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Topic: Neutron degeneracy pressure

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	Degenerate matter - Wikipedia, the free encyclopedia
		The pressure maintained by a body of degenerate matter is called the degeneracy pressure, and arises because the Pauli principle forbids the constituent particles from occupying identical quantum states.
		As protons and electrons occur in roughly equal numbers in most forms of matter, proton degeneracy is usually modelled as a correction to the equations of state of electron-degenerate matter, as opposed to the dominant source of degeneracy pressure (which would require proton-degenerate matter that was free of electrons).
		Neutron degeneracy is analogous to electron degeneracy and is demonstrated in neutron stars, which are supported by the pressure from a degenerate neutron gas.
	en.wikipedia.org /wiki/Degeneracy_pressure (1808 words)

	Physics 408 Exam 1
		Neutron degeneracy pressure arises when neutrons are so close that their quantum states begin to overlap.
		The combined pressure from neutron degeneracy pressure and the strong nuclear force prevent further gravitational collapse of a neutron star if the remaining supernova core (neutron star) is less than 2-3 solar masses.
		Neutron stars rotate more rapidly than ordinary stars because the rate of spin increased as the stars collapsed to a small size due to conservation of angular momentum (like the ice skater who pulls her mass in closer to her rotation axis and spins faster or my demonstration in class on the stool using masses).
	www.calpoly.edu /~rechols/6edastro102/astro112ch23sol.html (470 words)

	Neutron stars and pulsars
		When it reaches the threshold of energy necessary to force the combining of electrons and protons to form neutrons, the electron degeneracy limit has been passed and the collapse continues until it is stopped by neutron degeneracy.
		This neutron degeneracy radius is about 20 km for a solar mass, compared to about earth size for a solar mass white dwarf.
		Neutron degeneracy is a stellar application of the Pauli Exclusion Principle, as is electron degeneracy.
	hyperphysics.phy-astr.gsu.edu /hbase/astro/pulsar.html (1094 words)

	Pressure, Degeneracy, Exchange Interaction, Neutron Stars, Atoms, Etc.
		The pressure in a degenerate Fermi fluid is higher than it would be in a non-degenerate or non-fermionic fluid under comparable conditions of density and temperature.
		Pressure might have been on the list in the early 19th century, but it was stricken when people realized it can be fully explained in terms of the other items on the list, via “kinetic theory”.
		It is evident from equation 4 that for a nonrelativistic gas, the energy (and hence pressure) depend inversely on the mass of the particles.
	www.av8n.com /physics/degeneracy.htm (2811 words)

	Neutron Degeneracy (Site not responding. Last check: 2007-10-23)
		When neutrons are packed together, as they are in a neutron star, the number of available low energy states is too small and many neutrons are forced into high energy states.
		Because the pressure arises from this quantum mechanical effect, it is insensitive to temperature, i.e., the pressure doesn't go down as the star cools.
		Similar to electron degeneracy pressure but, because the neutron is much more massive than the electron, neutron degeneracy pressure is much larger and can support stars more massive than the Chandrasekhar mass limit.
	www.astro.virginia.edu /~jh8h/glossary/neutrondegen.htm (121 words)

	Digital Demo Room Stellar Structure and Evolution Tutorial
		If the core's mass is less than about 3 solar masses, the core's neutron degeneracy pressure continues to counteract the inward pull of gravity, stabilizing it into a neutron star.
		Neutron degeneracy pressure occurs at much higher densities than electron degeneracy pressure, making neutron stars even denser than white dwarfs.
		Neutron stars are also dimmer than white dwarfs, putting them even lower on the HR diagram, but still in the same general region below the main sequence.
	rainman.astro.uiuc.edu /ddr/stellar/evolution.html (1612 words)

	sciforums.com - Degeneracy pressure and Fermions
		11-03-99 11:17 PM Degeneracy pressure for non-relativistic electrons is given as p~1/((d^2)(Me)) where d is the mean inter electron distance and Me is electron mass, a similar equation is given for neutron degeneracy pressure p~1/((d^2)(Mn)).
		Barring situations where d^2 is sufficient to cause Mf to no longer exist, of course (as in the situation in neutron stars, where the electrons are absorbed into the protons: e+p=n+v).
		I see no good reason why a single general equation couldn't be applied to the degeneracy pressures of all Fermions.
	www.sciforums.com /printthread.php?t=246 (293 words)

	Neutron stars
		The star keeps on collapsing until a neutron degeneracy pressure sets in, due to the fact that neutrons also obey the Pauli exclusion principle.
		During the collapse it can happen that the outer envelope of the star collides with the inner neutron core, which sets up shock wave that results in the outer layer of the star exploding.
		A pulsar is a neutron star that emits radio waves at regular intervals, which are the result of fast moving particles being accelerated by the intense magnetic fields present.
	theory.uwinnipeg.ca /mod_tech/node211.html (307 words)

