scholarly journals Equation of state and force fields for Feynman–Hibbs-corrected Mie fluids. I. Application to pure helium, neon, hydrogen, and deuterium

2019 ◽  
Vol 151 (6) ◽  
pp. 064508 ◽  
Author(s):  
Ailo Aasen ◽  
Morten Hammer ◽  
Åsmund Ervik ◽  
Erich A. Müller ◽  
Øivind Wilhelmsen
2020 ◽  
Vol 152 (7) ◽  
pp. 074507 ◽  
Author(s):  
Ailo Aasen ◽  
Morten Hammer ◽  
Erich A. Müller ◽  
Øivind Wilhelmsen

The deviations from the equation of state for perfect gases which are observed in all known gases result from the interactions of their constituent atoms or molecules. The excess pressures observed at all but the lowest temperatures show that the dominating factor is the strong repulsion between atoms at close renge, due to the interpentration of complete electron shells. Little is known about these repulsions, and that is readily summarized. Between atoms with spherically symmetrical distributions it is likely that the repulsive potential is accurately represented by a function P(r)e -r/p , (1) Where r is separation of the atomic nuclei and P(r) a polynomial in r . Quantum theoretical calculations made by Slater (1928) for helium atoms (with a closed shell of two electrons) and by Bleick and Mayer (1934) for neon atoms (with a closed shell of eight electrons) show that an adequate expression may sometimes be obtained if the polynomial is replaced by a constant. Some confirmation of this (though over a very restricted range of r ) is given by Born and Mayer (1932) and Huggins (1937), whose work on ionic cubic crystals shows that their elastic properties are admirably correlated when the repulsive potential of two ions of rare gas type is represented by an exponential function be -r/p , with a range of about one atomic diameter.


1989 ◽  
Vol 114 ◽  
pp. 300-304
Author(s):  
D. Saumon ◽  
G. Chabrier

Studies of the structure and evolution of low mass stars, brown dwarfs and giant planets require an equation of state (EOS) that includes a detailed, accurate model of the strongly non-ideal behavior of matter in these cool, compact objects [Fig. (1)]. Physical processes in the outer layers of white dwarfs, especially the analysis of the pulsation properties of ZZ Ceti stars, depend sometimes critically on the thermal properties of partially ionized hydrogen. In view of the substantial developments in the statistical physics of dense fluids and plasmas over the past decade, the computation of a new, independent EOS for astrophysical applications is justified. The statistical mechanical models which we present for hydrogen can be adapted to treat both pure helium and hydrogen-helium mixtures.


Author(s):  
John W. Coleman

In the design engineering of high performance electromagnetic lenses, the direct conversion of electron optical design data into drawings for reliable hardware is oftentimes difficult, especially in terms of how to mount parts to each other, how to tolerance dimensions, and how to specify finishes. An answer to this is in the use of magnetostatic analytics, corresponding to boundary conditions for the optical design. With such models, the magnetostatic force on a test pole along the axis may be examined, and in this way one may obtain priority listings for holding dimensions, relieving stresses, etc..The development of magnetostatic models most easily proceeds from the derivation of scalar potentials of separate geometric elements. These potentials can then be conbined at will because of the superposition characteristic of conservative force fields.


1998 ◽  
Vol 94 (5) ◽  
pp. 809-814 ◽  
Author(s):  
C. BARRIO ◽  
J.R. SOLANA

2000 ◽  
Vol 10 (PR5) ◽  
pp. Pr5-281-Pr5-286
Author(s):  
M. Ross ◽  
L. H. Yang ◽  
G. Galli

1980 ◽  
Vol 41 (C2) ◽  
pp. C2-83-C2-83
Author(s):  
Ph. Choquard
Keyword(s):  

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