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Journal articles on the topic 'Neutron Degeneracy Pressure'

Author: Grafiati

Published: 5 June 2025

Last updated: 2 August 2025

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1

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’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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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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8

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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11

Gaztanaga, Enrique. "The Black Hole Universe, Part II." Symmetry 14, no. 10 (2022): 1984. http://dx.doi.org/10.3390/sym14101984.

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In part I of this series, we showed that the observed Universe can be modeled as a local Black Hole of fixed mass M≃6×1022M⊙, without Dark Energy: cosmic acceleration is caused by the Black Hole event horizon rS = 2GM. Here, we propose that such Black Hole Universe (together with smaller primordial Black Holes) could form from the hierarchical free-fall collapse of regular matter. We argue that the singularity could be avoided with a Big Bounce explosion, which results from neutron degeneracy pressure (Pauli exclusion principle). This happens at GeV energies, like in core collapse supernova, w

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12

PÉREZ MARTÍNEZ, A., H. PÉREZ ROJAS, H. J. MOSQUERA CUESTA, M. BOLIGAN, and M. G. ORSARIA. "QUARK STARS AND QUANTUM-MAGNETICALLY INDUCED COLLAPSE." International Journal of Modern Physics D 14, no. 11 (2005): 1959–69. http://dx.doi.org/10.1142/s0218271805007401.

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Quark matter is expected to exist in the interior of compact stellar objects as neutron stars or even the more exotic strange stars, based on the Bodmer–Witten conjecture. Bare strange quark stars and (normal) strange quark-matter stars, those possessing a baryon (electron-supported) crust, are hypothesized as good candidates to explain the properties of a set of peculiar stellar sources such as the enigmatic X-ray source RX J1856.5-3754, some pulsars such as PSR B1828-11 and PSR B1642-03, and the anomalous X-ray pulsars and soft γ-ray repeaters. In the MIT bag model, quarks are treated as a d

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13

Demissie, Abbi Seyoum. "The Contribution of Degenerate Electron Pressure to The Stability of The Outer Region of Thin Keplerian Accretion Disks Around a Neutron Star." JOURNAL OF ADVANCES IN PHYSICS 11, no. 1 (2015): 2886–91. http://dx.doi.org/10.24297/jap.v11i1.575.

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The stability analysis of a geometrically thin, gas-pressure dominated accretion disk aroundÂ a neutron star is presented. In purely radial perturbation case, thin disk is stable to thermal modes. The stability is analyzed at a small temperature, that is temperature approaching zero and at definite temperature. The contribution of both fully and partially degenerate electrons pressure for the stability of the disk in its outer region is investigated. We find that the disk is stable in this region, where the gas pressure is more dominant than radiation pressure.

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Aksenov, A. G., and V. M. Chechetkin. "Large-Scale Convection during Gravitational Collapse with Neutrino Transport in 2D and 3D Models on Fine Grids." Астрономический журнал 100, no. 3 (2023): 221–32. http://dx.doi.org/10.31857/s0004629923030015.

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The problem of the gravitational collapse of the core of a massive star is considered, taking into account the neutrino transport in the flux-limited diffusion approximation. To reduce the computational domain of a multidimensional problem on a fixed computational grid, the core of a star, which is already at the stage of collapse, is considered. Since the collapse stage is delayed in time compared to the gas-dynamic time scale for an emerging proto-neutron star, we consider the mathematical problem for the initial configuration in equilibrium and neglected the initial radial velocity. Pressur

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15

GAO, ZHI FU, NA WANG, QIU HE PENG, XIANG DONG LI, and YUAN JIE DU. "PRESSURE OF DEGENERATE AND RELATIVISTIC ELECTRONS IN A SUPERHIGH MAGNETIC FIELD." Modern Physics Letters A 28, no. 36 (2013): 1350138. http://dx.doi.org/10.1142/s0217732313501381.

