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The title and abstract read: On Massive Neutron Cores J. R. OPPENHEIMER AND G. M. VOLKOFF Department of Physics, University of California, Berkeley, California (Received January 3, 1939) It has been suggested that, when the pressure within stellar matter becomes high enough, a new phase consisting of neutrons will be formed. In this paper we study the gravitational equilibrium of masses of neutrons, using the equation of state for a cold Fermi gas, and general relativity. For masses under M☉/3 only one equilibrium solution exists, which is approximately described by the non-relativistic Fermi equation of state and Newtonian gravitational theory. For masses M☉/3 < 3M☉/4 two solutions exist, one stable and quasi-Newtonian, one more condensed, and unstable. For masses greater than 3M☉/4 there are no static equilibrium solutions.

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The title and abstract read: On Massive Neutron Cores J. R. OPPENHEIMER AND G. M. VOLKOFF Department of Physics, University of California, Berkeley, California (Received January 3, 1939) It has been suggested that, when the pressure within stellar matter becomes high enough, a new phase consisting of neutrons will be formed. In this paper we study the gravitational equilibrium of masses of neutrons, using the equation of state for a cold Fermi gas, and general relativity. For masses under M☉/3 only one equilibrium solution exists, which is approximately described by the non-relativistic Fermi equation of state and Newtonian gravitational theory. For masses M☉/3 < 3M☉/4 two solutions exist, one stable and quasi-Newtonian, one more condensed, and unstable. For masses greater than 3M☉/4 there are no static equilibrium solutions.
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Robert McNees (mcnees@mastodon.social)'s status on Saturday, 22-Apr-2023 23:51:24 UTC Robert McNees
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This was followed in 1939 by a paper with Volkoff, published alongside work by Tolman. They modeled neutron stars by applying Tolman's self-gravitating perfect fluid solution of general relativity to a degenerate neutron gas.
The Oppenheimer-Volkoff paper was the first serious treatment of the structure of neutron stars, which had been proposed by Baade and Zwicky five or six years earlier. It set the stage for realistic relativistic models of stellar structure.
Ref: https://link.aps.org/doi/10.1103/PhysRev.55.374

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