Relevant bibliographies by topics / Neutron Degeneracy Pressure

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Academic literature on the topic 'Neutron Degeneracy Pressure'

Author: Grafiati
Published: 5 June 2025
Last updated: 2 August 2025

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Journal articles on the topic "Neutron Degeneracy Pressure"

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Prosad, Bhattacharya. "Calculation of the TOV Limit Based on Neutron Degeneracy Pressure." Indian Journal of Advanced Physics (IJAP) 4, no. 1 (2024): 4–7. https://doi.org/10.54105/ijap.B1050.04010424.

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<strong>Abstract:</strong> Original theory on the mass limit beyond which a cold, non-rotating neutron star cannot be formed, instead only stellar black holes will be created, was stipulated by J.R. Oppenheimer and G.M. Volkoff based on R.C. Tolman&rsquo;s work in 1939. The limit calculated from the equation established by them is known as the TOV limit which is analogous to the Chandrasekhar limit for White Dwarfs. But the results obtained using the formula was found to be not valid today. Subsequent theoretical works place the limit in the range 1.5 to 3 solar masses. There are several basic
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2

Bhattacharya, Prosad. "Calculation of the TOV Limit Based on Neutron Degeneracy Pressure." Indian Journal of Advanced Physics 4, no. 1 (2024): 4–7. http://dx.doi.org/10.54105/ijap.b1050.04010424.

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Original theory on the mass limit beyond which a cold, non-rotating neutron star cannot be formed, instead only stellar black holes will be created, was stipulated by J.R. Oppenheimer and G.M. Volkoff based on R.C. Tolman’s work in 1939. The limit calculated from the equation established by them is known as the TOV limit which is analogous to the Chandrasekhar limit for White Dwarfs. But the results obtained using the formula was found to be not valid today. Subsequent theoretical works place the limit in the range 1.5 to 3 solar masses. There are several basic theories and related formulae fo
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3

Llamas, Gerardo Perez, and James Dove. "Modeling the Structure of a Neutron Star Using Relativistic Degeneracy Pressure." Journal of Undergraduate Research in Physics and Astronomy 34, no. 1 (2024): 100003. http://dx.doi.org/10.1063/10.0034184.

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4

Castillo, F., A. Reisenegger, and J. A. Valdivia. "Two-fluid simulations of the magnetic field evolution in neutron star cores in the weak-coupling regime." Monthly Notices of the Royal Astronomical Society 498, no. 2 (2020): 3000–3012. http://dx.doi.org/10.1093/mnras/staa2543.

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ABSTRACT In a previous paper, we reported simulations of the evolution of the magnetic field in neutron star (NS) cores through ambipolar diffusion, taking the neutrons as a motionless uniform background. However, in real NSs, neutrons are free to move, and a strong composition gradient leads to stable stratification (stability against convective motions) both of which might impact on the time-scales of evolution. Here, we address these issues by providing the first long-term two-fluid simulations of the evolution of an axially symmetric magnetic field in a neutron star core composed of neutro
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5

LONG, M. W. "MULTIPLE-Q STRUCTURES IN FRUSTRATED ANTIFERROMAGNETS." International Journal of Modern Physics B 07, no. 16n17 (1993): 2981–3002. http://dx.doi.org/10.1142/s0217979293003127.

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The concepts relevant to frustrated antiferromagnets are briefly reviewed. Antiferromagnets are classified according to their symmetry groups, with non-trivial point groups leading to the possibility of multiple-Q antiferromagnetism. The role of residual degeneracy is highlighted and the manner in which this degeneracy is lifted is discussed. The physical phenomena in competition within frustrated magnets, and the states that they prefer, yield ongoing theoretical research, and the way neutron scattering can be used, in conjunction with the application of pressure and magnetic fields, to deter
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DRYZEK, JERZY, AKIRA KATO, GERARDO MUÑOZ, and DOUGLAS SINGLETON. "ELECTRONS AS QUASI-BOSONS IN MAGNETIC WHITE DWARFS." International Journal of Modern Physics D 11, no. 03 (2002): 417–25. http://dx.doi.org/10.1142/s0218271802001512.