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Based on our previous work, we deduce a general formula for pressure of degenerate and relativistic electrons, Pe, which is suitable for superhigh magnetic fields, discuss the quantization of Landau levels of electrons, and consider the quantum electrodynamic (QED) effects on the equations of states (EOSs) for different matter systems. The main conclusions are as follows: Pe is related to the magnetic field B, matter density ρ, and electron fraction Ye; the stronger the magnetic field, the higher the electron pressure becomes; the high electron pressure could be caused by high Fermi energy of

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16

GREGG, MICHAEL, and SETH A. MAJOR. "ON MODIFIED DISPERSION RELATIONS AND THE CHANDRASEKHAR MASS LIMIT." International Journal of Modern Physics D 18, no. 06 (2009): 971–82. http://dx.doi.org/10.1142/s021827180901487x.

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Modified dispersion relations from effective field theory are shown to alter the Chandrasekhar mass limit. At exceptionally high densities, the modifications affect the pressure of a degenerate electron gas and can increase or decrease the mass limit, depending on the sign of the modifications. These changes to the mass limit are unlikely to be relevant to the astrophysics of white dwarf or neutron stars, due to the well-known dynamical instabilities that occur at lower densities. Generalizations to frameworks other than effective field theory are discussed.

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17

Workman, John M., Harry B. Fannin, Peter G. Brown, and Joseph A. Caruso. "A Comparative Study of Electron Density Determination Methodologies in the Helium Microwave-Induced Plasma." Applied Spectroscopy 43, no. 4 (1989): 621–26. http://dx.doi.org/10.1366/0003702894202599.

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Electron number densities were examined in a low-power atmospheric-pressure helium microwave-induced plasma. Two hydrogen-based methods and two helium-based methods were employed to estimate electron concentration. The hydrogen 4471 Å Balmer line was examined with the use of both line shape and full width at half-maximum intensity measurements. The data suggest that half-width calculations underestimate electron densities. Half-width measurements of neutral helium lines result in number densities which appear to be overestimated. This inaccuracy is thought to be the result of apparatus broaden

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18

Argüelles, C. R., A. Krut, J. A. Rueda, and R. Ruffini. "Can fermionic dark matter mimic supermassive black holes?" International Journal of Modern Physics D 28, no. 14 (2019): 1943003. http://dx.doi.org/10.1142/s021827181943003x.

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We analyze the intriguing possibility of explaining both dark mass components in a galaxy: the dark matter (DM) halo and the supermassive dark compact object lying at the center, by a unified approach in terms of a quasi-relaxed system of massive, neutral fermions in general relativity. The solutions to the mass distribution of such a model that fulfill realistic halo boundary conditions inferred from observations, develop a high-density core supported by the fermion degeneracy pressure able to mimic massive black holes at the center of galaxies. Remarkably, these dense core-diluted halo confi

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19

Baiko, D. A., and A. I. Chugunov. "Ab initio thermodynamics of one-component plasma for astrophysics of white dwarfs and neutron stars." Monthly Notices of the Royal Astronomical Society 510, no. 2 (2021): 2628–43. http://dx.doi.org/10.1093/mnras/stab3613.

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ABSTRACT Using path-integral Monte Carlo (PIMC) simulations, we have calculated energy of a crystal composed of atomic nuclei and uniform incompressible electron background in the temperature and density range, covering fully ionized layers of compact stellar objects, white dwarfs, and neutron stars, including the high-density regime, where ion quantization is important. We have approximated the results by convenient analytic formulae, which allowed us to integrate and differentiate the energy with respect to temperature and density to obtain various thermodynamic functions such as Helmholtz f

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20

AHLUWALIA, D. V. "ON QUANTUM NATURE OF BLACK-HOLE SPACETIME: A POSSIBLE NEW SOURCE OF INTENSE RADIATION." International Journal of Modern Physics D 08, no. 05 (1999): 651–57. http://dx.doi.org/10.1142/s0218271899000456.

