Probing the Equation of State of Nuclear Matter via Neutron Star Asteroseismology

Sotani, Hajime; Nakazato, Ken’ichiro; Iida, Kei; Oyamatsu, Kazuhiro

doi:10.1103/physrevlett.108.201101

Cited by 131 publications

(146 citation statements)

References 38 publications

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“…Li et al (2008);Tsang et al (2012)) give a conservative range L = 20 − 120 MeV, although some more recent results on the nuclear experimental side (Lattimer & Lim 2013), as well as tentative constraints from neutron star observation (Newton & Li 2009;Gearheart et al 2011;Wen et al 2012;Steiner & Gandolfi 2012) and from ab-initio pure neutron matter calculations (Gezerlis & Carlson 2010;Hebeler & Schwenk 2010;Gandolfi et al 2012) tend to favor the lower half of that range (although, for a counter-example, see e.g. Sotani et al (2012)). Particularly, combining inferred values of L from several nuclear experimental probes suggests a range L ≈ 30 − 60 MeV (Hebeler et al 2013;Lattimer & Steiner 2014).…”

Section: Introductionmentioning

confidence: 99%

Efficacy of crustal superfluid neutrons in pulsar glitch models

Hooker¹,

Newton²,

Li³

2015

Monthly Notices of the Royal Astronomical Society

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In order to assess the ability of purely crust-driven glitch models to match the observed glitch activity in the Vela pulsar, we conduct a systematic analysis of the dependence of the fractional moment of inertia of the inner crustal neutrons on the stiffness of the nuclear symmetry energy at saturation density L. We take into account both crustal entrainment and the fact that only a fraction Y g of the core neutrons may couple to the crust on the glitch-rise timescale. We use a set of consistently-generated crust and core compositions and equations-of-state which are fit to results of lowdensity pure neutron matter calculations. When entrainment is included at the level suggested by recent microscopic calculations and the core is fully coupled to the crust, the model is only able to account for the Vela glitch activity for a 1.4M star if the equation of state is particularly stiff L > 100 MeV. However, an uncertainty of about 10% in the crust-core transition density and pressure allows for the Vela glitch activity to be marginally accounted for in the range L ≈ 30 − 60MeV consistent with a range of experimental results. Alternatively, only a small amount of core neutrons need be involved. If less than 50% of the core neutrons are coupled to the crust during the glitch, we can also account for the Vela glitch activity using crustal neutrons alone for EOSs consistent with the inferred range of L. We also explore the possibility of Vela being a high-mass neutron star, and of crustal entrainment being reduced or enhanced relative to its currently predicted values.

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Section: Introductionmentioning

confidence: 99%

Efficacy of crustal superfluid neutrons in pulsar glitch models

Hooker¹,

Newton²,

Li³

2015

Monthly Notices of the Royal Astronomical Society

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“…[30,31]. In fact, the elasticity in such region is expected to be lower than that in the droplet region [61] …”

Section: Neutron Star Modelsmentioning

confidence: 99%

“…As in Refs. [29,31,66], we impose zero-traction conditions at the both boundaries of the HQ mixed phase. In practice, the matter element outside the HQ mixed phase can not affect the motion of torsional oscillations, which is the same situation in the crust torsional oscillations at the boundary between the crust and core regions.…”

Section: Torsional Oscillationsmentioning

confidence: 99%

“…In order to explain these QPO frequencies theoretically, a lot of numerical attempts have been done not only by the shear oscillations in the crust of neutron stars but also by the magnetic oscillations [17,18,19,20,21,22,23,24,25,26,27]. In addition, ascribing the observed QPOs to shear oscillations in the crust of neutron stars, the possibilities are also pointed out to reveal the properties of inhomogeneous nuclear matter in the crust [28,29,30,31,32].…”

Section: Introductionmentioning

confidence: 99%

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Shear oscillations in the hadron–quark mixed phase

2013

Self Cite

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Inside neutron stars, the hadron-quark mixed phase is expected during the first order phase transition from the hadron phase to the quark phase. The geometrical structure of the mixed phase strongly depends on the surface tension at the hadron-quark interface. We evaluate the shear modulus which is one of the specific properties of the hadron-quark mixed phase. As an application, we study shear oscillations due to the hadron-quark mixed phase in neutron stars. We find that the frequencies of shear oscillations depend strongly on the surface tension; with a fixed stellar mass, the fundamental frequencies are almost proportional to the surface tension. Thus, one can estimate the value of surface tension via the observation of stellar oscillations with the help of the information on the stellar mass.

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“…These structures resemble images of various kinds of pasta; gnocchi, spaghetti, lasagna, bucatini or antispaghetti, and Swiss cheese. The nuclear pasta phases consist of periodic Coulomb lattices whose static and dynamical properties could influence the oscillations of neutron star crusts, the cooling process, and the glitch phenomena [4][5][6].…”

Section: Introductionmentioning

confidence: 99%

Density Functional Calculations for the Neutron Star Matter at Subnormal Density

Kashiwaba¹,

Nakatsukasa²

2017

Proceedings of the 14th International Symposium on Nuclei in the Cosmos (NIC2016)

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The pasta phases of nuclear matter, whose existence is suggested at low density, may influence observable properties of neutron stars. In order to investigate properties of the neutron star matter, we calculate self-consistent solutions for the ground states of slab-like phase using the microscopic density functional theory with Bloch wave functions. The calculations are performed at each point of fixed average density and proton fraction (ρ, Y p ), varying the lattice constant of the unit cell. For small Y p values, the dripped neutrons emerge in the ground state, while the protons constitute the slab (crystallized) structure. The shell effect of protons affects the thickness of the slab nuclei.

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Probing the Equation of State of Nuclear Matter via Neutron Star Asteroseismology

Cited by 131 publications

References 38 publications

Efficacy of crustal superfluid neutrons in pulsar glitch models

Efficacy of crustal superfluid neutrons in pulsar glitch models

Shear oscillations in the hadron–quark mixed phase

Density Functional Calculations for the Neutron Star Matter at Subnormal Density

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