The interacting neutron gas at high density and temperature

Details The interacting neutron gas at high density and temperature The interacting neutron gas at high density and temperature

Mar 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...212..807b&link_type=abstract

Astrophysical Journal, Part 1, vol. 212, Mar. 15, 1977, p. 807-815. Research supported by the Ministere des Affaires Culturelle

Astronomy and Astrophysics

Astrophysics

25

Astrophysics, Equations Of State, Gas Density, High Temperature Gases, Neutron Stars, Gas Expansion, Nuclear Potential, Stellar Evolution, Supernovae, Tables (Data)

Scientific paper

A general many-body formalism developed for the treatment of interacting fermions at finite temperature is applied to compute the interaction energy of a partially degenerate neutron gas. The grand potential is expressed in terms of an independent-particle component and a linked-cluster expansion analogous to a certain zero-temperature expansion, and the isospin triplet soft-core Reid (1968) nuclear potential is adopted. The equations of state obtained for the interacting neutron gas and for the noninteracting gas are plotted for densities ranging from 2 by 10 to the 10th power to 10 to the 14th power g/cu cm and temperatures up to approximately 300 billion K.

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