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Atoms and the planets acquire their stability from the quantum mechanical incompatibility of the position and momentum measurements. This incompatibility is expressed by the fundamental commutator [x, px]=iℏ, or equivalently, via the Heisenberg's uncertainty principle Δx Δ px~ℏ. A further stability-related phenomenon where the quantum realm plays a dramatic role is the collapse of certain stars into white dwarfs and neutron stars. Here, an intervention of the Pauli exclusion principle, via the fermionic degenerate pressure, stops the gravitational collapse. However, by the neutron-star stage t

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21

Provencal, J. L., J. C. Clemens, G. Henry, et al. "The Time Dependence of the Phases of the Harmonics Relative to the 1490 sec Fundamental in PG1346+082." International Astronomical Union Colloquium 114 (1989): 296–99. http://dx.doi.org/10.1017/s0252921100099759.

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White dwarf stars provide important boundary conditions for the understanding of stellar evolution. An adequate understanding of even these simple stars is impossible without detailed knowledge of their interiors. PG1346+082, an interacting binary white dwarf system, provides a unique opportunity to view the interior of one degenerate as it is brought to light in the accretion disk of the second star as the primary strips material from its less massive companion (see Wood et at. 1987).PG1346+082 is a photometric variable with a four magnitude variation over a four to five day quasi-period. A f

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22

Punjabi, Alkesh, and George Vahala. "Effects of positive potential in the catastrophe theory study of the point model for bumpy tori." Journal of Plasma Physics 33, no. 1 (1985): 119–49. http://dx.doi.org/10.1017/s0022377800002361.

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With positive ambipolar potential, ion non-resonant neoclassical transport leads to increased particle confinement times. In certain regimes of filling pressure, microwave powers (ECRH and ICRH) and positive potential, new folds can now emerge from previously degenerate equilibrium surfaces allowing for distinct C, T, and M modes of operation. A comparison in the equilibrium fold structure is also made between (i) equal particle and energy confinement times, and (ii) particle confinement times enhanced over the energy confinement time. The nonlinear time evolution of these point model equation

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23

Irfan, M., S. Ali, Arshad M. Mirza, and Yunliang Wang. "Modulationally stable envelope solitons in astrophysical magnetoplasmas with degenerate relativistic electrons." Journal of Plasma Physics 81, no. 6 (2015). http://dx.doi.org/10.1017/s0022377815001208.

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The formation and propagation characteristics of small-amplitude magnetoacoustic dark/grey solitons are investigated in a semi relativistic degenerate magnetoplasma whose constituents are electrons and singly ionized positive ions. For this purpose, the electrons are assumed to follow the degeneracy pressure law through the Chandrasekhar equation of state, while the inertial cold ions are taken as non-degenerate and magnetized. By solving the one-fluid quantum magnetohydrodynamic (QMHD) model with the aid of a reductive perturbation technique, a nonlinear Schrödinger (NLS) equation is derived

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24

Kim, Yoonsoo, Jinho Kim, Hee Il Kim, and Hyung Mok Lee. "General relativistic self-gravitating equilibrium disks around rotating neutron stars." Monthly Notices of the Royal Astronomical Society, October 4, 2024. http://dx.doi.org/10.1093/mnras/stae2287.

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Abstract In modeling a relativistic disk around a compact object, the self-gravity of the disk is often neglected while it needs to be incorporated for more accurate descriptions in several circumstances. Extending the Komatsu-Eriguchi-Hachisu self-consistent field method, we present numerical models of a rapidly rotating neutron star with a self-gravitating disk in stationary equilibrium. In particular, our approach allows us to obtain numerical solutions involving a massive disk with the rest mass $\mathcal {O}(10^{-1})-\mathcal {O}(10^0)\, M_\odot$ closely attached to a rotating neutron sta

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25

Irfan, M., S. Ali, and Arshad M. Mirza. "Magnetoacoustic solitons and shocks in dense astrophysical plasmas with relativistic degenerate electrons." Journal of Plasma Physics 82, no. 1 (2016). http://dx.doi.org/10.1017/s0022377816000040.

