Abstract
ASSUMING that pulsars are spinning, contracted stellar objects of enormous mass, we can divide the interior of a pulsar into three distinct density regions. Region 1 has a density below 5 × 1011 g cm−3, region 2 has a density from 5 × 1011 to 1015 g cm−3, and region 3 has a density > 1015 g cm−3. In region 1, the pressure is generated by an electron gas obeying the laws of atomic physics and the semi-empirical nuclear mass formula plays an important part in the equation of state. The unsolved problems will not require new methods, but only better accuracy.
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LEUNG, Y., WANG, C. The Limiting Mass of a Neutron Star. Nature Physical Science 233, 99–100 (1971). https://doi.org/10.1038/physci233099a0
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DOI: https://doi.org/10.1038/physci233099a0
