Charge Screening Effect in the Hadron-Quark Mixed Phase

Endo, Tomoki; Maruyama, Toshiki; Chiba, Satoshi; Tatsumi, Toshitaka

doi:10.1143/ptp.115.337

Cited by 73 publications

(90 citation statements)

References 24 publications

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“…However, the case with V /S = 10 fm (which would correspond to a radius R = 3V /S = 30 fm if the drop were spherical) requires a more sophisticated analysis including the Coulomb potential and solving consistently the Poisson equation together with the other equations. Such analysis is beyond the scope of the present work, but, in spite of the problem being highly non-linear, some approximate conclusions can be foreseen in the light of previous works [37,38]. In Ref.…”

Section: Discussionmentioning

confidence: 78%

Surface tension of highly magnetized degenerate quark matter

Lugones

Grunfeld

2017

Phys. Rev. C

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We study the surface tension of highly magnetized three flavor quark matter within the formalism of multiple reflection expansion (MRE). Quark matter is described as a mixture of free Fermi gases composed by quarks u, d, s and electrons, in chemical equilibrium under weak interactions. Due to the presence of strong magnetic fields the particles' transverse motion is quantized into Landau levels, and the surface tension has a different value in the parallel and transverse directions with respect to the magnetic field. We calculate the transverse and longitudinal surface tension for different values of the magnetic field and for quark matter drops with different sizes, from a few fm to the bulk limit. For baryon number densities between 2 − 10 times the nuclear saturation density, the surface tension falls in the range 2 − 20 MeV /fm 2 . The largest contribution comes from strange quarks which have a surface tension an order of magnitude larger than the one for u or d quarks and more than two orders of magnitude larger than for electrons. Our results show that the total surface tension is quite insensitive to the size of the drop. We also find that the surface tensions in the transverse and parallel directions are almost unaffected by the magnetic field if eB is below ∼ 5 × 10 −3 GeV 2 . Nevertheless, for higher values of eB, there is a significant increase in the parallel surface tension and a significant decrease in the transverse one with respect to the unmagnetized case.

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Section: Discussionmentioning

confidence: 78%

Surface tension of highly magnetized degenerate quark matter

Lugones

Grunfeld

2017

Phys. Rev. C

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“…The transition from hadronic to quark matter is a first order transition which will take place through a mixed phase [71] if finite size effects and charge screening do not prohibit such a phase [101,102] (although see the comments in [103]). If the transition is sharp it happens at a specific critical pressure, where the density will be discontinuous and heat will be released there at a total rate of −e −φ T ∆σ(dN q /dt), with dN q /dt the number of particles making the transition per unit time.…”

Section: Latent Heat Of Phase Transitionsmentioning

confidence: 99%

Pulsars as Astrophysical Laboratories for Nuclear and Particle Physics

Weber¹

2017

190

265

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A forefront area of research concerns the exploration of the properties of hadronic matter under extreme conditions of temperature and density, and the determination of the equation of state-the relation between pressure, temperature and density-of such matter. Experimentally, relativistic heavy-ion collision experiments enable physicists to cast a brief glance at hot and ultra-dense matter for times as little as about 10 −22 seconds. Complementary to this, the matter that exists in the cores of neutron stars, observed as radio pulsars, X-ray pulsars, and magnetars, is at low temperatures but compressed permanently to ultra-high densities that may be more than an order of magnitude higher than the density of atomic nuclei. This makes pulsars superb astrophysical laboratories for medium and high-energy nuclear physics, as discussed in this paper.

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“…We use our previous formulation [9,10], which we briefly review here. The quark phase consists of the lighter u, d, and s quarks, together with electrons.…”

Section: Formalism and Numerical Resultsmentioning

confidence: 99%

“…We also adopt the EOS derived in a previous paper [9] and then apply it to the TOV equation [10,16]. For comparison, we perform a calculation for a stationary rotating star using our EOS.…”

Section: Formalism and Numerical Resultsmentioning

confidence: 99%

Impact of Rotation on Quark–Hadron Hybrid Stars

Endo

2018

Proceedings of the Workshop on Quarks and Compact Stars 2017 (QCS2017)

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Many recent observations give restrictions to the equation of state (EOS) for high-density matter. Theoretical studies are needed to try to elucidate these EOSs at high density and/or temperature. With the many known rapidly rotating neutron stars, e.g., pulsars, several theoretical studies have tried to take into account the effects of rotation. In our study of these systems, we find that one of our EOSs is consistent with recent observation, whereas the other is inconsistent.

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Charge Screening Effect in the Hadron-Quark Mixed Phase

Cited by 73 publications

References 24 publications

Surface tension of highly magnetized degenerate quark matter

Surface tension of highly magnetized degenerate quark matter

Pulsars as Astrophysical Laboratories for Nuclear and Particle Physics

Impact of Rotation on Quark–Hadron Hybrid Stars

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