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Two-fluid quantum magnetohydrodynamic (QMHD) equations are employed to investigate linear and nonlinear properties of the magnetosonic waves in a semi-relativistic dense plasma accounting for degenerate relativistic electrons. In the linear analysis, a plane wave solution is used to derive the dispersion relation of magnetosonic waves, which is significantly modified due to relativistic degenerate electrons. However, for a nonlinear investigation of solitary and shock waves, we employ the reductive perturbation technique for the derivation of Korteweg–de Vries (KdV) and Korteweg–de Vries Burge

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26

Jacak, Janusz Edward. "Quantum mechanism of extremely high energy processes at neutron star collapse and of quasar luminosity." Journal of High Energy Physics 2022, no. 3 (2022). http://dx.doi.org/10.1007/jhep03(2022)002.

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Abstract Using the braid group topological approach to quantum statistics we demonstrate that for strong gravitational field occurring in neutron star merger with mass exceeding the Tolman, Oppenheimer and Volkoff limit the quantum statistics of particles beneath the photon sphere decays, which results in an instant relief of quantum degeneracy pressure in the star. This causes a rapid shrink of the matter to a black hole with quite different quantum collective character of particles. The scheme of neutron Fermi sphere collapse is proposed as the possible isotropic source of short giant gamma-

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27

An, Shihai, Fan Yang, Ying Sun, et al. "Emergent Multiple Spin States From Baromagnetic Effect in Strongly Correlated Magnet Mn₃GaC." Advanced Materials, March 23, 2025. https://doi.org/10.1002/adma.202420502.

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AbstractStrongly correlated magnets, exhibiting distinctive spin properties such as spin‐orbit coupling, spin polarization, and chiral spin, are regarded as the next‐generation high‐density magnetic storage materials in spintronics. Nevertheless, owing to intricate spin interactions, realizing controllable spin arrangement and high‐density magnetic storage remains a formidable challenge. Here, controllable multiple spin states induced by the baromagnetic effect in kagome lattice magnet Mn₃GaC are first reported, achieved by manipulating spin rotation within the spin‐polarized plane employing p

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28

Rozina, Ch, N. L. Tsintsadze, and L. N. Tsintsadze. "Magnetic field quantization in pulsars." Journal of Plasma Physics 86, no. 2 (2020). http://dx.doi.org/10.1017/s0022377820000252.

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Magnetic field quantization is an important issue for degenerate environments such as neutron stars, radio pulsars and magnetars etc., due to the fact that these stars have a magnetic field higher than the quantum critical field strength of the order of $4.4\times 10^{13}~\text{G}$ , accordingly, the cyclotron energy may be equal to or even much more than the Fermi energy of degenerate particles. We shall formulate here the exotic physics of strongly magnetized neutron stars, known as pulsars, specifically focusing on the outcomes of the quantized magnetic pressure. In this scenario, while fol

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29

"Incommensurate Crystallization of Neutron Matter in Neutron Stars." Issue 2 2020, no. 2 (2020). http://dx.doi.org/10.26565/2312-4334-2020-2-04.

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The composition of the neutron stars from its surface region, outer-core, inner-core, and to its center is still being investigated. One can only surmise on the properties of neutron stars from the spectroscopic data that may be available from time to time. A few models have suggested that the matter at the surface region of the neutron star is composed of atomic nuclei that get crushed under extremely large pressure and gravitational stress, and this leads to the creation of solid lattice with a sea of electrons, and perhaps some protons, flowing through the gaps between them. Nuclei with hig

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30

Shick, Alexander B., Václav Janiš, Václav Drchal, and Warren E. Pickett. "Pressure Dependence of Magnetic States of UGe2." MRS Proceedings 802 (2003). http://dx.doi.org/10.1557/proc-802-dd6.10.

