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As early as 1934 Baade and Zwicky correctly predicted the birth of the strange objects neutron stars in supernova explosions (BAADE, ZWICKY, 1934). The first models were calculated by OPPENHEIMER, VOLKOFF (1939), and the stage was then left for the next 28 years to particle physicists who struggled with the problem of matter at extreme densities (a struggle not yet finished). Radio astronomers accidentally found the first pulsar in 1967; it was interpreted soon after as a rapidly rotating neutron star (GOLD, 1968). Everything is extreme with neutron stars, their interior state (simulating a huge nucleus), the velocity of sound (not far from c), their rotation (frequencies 1… 1000 Hz), and their magnetic fields (up to 1012 gauss). One is far from really understanding them. So we content ourselves here with a few remarks on the state of matter and the resulting models.
KeywordsNeutron Star Maximum Mass Hydrostatic Equilibrium Mass Defect Newtonian Limit
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