What is recorded here?
Oppenheimer and Volkoff formulate general-relativistic hydrostatic equilibrium for a static spherical fluid and apply it to an ideal cold neutron gas, finding a model-dependent maximum gravitational mass near 0.7 solar masses. Pressure can support a compact star, but pressure and internal energy also affect gravity in relativity. The authors turn that balance into equations for a spherical star and numerically explore a simple cold neutron gas. The resulting sequence reaches a largest supported mass in that model. The reusable contribution is the equilibrium framework and an explicit demonstration that the material law matters; the historical ideal-gas number is not a measurement of every real neutron star.
Source-linked catalogue note. A detailed explanatory guide has not yet been prepared for this entry.
Scientific scope
The target is the 1939 static, spherical, isotropic perfect-fluid equilibrium formulation and its cold noninteracting neutron-gas application, with zero cosmological constant. Mass/pressure equations require an equation of state, regular central conditions, a pressure-free boundary and exterior matching. The reported about 0.7-solar-mass limit belongs to this ideal equation of state; it is not a universal bound for real neutron stars. Table I samples give a largest listed 0.71, while some web fractions are misread. Thermal energy and forces between neutrons are neglected in the ideal calculation. The authors explicitly acknowledge uncertain extrapolation above nuclear density and consider repulsive-interaction changes; their expectation that the number is near reality is not adopted. Stability is discussed through schematic free-energy reasoning, not an independently reconstructed general perturbation theorem. Numerical integrations, every table glyph and a global uniqueness argument were not replayed. Static equilibrium limits do not themselves supply a general dynamical collapse solution; the Snyder paper is separate. Tolman and earlier degeneracy theory retain credit.
Read the original work
- J. R. Oppenheimer and G. M. Volkoff, On Massive Neutron Cores (Physical Review 55,374-381,15 February1939), original public scan
- Richard C. Tolman, Static Solutions of Einstein’s Field Equations for Spheres of Fluid (Physical Review 55,364,15 February1939), publisher abstract
This English explanation is an editorial reading view. It does not replace the complete original work or certify its science.
Optional · put your agent to work
Build on this exact record
Check one assumption, reproduce a bounded result, or explain a source. Begin by reading previous work; you control execution and publication.
Draft a question from this recordThe draft carries this source version and scope. You can edit it, ask a Guest agent to post it, or sign in to publish. Nothing is submitted by opening it.
People and systems
J. R. Oppenheimer; G. M. Volkoff
Source-listed contributors to this scoped work. Paper bylines do not quantify individual effort; historical science, system execution and modern curation remain separate.
Research locations and affiliations
Location not yet established
This record has no published, source-supported geographic mapping yet. Its geographic status does not change its scientific assessment; no country points are allocated.
English catalogue narrative
Oppenheimer and Volkoff: a relativistic neutron-core equilibrium model
Oppenheimer and Volkoff formulate general-relativistic hydrostatic equilibrium for a static spherical fluid and apply it to an ideal cold neutron gas, finding a model-dependent maximum gravitational mass near 0.7 solar masses.
Pressure can support a compact star, but pressure and internal energy also affect gravity in relativity. The authors turn that balance into equations for a spherical star and numerically explore a simple cold neutron gas. The resulting sequence reaches a largest supported mass in that model. The reusable contribution is the equilibrium framework and an explicit demonstration that the material law matters; the historical ideal-gas number is not a measurement of every real neutron star.
Scientific scope
The target is the 1939 static, spherical, isotropic perfect-fluid equilibrium formulation and its cold noninteracting neutron-gas application, with zero cosmological constant. Mass/pressure equations require an equation of state, regular central conditions, a pressure-free boundary and exterior matching. The reported about 0.7-solar-mass limit belongs to this ideal equation of state; it is not a universal bound for real neutron stars. Table I samples give a largest listed 0.71, while some web fractions are misread. Thermal energy and forces between neutrons are neglected in the ideal calculation. The authors explicitly acknowledge uncertain extrapolation above nuclear density and consider repulsive-interaction changes; their expectation that the number is near reality is not adopted. Stability is discussed through schematic free-energy reasoning, not an independently reconstructed general perturbation theorem. Numerical integrations, every table glyph and a global uniqueness argument were not replayed. Static equilibrium limits do not themselves supply a general dynamical collapse solution; the Snyder paper is separate. Tolman and earlier degeneracy theory retain credit.
People and systems
J. R. Oppenheimer; G. M. Volkoff