the overestimation of nt and Pt and consequently, on inaccurate predictions.

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$R$-mode Stability of GW190814's Secondary Component as a Supermassive and Superfast Pulsar

Cited by 4 publications

References 67 publications

Constraints on the maximum mass of neutron stars with a quark core from GW170817 and NICER PSR J0030+0451 data

Constraints on the maximum mass of neutron stars with a quark core from GW170817 and NICER PSR J0030+0451 data

Population Synthesis of Black Hole Binaries with Normal-star Companions. I. Detached Systems

Crust-core interface and bulk neutron star properties

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