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ABSTRACTThe correlated band theory picture (LSDA+U) has been applied to UGe2, in which superconductivity has been found to coexist with robust ferromagnetism. Over a range of volumes (i.e. pressures), two nearly degenerate states are obtained, which differ most strikingly in their orbital character (on uranium). The calculated moment, and its separation into spin and orbital parts, is consistent with recent polarized neutron scattering data. These two states are strong candidates for the two ferromagnetic phases, one low-temperature -- low-pressure, the other higher-temperature -- higher press

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Mukta, K. N., M. S. Zobaer, N. Roy, and A. A. Mamun. "Compressive and rarefactive dust ion-acoustic solitary waves with degenerate electron–positron–ion plasma." Journal of Plasma Physics 81, no. 3 (2015). http://dx.doi.org/10.1017/s0022377813000032.

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The nonlinear propagation of dust ion-acoustic (DIA) waves in a unmagnetized collisionless degenerate dense plasma (containing degenerate electron and positron, and classical ion fluids) has been theoretically investigated. The K-dV equation has been derived by employing the reductive perturbation method and by taking into account the effect of different plasma parameters in plasma fluid. The stationary solitary wave solution of K-dV equation is obtained, and numerically analyzed to identify the basic properties of DIA solitary structures. It has been shown that depending on plasma parametric

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Dasgupta, Sayanti, and Pralay Kumar Karmakar. "Propagatory dynamics of nucleus-acoustic waves excited in gyrogravitating degenerate quantum plasmas electrostatically confined in curved geometry." Scientific Reports 11, no. 1 (2021). http://dx.doi.org/10.1038/s41598-021-98543-2.

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AbstractA theoretic model to investigate the dynamics of the longitudinal nucleus-acoustic waves (NAWs) in gyrogravitating electrostatically confined degenerate quantum plasma (DQP) system in spherically symmetric geometry is constructed. The model setup consists of non-degenerate heavy nuclear species (HNS), lighter nuclear species (LNS), and quantum degenerate electronic species (DES). It specifically considers the influences of the Bohm potential, Coriolis rotation, viscoelasticity, and electrostatic confinement pressure (ECP, scaling quadratically in density). A standard normal spherical m

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33

Shah, M. G., M. R. Hossen, and A. A. Mamun. "Nonlinear propagation of positron-acoustic waves in a four component space plasma." Journal of Plasma Physics 81, no. 5 (2015). http://dx.doi.org/10.1017/s0022377815001014.

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The nonlinear propagation of positron-acoustic waves (PAWs) in an unmagnetized, collisionless, four component, dense plasma system (containing non-relativistic inertial cold positrons, relativistic degenerate electron and hot positron fluids as well as positively charged immobile ions) has been investigated theoretically. The Korteweg–de Vries (K–dV), modified K–dV (mK–dV) and further mK–dV (fmK–dV) equations have been derived by using reductive perturbation technique. Their solitary wave solutions have been numerically analysed in order to understand the localized electrostatic disturbances.

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34

Rozina, Ch, Maroosh Akhter, Stefaan Poedts, and Hassan Amir Shah. "The impact of quantized magnetic pressure on the stimulated Brillouin scattering of electromagnetic waves." Physica Scripta, August 16, 2023. http://dx.doi.org/10.1088/1402-4896/acf0f4.

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Abstract Within the framework of Landau quantization theory of Fermi gas, we formulate here the exotic physics of magnetic stimulated Brillouin scattering instability (MSBS) arising due to the nonlinear interaction of high frequency electromagnetic waves (EMWs) with degenerate, strongly magnetized electron-ion plasma. Quantum magneto hydrodynamic model (QMHD) is followed to develop the basic differential equations of quantized magnetosonic waves (QMWs) in the presence of super strong magnetic (SSH) field, whereas Maxwell equations are used to derive the governing differential equation of pump

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35

Sarkar, M. M., S. Barua, and M. G. Hafez. "Ion-acoustic wave propagation with Bohm quantum potential near and at supercritical values in degenerate plasmas." Physics of Plasmas 32, no. 7 (2025). https://doi.org/10.1063/5.0274444.

