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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.
Its size is approximately 10 −15 meters and its density 10 18 kg/m 3. The descriptive term nuclear density is also applied to situations where similarly high densities occur, such as within neutron stars. Using deep inelastic scattering, it has been estimated that the "size" of an electron, if it is not a point particle, must be less than 10 ...
An overview of ranges of mass. To help compare different orders of magnitude, the following lists describe various mass levels between 10 −67 kg and 10 52 kg. The least massive thing listed here is a graviton, and the most massive thing is the observable universe.
See Weight for detail of mass/weight distinction and conversion. Avoirdupois is a system of mass based on a pound of 16 ounces, while Troy weight is the system of mass where 12 troy ounces equals one troy pound. The symbol g 0 is used to denote standard gravity in order to avoid confusion with the (upright) g symbol for gram.
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 ...
Densities are in terms of ρ 0 the saturation nuclear matter density, where nucleons begin to touch. Patterned after Haensel et al. , [ 7 ] page 12 Some authors use "nuclear matter" in a broader sense, and refer to the model described above as "infinite nuclear matter", [ 1 ] and consider it as a "toy model", a testing ground for analytical ...
Name Mass (M ☉) Distance ()Companion class Mass determination method Notes Refs. PSR J1748-2021B: 2.548 +0.047 −0.078: 27,700: D: Rate of advance of periastron.: In globular cluster NGC 6440.
As we go deeper into the neutron star the free neutron density increases, and as the Fermi momentum increases with increasing density, the Fermi energy increases, so that energy levels lower than the top level reach neutron drip and more and more neutrons drip out of nuclei so that we get nuclei in a neutron fluid. Eventually all the neutrons ...