Neutron degeneracy pressure, which is a stellar application of the Pauli Exclusion Principle, is actually "stronger" than electron degeneracy pressure, which is also a stellar application of the aforementioned principle because neutrons are more massive and have shorter wavelengths and more closely space energy levels than electrons.
Fundamentally, they are the same ...
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A neutron star is created when a star is around eight to ten times Earth's sun burns out. The outward pressure generated by fusion reduces rapidly, allowing gravity to pull the star in on itself and start up a supernova, where the outer layers of a star’s atmosphere get blown into space.
Neutron stars actually deploys a lot of gravity for objects as small as they are, ...
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A quark star is really an intermediate stage in between neutron stars and black holes. It has too much mass at its core for the neutrons to hold their structure, but it doesn’t have enough to fully collapse into a black hole. The underlying quarks that form the neutrons are further compressed in these objects.
A quark star is also a hypothetical type of compact exotic star, ...
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With only 7.5% of the sun’s mass, the coolest possible red dwarf star will still have a temperature of about 2,300 C, less than the melting point of carbon. However, if a star doesn’t have enough mass to ignite fusion, it becomes a brown dwarf, heated by the mechanical action of all that mass compressing inward. Average brown dwarfs will be about 1,700 C, which is still ...
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The maximum mass of a stable white dwarf star is called the Chandrasekhar limit . The currently accepted value of the Chandrasekhar limit is about 1.4 solar masses. The limit was named after Subrahmanyan Chandrasekhar, the Indian astrophysicist who, at 20 years old, improved upon the calculation’s accuracy in 1930 by calculating the limit for a polytrope model of a star in ...
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Before quantum mechanics were discovered, physicists knew of no force capable of supporting any star against such gravitational pressure. Quantum mechanics, though, suggested a new way for a star to hold itself up against the force of gravity. The rules of quantum mechanics note that no two electrons can be in the exact same state. Inside an dense star, this means some electrons are ...
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A dwarf star generally refers to any main-sequence star, a star of luminosity class V: main-sequence stars (dwarfs). Red dwarfs are low-mass main-sequence stars; yellow dwarfs are main-sequence (dwarf) stars with masses comparable to that of the sun and orange dwarfs are K-type main-sequence stars.
A blue dwarf is a hypothesized class of very-low-mass stars that increase in ...
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Electron degeneracy pressure is an exact materialization of the more general phenomenon of quantum degeneracy pressure. The Pauli Exclusion Principle disallows two identical half-integer spin particles, including electrons and all other fermions, from concurrently occupying the same quantum state. The result is an emergent pressure against compression of matter into smaller volumes of ...
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Yes and no. It's a fact that both black holes and neutron stars are product of a dying star. When a star dies, it spent all of its energy and then collapses. However, their difference lies on their parent star. It's best to compare black holes and neutron stars with the mass of the sun. If a star similar to that of the sun's mass dies, it will form a white dwarf.
When a dying ...
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After a supernova explosion, a number of things that can be left behind, because the star’s center, or core, collapses in less than a second. The star’s outer layers of the star are blown off in the explosion, 3 a contracting core of the star after the supernova. The shock waves and material that fly out from the supernova can cause the formation of new ...
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