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This research investigates the nonlinear propagation of solitons and periodic oscillatory waves near and at supercritical values (S-CVs) in a relativistic degenerate plasma consisting of relativistic electron and positron fluids, alongside an inertial nonrelativistic ion fluid, such as helium. By employing a higher-order correction within the reductive perturbation framework, a quartic nonlinear Korteweg–de Vries equation is derived. Solutions to this equation are explored, revealing both stationary soliton and novel periodic oscillatory wave structures. The study finds that factors such as th

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Douanla, Delmas Verres, Camus Gaston Tiofack Latchio, Alim Alim, et al. "Three-dimensional rogue waves and dust-acoustic dark solitons collisions in degenerate ultra dense magnetoplasma in the presence of dust pressure anisotropy." Physics of Fluids, July 9, 2022. http://dx.doi.org/10.1063/5.0096990.

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A three-dimensional Thomas-Fermi dense anisotropic magnetized plasma containing Fermi-Dirac distributed electrons and ions in addition with classical negatively charged dust grains is considered to analyse oblique modulational instability (MI) and head-on collisions among dust-acoustic (DA) dark solitons. The Chew{Goldberger{Low (CGL) description is employed to dene the anisotropicdust pressure. Following the multiscale reductive perturbation method, the (3+1)-dimensional nonlinear Schrodinger (NLS) equation has been derived and the MI criterion have been identified. It is found that for large

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García-Senz, Domingo, Rubén M. Cabezón, Moritz Reichert, et al. "Do not forget the electrons: Extending moderately-sized nuclear networks for multidimensional hydrodynamic codes." Astronomy & Astrophysics, July 24, 2024. http://dx.doi.org/10.1051/0004-6361/202449863.

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Nuclear networks are widely used coupled with hydrodynamical simulations of explosive scenarios to account for the change of nuclear species and energy generation rate due to nuclear reactions. In this way, there is a feedback mechanism between the hydrodynamical state and the nuclear processes. Unfortunately, the timescale of nuclear reactions is orders of magnitude smaller than the dynamical timescale that drives hydrodynamical simulations. Therefore, these nuclear networks are usually very small, reduced in most cases to a dozen elements, especially when simulations are carried out in more

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Ding, D., and J. B. Bostwick. "Oscillations of a partially wetting bubble." Journal of Fluid Mechanics 945 (July 21, 2022). http://dx.doi.org/10.1017/jfm.2022.584.

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We study the linear stability of a compressible sessile bubble in an ambient fluid that partially wets a planar solid support, where the gas is assumed to be an ideal gas that obeys the adiabatic law. The frequency spectrum is computed from an integrodifferential boundary value problem and depends upon the wetting conditions through the static contact angle $\alpha$ , the dimensionless equilibrium bubble pressure $\varPi$ , and the contact-line dynamics that we assume to be either (i) pinned or (ii) freely moving with fixed contact angle. Corresponding mode shapes are defined by the polar-azim

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Ai-Jun Dong, Zhifu Gao, Xiao Feng Yang, Na Wang, Chang Liu, and Qiu-He Peng. "The modified pressure of relativistic electrons in a superhigh magnetic field." Acta Physica Sinica, 2023, 0. http://dx.doi.org/10.7498/aps.72.20220092.

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Magnetars are a kind of pulsars powered by magnetic field energy. The study of magnetars is an important hotspot in the field of pulsars. In this paper, based on the work of Zhu Cui et al. (2016), we reinvestigate the Landau-level stability of electrons in a superhigh magnetic field (SMF), <em>B</em>>> <em>B</em><sub>cr</sub> (<em>B</em><sub>cr</sub> =4.414×10<sup>13</sup>G is the quantum critical magnetic field) and their influences on the pressure of electrons in magnetars. Firstly, we briefly review the pressure o

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