Shear modulus of the hadron-quark mixed phase

Johnson-McDaniel, Nathan K.; Owen, B. J.

doi:10.1103/physrevd.86.063006

Cited by 11 publications

(5 citation statements)

References 99 publications

(241 reference statements)

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“…It depends on the properties of the mixed phase: the shear modulus is brought about by the pasta structures [21] while the amorphous state is not.…”

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confidence: 99%

Amorphous state in the mixed phase of hadron-quark phase transition in protoneutron stars

2012

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We study the hadron-quark mixed phase in protoneutron stars, where neutrinos are trapped and lepton number becomes a conserved quantity besides the baryon number and electric charge. Considering protoneutron-star matter as a ternary system, the Gibbs conditions are applied together with the Coulomb interaction. We find that there no crystalline (''pasta'') structure appears in the regime of high leptonnumber fraction; the size of pasta becomes very large and the geometrical structure becomes mechanically unstable due to the charge screening effect. Consequently the whole system is separated into two bulk regions like an amorphous state, where the surface effect is safely neglected. There, the local charge neutrality is approximately attained, so that the equation of state is effectively reduced to the one for a binary system. Hence, we conclude that there is no possibility for the density discontinuity to appear in protoneutron-star matter, which is a specific feature in a pure system. These features are important when considering astrophysical phenomena such as supernova explosions or radiation of the gravitational wave from protoneutron stars.Recently there have been many works about the hadronquark (HQ) phase transition in compact stars [1], where signatures of the phase transition are explored during supernova explosions [2,3] in the spectrum of the gravitational wave [4] and so on. The deconfinement transition might be of the first order at finite density although uncertainties remain, e.g., the equation of state (EOS) of quark matter or deconfinement mechanism [5]. In this case, the HQ-mixed phase appears and the phase equilibrium in the mixed phase must be carefully treated by applying the Gibbs conditions [6]. A simple treatment of the mixed phase may be the bulk Gibbs calculation, where phase equilibrium of two pieces of bulk matter is considered without the electromagnetic interaction. The EOS then looks like the second-order phase transition in the sense of Ehrenfest; there appears no constant-pressure region as in the van der Waals liquid. A realistic treatment of the mixed phase takes into account the finite-size effects, the electromagnetic interaction, and the surface tension. Generally, the properties of the mixed phase strongly depend on the finite-size effects to lead to the inhomogeneous crystalline (pasta) structures [7,8]. The EOS resembles the one given by the bulk Gibbs calculation for the weak surface tension, and close to the one given by the Maxwell construction for the strong surface tension [9,10]. These differences are mainly brought about by the charge-screening effect and rearrangement of the charge distribution in the presence of the Coulomb interaction [11].Here we consider the HQ-phase transition in protoneutron stars (PNSs), where neutrinos are trapped and lepton number is conserved. Consequently there are three conserved quantities-baryon number, electric charge, and lepton number. Thus, PNS matter should be treated as a ternary system, different from the usual neutron star mat...

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“…It depends on the properties of the mixed phase: the shear modulus is brought about by the pasta structures [21] while the amorphous state is not.…”

mentioning

confidence: 99%

Amorphous state in the mixed phase of hadron-quark phase transition in protoneutron stars

2012

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“…Finally, we suggest that the domain decomposition method described here could be extended to treat certain "pasta phases" in neutron star cores, complementary to dimensional continuation techniques (Johnson-McDaniel & Owen 2012).…”

Section: Discussionmentioning

confidence: 99%

“…for longitudinal and transverse modes, respectively. In analysis of neutron star material, the effective shear modulus µ eff is typically taken to be the angle-averaged quantity proposed by Ogata & Ichimaru (1990) -see for example Baiko (2012); Johnson-McDaniel & Owen (2012).…”

Section: Elastic Constants and Zone-edge Phononsmentioning

confidence: 99%

Microphysics of Neutron Star Outer Envelopes in the Periodized, Magnetic Thomas-Fermi Model

Engstrom,

Crespi,

Owen

et al. 2014

Preprint

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Static and dynamic properties of low density outer envelopes of neutron stars are calculated within the nonlinear magnetic Thomas-Fermi model, assuming degenerate electrons. A novel domain decomposition enables proper description of lattice symmetry and may be seen as a prototype for the general class of problems involving nonlinear charge screening of periodic, quasi-low-dimensionality structures, e.g. liquid crystals. We describe a scalable implementation of the method using Hypre. Phase velocity of long wavelength transverse phonons is found to be a factor of 5-7 larger than in the corresponding Coulomb crystal model, which could have implications for low temperature phononmediated thermal conductivity. Other findings include c < 0 elastic instabilities for both bcc and fcc lattices, reminiscent of the situation in some light actinides, and suggestive of a symmetry-lowering transition to a tetragonal or orthorhombic lattice.

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“…For numerical purposes, we use κ ρ = 10 16 cm 2 s −2 since it would be a fit compatible with  m k = p p with κ p ≈ 0.01 (Chamel & Haensel 2008), for the EOSs used. For completeness, we stress that elasticity could also be present in other parts of an NS, such as its mixed phase/state (Johnson-McDaniel & Owen 2012, 2013, or even the quark core (Mannarelli et al 2007). However, we leave breaking analyses of these phases for future works.…”

Section: Modelsmentioning

confidence: 99%

Crustal Failure as a Tool to Probe Hybrid Stars

Pereira

Bejger

Haensel

et al. 2023

ApJ

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It is currently unknown if neutron stars (NSs) are composed of nucleons only or are hybrid stars, i.e., in addition to nucleonic crusts and outer cores, they also possess quark cores. Quantum chromodynamics allows for such a possibility, but accurate calculations relevant for compact stars are still elusive. Here we investigate some crust-breaking aspects of hybrid stars. We show that the crust-breaking frequency and maximum fiducial ellipticity are sensitive to the quark–hadron density jump and equation of state stiffness. Remarkably, the crust-breaking frequency related to static tides scales linearly with the mass of the star (for a given companion mass), and its slope encompasses information about the microphysics of the star. However, for precise crust-breaking frequency predictions, relativistic corrections to Kepler’s third law and the Newtonian tidal field should not be ignored. When a liquid quark core touches an elastic hadronic phase (the result of a significant energy density jump), the maximum ellipticity can increase by around an order of magnitude when compared to a liquid quark core touching a liquid hadronic phase. That is relevant because it would increase the odds of detecting continuous gravitational waves from NSs. Our order-of-magnitude analysis also suggests that a given upper limit to the ellipticity (crust-breaking frequency) could have representatives in stars with either small or intermediate (large) energy density jumps. Therefore, when upper limits to the ellipticity for isolated stars are better constrained or electromagnetic radiation (e.g., gamma-ray precursors) is detected along with gravitational waves in inspiraling binary systems, they may help constrain some aspects of phase transitions in NSs.

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Shear modulus of the hadron-quark mixed phase

Cited by 11 publications

References 99 publications

Amorphous state in the mixed phase of hadron-quark phase transition in protoneutron stars

Amorphous state in the mixed phase of hadron-quark phase transition in protoneutron stars

Microphysics of Neutron Star Outer Envelopes in the Periodized, Magnetic Thomas-Fermi Model

Crustal Failure as a Tool to Probe Hybrid Stars

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