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A white dwarf star achieves its equilibrium from the balancing of the gravitational compression against the Fermi degeneracy pressure of the electron gas. In field theory there are examples (e.g. the monopole-charge system) where a strong magnetic field can transform a boson into a fermion or a fermion into a boson. In some condensed matter systems (e.g. fractional quantum Hall systems) a strong magnetic field can transform electrons into effective fermions, or effective anyons. Based on these examples we investigate the possibility that the strong magnetic fields of some white dwarfs may tran
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7

Lebert, Blair W., Tommaso Gorni, Michele Casula, et al. "Epsilon iron as a spin-smectic state." Proceedings of the National Academy of Sciences 116, no. 41 (2019): 20280–85. http://dx.doi.org/10.1073/pnas.1904575116.

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Using X-ray emission spectroscopy, we find appreciable local magnetic moments until 30 GPa to 40 GPa in the high-pressure phase of iron; however, no magnetic order is detected with neutron powder diffraction down to 1.8 K, contrary to previous predictions. Our first-principles calculations reveal a “spin-smectic” state lower in energy than previous results. This state forms antiferromagnetic bilayers separated by null spin bilayers, which allows a complete relaxation of the inherent frustration of antiferromagnetism on a hexagonal close-packed lattice. The magnetic bilayers are likely orientat
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SILVERMAN, M. P. "FERMION CONDENSATION IN A RELATIVISTIC DEGENERATE STAR: ARRESTED COLLAPSE AND MACROSCOPIC EQUILIBRIUM." International Journal of Modern Physics D 15, no. 12 (2006): 2257–65. http://dx.doi.org/10.1142/s0218271806009522.

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Fermionic Cooper pairing leading to the BCS-type hadronic superfluidity is believed to account for periodic variations ("glitches") and subsequent slow relaxation in spin rates of neutron stars. Under appropriate conditions, however, fermions can also form a Bose–Einstein condensate of composite bosons. Both types of behavior have recently been observed in tabletop experiments with ultra-cold fermionic atomic gases. Since the behavior is universal (i.e., independent of atomic potential) when the modulus of the scattering length greatly exceeds the separation between particles, one can expect a
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9

Moreno, Pablo Navarro, Aneta Wojnar, and Felipe J. Llanes-Estrada. "Testing gravity with the latent heat of neutron star matter." Journal of Cosmology and Astroparticle Physics 2025, no. 01 (2025): 015. https://doi.org/10.1088/1475-7516/2025/01/015.

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Abstract The Seidov limit is a bound on the maximum latent heat that a presumed first-order phase transition of neutron-star matter can have before its excess energy density, not compensated by additional pressure, results in gravitational collapse. Because latent heat forces an apparent nonanalytic behaviour in plots correlating physical quantities (kinks in two-dimensional, ridges in three-dimensional ones), it can be constrained by data. As the onset of collapse depends on the intensity of gravity, testing for sudden derivative changes and, if they are large, breaching the Seidov limit woul
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10

Zhu, Cui, Zhi Fu Gao, Xiang Dong Li, Na Wang, Jian Ping Yuan, and Qiu He Peng. "Modified Fermi energy of electrons in a superhigh magnetic field." Modern Physics Letters A 31, no. 11 (2016): 1650070. http://dx.doi.org/10.1142/s021773231650070x.

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In this paper, we investigate the electron Landau level stability and its influence on the electron Fermi energy, [Formula: see text], in the circumstance of magnetars, which are powered by magnetic field energy. In a magnetar, the Landau levels of degenerate and relativistic electrons are strongly quantized. A new quantity [Formula: see text], the electron Landau level stability coefficient is introduced. According to the requirement that [Formula: see text] decreases with increasing the magnetic field intensity [Formula: see text], the magnetic field index [Formula: see text] in the expressi
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Book chapters on the topic "Neutron Degeneracy Pressure"

1

Moffat, John W. "Stars and Black Holes." In The Shadow of the Black Hole. Oxford University Press, 2020. http://dx.doi.org/10.1093/oso/9780190650728.003.0003.

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Physicists began to believe in black holes when research revealed new information about the constitution of stars and their life cycles, indicating that a black hole represents the death of certain massive stars. Chandrasekhar used quantum mechanics and the notion of a degenerate electron gas to obtain the maximum mass of a white dwarf. A degenerate neutron gas produced enough pressure to stop the gravitational collapse of a massive star, producing a neutron star or pulsar. For a massive-enough star, the degenerate neutron gas fails to prevent gravitational collapse into a black hole. Supernov
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