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The abstract of Tolman’s paper reads: FEBRUARY 15, 1939 PHYSICAL REVIEW Static Solutions of Einstein's Field Equations for Spheres of Fluid RICHARD C. TOLMAN Norman Bridge Laboratory of Physics, California Institute of Technology, Pasadena, California (Received January 3, 1939) A method is developed for treating Einstein's field equations, applied to static spheres of Auid, in such a manner as to provide explicit solutions in terms of known analytic functions. A number of new solutions are thus obtained, and the properties of three of the new solutions are examined in detail. It is hoped that the investigation may be of some help in connection with studies of stellar structure. (See the accompanying article by Professor Oppenheimer and Mr. Volkoff.)

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The abstract of Tolman’s paper reads: FEBRUARY 15, 1939 PHYSICAL REVIEW Static Solutions of Einstein's Field Equations for Spheres of Fluid RICHARD C. TOLMAN Norman Bridge Laboratory of Physics, California Institute of Technology, Pasadena, California (Received January 3, 1939) A method is developed for treating Einstein's field equations, applied to static spheres of Auid, in such a manner as to provide explicit solutions in terms of known analytic functions. A number of new solutions are thus obtained, and the properties of three of the new solutions are examined in detail. It is hoped that the investigation may be of some help in connection with studies of stellar structure. (See the accompanying article by Professor Oppenheimer and Mr. Volkoff.)
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Robert McNees (mcnees@mastodon.social)'s status on Monday, 04-Mar-2024 16:36:19 UTC Robert McNees
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In the late 1930s, Tolman (remember him?) worked on astrophysical and cosmological solutions of Einstein's equations.
A 1939 paper, published alongside an article by Oppenheimer and Volkoff, considered static, spherical distributions of "perfect fluid" like radiation or dust.
An immediate application was modeling stellar structure. Oppenheimer and Volkoff's paper applied Tolman's solutions to a degenerate Fermi gas of neutrons that might exist at the core of a collapsed star.

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