On Dense Matter

Fowler, R. H.

doi:10.1093/mnras/87.2.114

Cited by 270 publications

(129 citation statements)

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“…In a series of papers Fowler, Chandrasekhar, Bohm, Pines, and Levine ( [7,11,16,24,34]) have founded the concepts of relativistic-degeneracy and quantum plasma theories. Recent developments of quantum hydrodynamics (QHD) ( [18,26]) and spin-1/2 quantum magnetohydrodynamics (QMHD) models ( [9,27,28]) based on Wigner-Poisson and Schrödinger-Poisson formulation (e.g.…”

Section: Introductionmentioning

confidence: 99%

Shukla–Eliasson attractive force: Revisited

Akbari-Moghanjoughi¹

2012

J. Plasma Phys.

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By investigation of the dielectric response of a Fermi-Dirac plasma in the linear limit and evaluation of the electrostatic potential around the positive stationary test charge, we find that the Shukla-Eliasson attractive force is present for the plasma density range expected in the interiors of large planets for a wide range of plasma atomic-number. This research which is based on the generalized electron Fermi-momentum further confirms the existence of the newly discovered Lennard-Jones-like attractive potential and its inevitable role in plasma crystallization in the cores of planets. Moreover, it is observed that the characteristics of the attractive potential is strongly sensitive to the variation of the plasma density and composition. Current research can also have applications in the study of strong laser-matter interactions and inertially confined plasmas.

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Section: Introductionmentioning

confidence: 99%

Shukla–Eliasson attractive force: Revisited

Akbari-Moghanjoughi¹

2012

J. Plasma Phys.

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“…Once in this state, the fermions resist further compression, a force known as degeneracy pressure. In 1926 Sir Ralph Fowler showed that electron degeneracy pressure could theoretically support a white dwarf against gravitational collapse (Fowler 1926).…”

Section: White Dwarf Structurementioning

confidence: 99%

Ultracool Companions to White Dwarfs

Steele

Burleigh²,

Barstow³

et al. 2010

AIP Conference Proceedings

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“…However, according to the Pauli Exclusion Principle, no two electrons can occupy the same quantum state, which has a finite volume in position-momentum space, so there is a limit where a repulsive force arising from this, the "electron degeneracy pressure", resists further compression of the material. Fowler (1926) showed that this pressure could support a stellar mass against gravitational collapse and proposed that this might explain the existence of white dwarfs. Combining this insight with the equations of stellar structure, Chandrasekhar (1931Chandrasekhar ( , 1935 determined the mass-radius relation for white dwarfs and the maximum mass (1.4M ) that electron degeneracy pressure could support against gravity, the Chandrasekhar limit.…”

Section: Physical Structure and Classification Of White Dwarfsmentioning

confidence: 99%

Structure and Evolution of White Dwarfs and their Interaction with the Local Interstellar Medium

Barstow

Werner

2006

Astrophys Space Sci

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Abstract:The development of far-UV astronomy has been particularly important for the study of hot white dwarf stars. A significant fraction of their emergent flux appears in the far-UV and traces of elements heavier than hydrogen or helium are, in general, only detected in this waveband or at shorter wavelengths that are also only accessible from space. Although white dwarfs have been studied in the far-UV throughout the past ~25 years, since the launch of IUE, only a few tens of objects have been studied in great detail and a much larger sample is required to gain a detailed understanding of the evolution of hot white dwarfs and the physical processes that determine their appearance. We review here the current knowledge regarding hot white dwarfs and outline what work needs to be carried out by future far-UV observatories.

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On Dense Matter

Cited by 270 publications

References 0 publications

Shukla–Eliasson attractive force: Revisited

Shukla–Eliasson attractive force: Revisited

Ultracool Companions to White Dwarfs

Structure and Evolution of White Dwarfs and their Interaction with the Local Interstellar Medium

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