Journal ArticleDOI
Phase transition from baryon to quark matter
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In this article, it was shown that if the mean distance between quarks in different baryons is larger than 10−13 cm, the description of matter as interacting baryonic matter becomes invalid, and instead, a description of a matter composed of quarks becomes relevant.Abstract:
THE equation of state of matter compressed to supernuclear densities is of considerable interest in astrophysics. For example, pulsars are stars compressed to densities greater than the density of atomic nuclei and are thought to be composed primarily of neutrons, based on detailed calculations of the equation of state of baryonic matter assuming that interaction potentials for the baryons (nucleons and hyperons) are derived from low energy nuclear physics1. There is, however, considerable evidence from high energy physics that baryons have structure, and it is currently believed that this structure is due to the fact that all hadrons consist of quarks bound by vector gluons2. The fact that free, isolated quarks have not been observed has led to the speculation that quarks may be permanently bound inside hadrons3. Since the quarks inside the nucleon behave as free particles2, the forces confining the quarks apparently become strong only when the distance between quarks exceeds the radius of a nucleon, ∼ 10−13 cm. When the density of matter is increased beyond the point that the mean distance between quarks in different baryons is ≪ 10−13 cm the description of matter as interacting baryons becomes invalid, and instead, a description of matter composed of quarks becomes relevant. At sufficiently high densities matter will behave like a relativistic gas of free quarks4 with P ≃ ρ/3, where P is the pressure and ρ is the energy density of matter. The density at which the baryon to quark transition occurs is of crucial importance to the structure of pulsars. General relativity implies that for a given equation of state there is a maximum energy density for stable stars1. It is therefore of considerable interest to know whether the energy density of baryon matter at the baryon–quark phase transition is less than this maximum value. Indeed, it has recently been suggested5 that the existence of quark matter inside pulsars would allow larger masses for pulsars than was previously thought possible. We will show, however, that there are reasons to doubt this.read more
Citations
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Quark phases in neutron stars and a third family of compact stars as signature for phase transitions
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Physics and astrophysics of strange quark matter
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Phase transitions and crystalline structures in neutron star cores
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References
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Journal ArticleDOI
Superdense Matter: Neutrons Or Asymptotically Free Quarks?
John Collins,Malcolm J. Perry +1 more
TL;DR: The quark model implies that superdense matter (found in neutron star cores, exploding black holes, and the early big-bang universe) consists of quarks rather than of hadrons as discussed by the authors.
Journal ArticleDOI
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Journal ArticleDOI
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V.R. Pandharipande,R.A. Smith +1 more
TL;DR: In this paper, the energy of solid neutron matter configurations in which layers of parallel spin neutrons with spin direction perpendicular to the plane of the layer are stacked such that neutrons in adjacent layers have antiparallel spins was investigated.
Journal ArticleDOI
Obese ‘neutron’ stars
K. Brecher,George J Caporaso +1 more
TL;DR: In this paper, it was shown that non-rotating, spherically symmetric, general relativistic "neutron" stars of mass ≥ 3M⊙ are consistent with the known laws of physics.