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Understanding the nature of the matter present in the various layers of neutron stars, and the phase transitions that occur at the boundaries of the layers is a major unsolved problem in fundamental physics. The neutron star equation of state encodes information about the structure of a neutron star and thus tells us how matter behaves at the ...
Since this equation of state is not realistic for a neutron star, this limiting mass is likewise incorrect. Using gravitational wave observations from binary neutron star mergers (like GW170817) and the subsequent information from electromagnetic radiation , the data suggest that the maximum mass limit is close to 2.17 solar masses.
[7] And indeed, the most massive neutron star detected so far, PSR J0952–0607, is estimated to be much heavier than Oppenheimer and Volkoff's TOV limit at 2.35 ± 0.17 M ☉. [8] [9] More realistic models of neutron stars that include baryon strong force repulsion predict a neutron star mass limit of 2.2 to 2.9 M ☉.
The equations of state for the various proposed forms of quark-degenerate matter vary widely, and are usually also poorly defined, due to the difficulty of modelling strong force interactions. Quark-degenerate matter may occur in the cores of neutron stars, depending on the equations of state of neutron-degenerate matter.
Cross-section of neutron star In astrophysics and nuclear physics , nuclear pasta is a theoretical type of degenerate matter that is postulated to exist within the crusts of neutron stars . If it exists, nuclear pasta would be the strongest material in the universe. [ 1 ]
The boundaries of this valley are the neutron drip line on the neutron-rich side, and the proton drip line on the proton-rich side. [2] These limits exist because of particle decay, whereby an exothermic nuclear transition can occur by the emission of one or more nucleons (not to be confused with particle decay in particle physics).
Planets and stars have radial density gradients from their lower density surfaces to their much denser compressed cores. Degenerate matter objects (white dwarfs; neutron star pulsars) have radial density gradients plus relativistic corrections. Neutron star relativistic equations of state include a graph of radius vs. mass for various models. [6]
[9] [10] In a neutron star, pressure rises from zero (at the surface) to an unknown large value in the center. Methods capable of treating finite regions have been applied to stars and to atomic nuclei. [11] [12] One such model for finite nuclei is the liquid drop model, which includes surface effects and Coulomb interactions.