Isovector Effects in Neutron Stars, Radii, and the GW170817 Constraint

Motta, Theo F.; Kalaitzis, A. M.; Antić, S.; Guichon, P.A.M.; Stone, J. R.; Thomas, A. W.

doi:10.3847/1538-4357/ab218e

Cited by 44 publications

(36 citation statements)

References 58 publications

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“…The larger values of the radius required to fit the NICER points seem to be somewhat difficult to reconcile with the Λ values required by the GW170817 estimates. Other calculations performed with quark matter stars [44,[52][53][54][55] or hybrid stars [19,[56][57][58][59][60] arrive at similar results. On the other hand, calculations of the tidal deformability with purely hadronic equations of states [61][62][63] seem to reproduce the experimental data more easily.…”

Section: Tov Equation Mass and Radiussupporting

confidence: 62%

Tidal Deformability of Quark Stars with Repulsive Interactions

Albino,

Fariello,

Navarra

2021

Preprint

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In an early work, we applied a QCD-based EOS to the study of the stellar structure of self-bound strange stars, obtaining sequences with maximum masses larger than two solar masses and radii ranging from 8 to 12 Km. In this work, we update the previous calculations and compare them with the most recent data, including the very recent determination of the mass and radius of the massive pulsar PSR J0740+6620 performed by the NICER and XMM-Newton Collaborations. Our equation of state is similar to the MIT bag model one, but it includes repulsive interactions, which turn out to be essential to reproduce the accumulated experimental information. We find that our EOS is still compatible with all astrophysical observations but the parameter window is now narrower.

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Section: Tov Equation Mass and Radiussupporting

confidence: 62%

Tidal Deformability of Quark Stars with Repulsive Interactions

Albino,

Fariello,

Navarra

2021

Preprint

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“…The NS MOI has been theoretically calculated using a wide range of EOS models (e.g., Yuan & Zhang 1999;Morrison et al 2004;Lattimer & Schutz 2005;Bejger et al 2005;Rikovska Stone et al 2007;Klähn et al 2007;Read et al 2009;Urbanec et al 2013;Motta et al 2019;Sun et al 2019;Wei et al 2019;Lourenço et al 2020;Margaritis et al 2020). Several studies have been performed using EOS models, including those incorporating strangeness phase transitions (e.g., Klähn et al 2007;Bandyopadhyay et al 2018;Sen & Jha 2019;Ribes et al 2019;Fortin et al 2020;Raduta et al 2020).…”

Section: Introductionmentioning

confidence: 99%

On the moment of inertia of PSR J0737-3039 A from LIGO/Virgo and NICER

Miao¹,

Li²

2021

Preprint

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We extend our previous study (Li et al. 2021) on neutron stars with a quark core to predict the moment of inertia of pulsar A in the double pulsar binary J0737-3039, assuming there is a phase transition in the pulsar inner core from the soft QMF or the stiff DD2 hadronic equation of state (EOS) to a high-density phase of quark matter modelled by the generic "constant-sound-speed" (CSS) parameterization. We perform a Bayesian analysis of the moment of inertia by incorporating observational data for the tidal deformability of the GW170817 and GW190425 binary neutron star mergers, as detected by LIGO/Virgo, and the mass and radius of PSR J0030+0451 and MSP J0740+6620, as detected by the Neutron Star Interior Composition Explorer. We find that the most probable values of the moment of inertia of PSR J0737-3039 A are 1.27 +0.18 −0.14 × 10 45 g cm 2 for QMF+CSS and similarly 1.29 +0.26 −0.15 × 10 45 g cm 2 for DD2+CSS at 90% credible interval. We also demonstrate how a moment of inertia measurement would improve our knowledge of the EOS and the mass-radius relation for hybrid stars and discuss whether a quark deconfinement phase transition is supported by the available data and forthcoming data that could be consistent with this hypothesis.

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“…Another solution, assuming the presence of hyperons in the stellar core, is to adjust the parameters of the microphysical model including hyperons (e.g. the coupling strength among baryons and mesons) to raise the maximum mass to ≈ 2 𝑀 (Rikovska Stone et al 2007;Gusakov et al 2014;Fortin et al 2015;Motta et al 2019). Some neutron stars with parameters adjusted in this way are predicted to cool rapidly, due to nucleonic and hyperon direct Urca emission (Raduta et al 2018(Raduta et al , 2019.…”

Section: Introductionmentioning

confidence: 99%

Fast cooling and internal heating in hyperon stars

Anzuini,

Melatos,

Dehman

et al. 2021

Preprint

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Neutron star models with maximum mass close to 2 𝑀 reach high central densities, which may activate nucleonic and hyperon direct Urca neutrino emission. To alleviate the tension between fast theoretical cooling rates and thermal luminosity observations of moderately magnetized, isolated thermally-emitting stars (with 𝐿 𝛾 10 31 erg s −1 at 𝑡 10 5.3 yr), some internal heating source is required. The power supplied by the internal heater is estimated for both a phenomenological source in the inner crust and Joule heating due to magnetic field decay, assuming different superfluidity models and compositions of the outer stellar envelope. It is found that a thermal power of 𝑊 (𝑡) ≈ 10 34 erg s −1 allows neutron star models to match observations of moderately magnetized, isolated stars with ages 𝑡 10 5.3 yr. The requisite 𝑊 (𝑡) can be supplied by Joule heating due to crust-confined initial magnetic configurations with (i) mixed poloidal-toroidal fields, with surface strength 𝐵 dip = 10 13 G at the pole of the dipolar poloidal component and ∼ 90 per cent of the magnetic energy stored in the toroidal component; and (ii) poloidal-only configurations with 𝐵 dip = 10 14 G.

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Isovector Effects in Neutron Stars, Radii, and the GW170817 Constraint

Cited by 44 publications

References 58 publications

Tidal Deformability of Quark Stars with Repulsive Interactions

Tidal Deformability of Quark Stars with Repulsive Interactions

On the moment of inertia of PSR J0737-3039 A from LIGO/Virgo and NICER

Fast cooling and internal heating in hyperon stars

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