The Equation of State of Neutron Star Matter

Bombaci, Ignazio

doi:10.1007/978-3-030-85198-9_9

Cited by 2 publications

(2 citation statements)

References 116 publications

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“…Thus, matter breaks when the pressure of gravity corresponds to ρ c = ρ M /α G ≈ 3.3 • 10 18 kg/m 3 . As the ratio of strong force to gravity yields an order of magnitude ρ c larger than the Tolman-Oppenheimer-Volkov limit or the nuclear saturation density, ρ o [92], there should be stars in the range from ρ d ≈ 5.0 • 10 17 kg/m 3 to ρ c ≈ 3.3 • 10 18 kg/m 3 that are massive, M, enough to be black, c 2 < 4πGρr 2 = GM/r, but sparse, ρ, enough not to collapse [93,94]. From this perspective, dormant stellar black holes are, in fact, compact stars with inner shells of neutron, tetraquark, and dineutron lattices.…”

Section: Breakdownmentioning

confidence: 98%

Neutron star characteristics from the neutron structure

Annila

2023

Front. Phys.

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We draw insight into the neutron star structure and characteristics from the neutron structure. The eigenvectors of the special unitary group, SU(3), describing baryons, imply that neutron quarks reside on three faces of a tetrahedron. The tetrahedral structure accounts for the neutron magnetic moment and mass. Thus, we reason that neutrons precipitate with aligned magnetic moments into the triakis truncated tetrahedron tessellation under immense gravitational pressure. As the particle’s tetrahedral symmetry does not match the crystal’s rhombic symmetry, the total magnetic moment invariably misaligns with the star’s spinning axis. We infer further from the neutron structure that with increasing gravitational pressure, two neutrons condense into the same tetrahedron. Due to doubling density, the contracting star spins up abruptly but then settles down slowly as the gradients in density smoothen. As down quarks are positioned for pairwise fusions into anti-up quarks in the dineutron, we reason that tetraquark indeed forms as gravitational pressure increases further. The star balances the accompanying loss of mass by spinning down suddenly but recovers as the gradients in density smoothen again. Ultimately, when gravitational pressure increases even more, the anti-up quarks will annihilate with up quarks. As the core becomes ever more structured, such high-energy events fade out, and eventually, only magnetic field-collimated radio-frequency dissipation drives the spin down. The nuclear moments manifest fully in a magnetar, free from floating, hence counteraligning baryonic matter. In conclusion, the neutron structure makes sense of the neutron star density, magnetism, beams at an angle to the spinning axis, and pulsing transients, and paves the way for making sense of reactions in a black hole.

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Section: Breakdownmentioning

confidence: 98%

Neutron star characteristics from the neutron structure

Annila

2023

Front. Phys.

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“…• If SQM is not the true ground state of baryonic matter but is only a metastable state, hybrid stars (NSs consisting of an SQM core or a hadron-quark mixed phase) might exist (e.g., [38][39][40]). • There is the possibility that metastable hadronic stars could coexist with SSs, which is called the two-families scenario (e.g., [41][42][43][44][45]).…”

Section: Introductionmentioning

confidence: 99%

Confronting Strange Stars with Compact-Star Observations and New Physics

Yang

Zheng

et al. 2023

Universe

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Strange stars ought to exist in the universe according to the strange quark matter hypothesis, which states that matter made of roughly equal numbers of up, down, and strange quarks could be the true ground state of baryonic matter rather than ordinary atomic nuclei. Theoretical models of strange quark matter, such as the standard MIT bag model, the density-dependent quark mass model, or the quasi-particle model, however, appear to be unable to reproduce some of the properties (masses, radii, and tidal deformabilities) of recently observed compact stars. This is different if alternative gravity theory (e.g., non-Newtonian gravity) or dark matter (e.g., mirror dark matter) are considered, which resolve these issues. The possible existence of strange stars could thus provide a clue to new physics, as discussed in this review.

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The Equation of State of Neutron Star Matter

Cited by 2 publications

References 116 publications

Neutron star characteristics from the neutron structure

Neutron star characteristics from the neutron structure

Confronting Strange Stars with Compact-Star Observations and New Physics

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