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A neutron star is so dense that one teaspoon (5 milliliters) of its material would have a mass over 5.5 × 10 12 kg, about 900 times the mass of the Great Pyramid of Giza. [b] The entire mass of the Earth at neutron star density would fit into a sphere 305 m in diameter, about the size of the Arecibo Telescope.
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.
PSR J0952–0607 is a massive millisecond pulsar in a binary system, located between 3,200–5,700 light-years (970–1,740 pc) from Earth in the constellation Sextans. [6] It holds the record for being the most massive neutron star known as of 2022, with a mass 2.35 ± 0.17 times that of the Sun—potentially close to the Tolman–Oppenheimer–Volkoff mass upper limit for neutron stars.
The equations of motion are contained in the continuity equation of the stress–energy tensor: =, where is the covariant derivative. [5] For a perfect fluid, = (+) +. Here is the total mass-energy density (including both rest mass and internal energy density) of the fluid, is the fluid pressure, is the four-velocity of the fluid, and is the metric tensor. [2]
Neutron degeneracy is analogous to electron degeneracy and exists in neutron stars, which are partially supported by the pressure from a degenerate neutron gas. [8] Neutron stars are formed either directly from the supernova of stars with masses between 10 and 25 M ☉ (solar masses), or by white dwarfs acquiring a mass in excess of the ...
A neutron star would approximate the most dense system capable of matter-antimatter annihilation. A black hole, although denser than a neutron star, does not have an equivalent anti-particle form, but would offer the same 100% conversion rate of mass to energy in the form of Hawking radiation. Even in the case of relatively small black holes ...
[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.
Oppenheimer and Snyder did, however, refer to an earlier article by Oppenheimer and Volkoff on neutron stars, improving upon the work of Lev Davidovich Landau. [7] Previously, and in the same year, Oppenheimer and three colleagues, Richard Tolman , Robert Serber , and George Volkoff , had investigated the stability of neutron stars, obtaining ...