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Equation of State at Densities Greater than Nuclear Density

Published online by Cambridge University Press:  14 August 2015

H. A. Bethe
H. A. Bethe*
Affiliation:
Laboratory of Nuclear Studies Cornell University, Ithaca, N.Y. 14850, U.S.A.

Abstract

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An equation of state is developed for densities from nuclear density (3 x 1014 g cm−3) to about 1016 g cm−3. The repulsive interaction between baryons dominates and empirical arguments for its existence are given. This interaction is attributed to vector meson exchange, and is derived from classical field theory whereupon a Yukawa potential results. The potential actually assumed is a modification of the Reid potential. Arguments are given that the baryons will not form a crystal lattice. The actual calculations were done using Pandharipande's method. The particles present at high density certainly include nucleons, Λ and Σ. The presence of Δ is questionable but that of π is likely. Results are given for the concentration of various species. With the more likely assumption about interactions, the concentration of each permissible species of particle is about equal at ϱ = 1016 g cm−3. The relation between energy and density is nearly independent of the assumptions on the species permitted and the energy is about 3 GeV particle−1 at ϱ = 1016 g cm−3. The relation between pressure and energy density is given, which yields a sound velocity equal to c at a few times 1015 g cm−3. Results for the structure of neutron stars are given. The maximum mass is about 2 solar masses and the maximum moment of inertia 1045 g cm2.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 53: Physics of Dense Matter , 1974 , pp. 27 - 46
Copyright
Copyright © Reidel 1974 

References

Aichelburg, P. C., Ecker, G., and Sexl, R. U.: 1971, Nuovo Cimento 2B, 63.Google Scholar
Anderson, P. W. and Palmer, R. G.: 1971, Nature Phys. Sci. 231, 145.Google Scholar
Baym, G., Bethe, H. A., and Pethick, C. J.: 1971a, Nucl. Phys. A175, 225.Google Scholar
Baym, G., Pethick, C. J., and Sutherland, P.: 1971b, Astrophys. J. 170, 299.CrossRefGoogle Scholar
Bethe, H. A.: 1971, Ann. Rev. Nucl. Sci. 21, 93.CrossRefGoogle Scholar
Calogero, F. and Simonov, Yu. A.: 1969, Nuovo Cimento 64B, 337.Google Scholar
Calogero, F. and Simonov, Yu. A.: 1970a, Phys. Rev. Letters 25, 881.Google Scholar
Calogero, F. and Simonov, Yu. A.: 1970b, Nuovo Cimento Letters 4, 219.Google Scholar
Calogero, F., Simonov, Yu. A., and Surkov, E. L.: 1972, Phys. Rev. C5, 1493.Google Scholar
Chemtob, M., Durso, J. W., and Riska, D. O.: 1971, Phys. Letters 36B, 313.Google Scholar
Coldwell, R. L.: 1972, Phys. Rev. D5, 1273.Google Scholar
Leung, Y. C. and Wang, C. G.: 1971, Astrophys. J. 170, 499.Google Scholar
Pandharipande, V. R.: 1971a, Nucl. Phys. A178, 123.Google Scholar
Pandharipande, V. R.: 1971b, Nucl. Phys. A174, 641.Google Scholar
Reid, R. V. Jr.: 1968, Ann. Phys. N.Y. 50, 411.CrossRefGoogle Scholar
Sawyer, R. F.: 1972a, Astrophys. J. 176, 531.Google Scholar
Sawyer, R. F.: 1972b, Phys. Rev. Letters 29, 382.Google Scholar
Scalapino, D. J.: 1972, Phys. Rev. Letters 29, 386.CrossRefGoogle Scholar
Siemens, P. and Pandharipande, V. R.: 1971, Nucl. Phys. A173, 561.Google Scholar
Wentzel, G.: 1949, Quantum Theory of Fields, Interscience Publ., New York.Google Scholar
Yang, C. H. and Clark, J. W.: 1971, Nucl. Phys. A174, 49.Google Scholar