	Archive of Astronomy Questions and Answers (Site not responding. Last check: 2007-10-23)
		These stellar cinders are supported by electron degeneracy pressure (white dwarfs) and neutron degeneracy pressure (neutron stars) which are two very different mechanisms.
		Even though the pressure comes from the light-weight electrons in white dwarfs, the mass of the body is still determined by the number of protons and neutrons.
		The maximum mass of a neutron star is, however, a bit more complicated that what is suggested by the Oppenheimer-Volkov limit and depends on the details of the rotation of the neutron star, and the specific 'equation of state' used to describe matter at densities of 10^13 grams/cc or higher.
	www.astronomycafe.net /qadir/q2228.html (254 words)

	Curious About Astronomy: What process would bring about a quark star?
		A neutron star is the remnant core of a massive, normal star after it has undergone a supernova explosion.
		It consists mostly of neutrons and is held up against gravitational collapse by "neutron degeneracy pressure" - this is a quantum mechanical effect that resists two neutrons being in the same place and therefore tends to push them apart when they get too close together.
		If the remant core of the original star is massive enough (greater than a few times the mass of the sun) then the force of gravity will be stronger than the force of neutron degeneracy pressure and so the star will continue to collapse right on past the neutron star stage.
	curious.astro.cornell.edu /question.php?number=445 (315 words)

	What is a Pulsar?
		Again, we have two opposing forces, but this time they are gravity and neutron degeneracy pressure: protons and electrons have been melded together into neutrons, and neutron degeneracy pressure is much greater than electron degeneracy pressure.
		Equilibrium is eventually reached and a stable neutron star is created (calling it a star may seem deceptive, since we just told you that its life as a star was over, but astronomers are notoriously flexible with the English language).
		Neutron stars, unlike normal stars, tend to rotate at incredibly high speeds: they will go through one full rotation in a fraction of a second, while it takes the sun (a quite ordinary sort of star) about a month.
	www.oberlin.edu /physics/stinebring/research/pulsar.html (591 words)

	NRL - Timing Studies of X-ray Binary Orbits
		This pressure is the result of the fact that electrons are fermions and are thus subject to the Pauli Exclusion Principle, which prevents more than two fermions from occupying the same volume.
		The collapse of the most massive stars cannot even be stopped by neutron degeneracy pressure and thus they continue collapsing all the way to a fl hole, an object so compact and massive that even light cannot escape.
		A binary period of at least 6 days is required for the neutron star's orbit to be outside the surface of the companion star so a measurement of the orbital parameters of the system was of considerable interest.
	www.nrl.navy.mil /content.php?P=03REVIEW79-2 (1118 words)

	Neutron star
		Neutron stars are stars that result from the implosion of a very heavy star.
		As for the core, it may just continue to be neutrons as well, but it might be that their is further degradation of neutrons into a type of quark matter.
		Protons and neutrons are baryons, and electrons and neutrinos are leptons, and their numbers are conserved too.
	www.physicsforums.com /showthread.php?t=83055 (1646 words)

	Chapter 15: The Bizarre Stellar Graveyard (Site not responding. Last check: 2007-10-23)
		Neutron stars are held up by neutron degeneracy pressure.
		Neutron stars in a close binary system may also steal gas from their neighbors.
		But since other processes can also emit X-rays (like binary neutron stars), to qualify as a possible fl hole, the object must also be massive enough.
	www.accd.edu /sac/astronom/astr1370/bennett15.htm (976 words)

	[No title]
		Degeneracy pressure is when the electrons (or neutrons) are so closely packed together that they cannot get any closer, due to the exclusion principle.
		The core contraction continues until it reaches electron degeneracy, and electron degeneracy pressure is then supporting the core.
		Because of the high temperatures, the thermal pressure increases, causing the expansion of the envelope of the star.
	www.astro.lsa.umich.edu /~rstanek/w02/hmwk7.html (882 words)

	Science Partners Science Fair for Grownups: L. Munoz-Franco poster
		Degeneracy pressure is not originated by using a fuel source.
		Neutron star is very hot, more than 100,000 K for most of its lifetime, so this sounds promising...
		Another way to see a neutron star is if it is one member of a binary, in which case the gravity of the neutron star can strip gas off its companion.
	astro.uchicago.edu /home/web/lucia/partners/starsdie.html (1424 words)

	ASTR 201 3 March 2003 (Site not responding. Last check: 2007-10-23)
		They end in a planetary nebula (the remnants of the envelope and atmosphere) and a white dwarf (the remnant of the core, supported by the balance between gravity and electron degeneracy pressure).
		The core ultimately becomes supported by neutron degeneracy pressure, and the result is a neutron star.
		High mass stars (greater than about 12 solar masses) undergo similar evolution as the intermediate mass stars, except that gravity overcomes neutron degeneracy pressure and the core collapses to a singularity, or fl hole.
	www.eg.bucknell.edu /physics/ASTR201/03mar03.htm (440 words)

	ASTRO-1 Lecture 04
		The neutrons stay where they are formed but the neutrinos escape, carrying away energy.
		, neutron degeneracy pressure cannot support the neutron star against gravity; nothing will stop the collapse and the core will contract to a single point of infinite density (a singularity): this is a fl hole.
		That fact alone suggests that one of the two stars is a compact object, specifically a neutron star or a fl hole.
	www.astro.psu.edu /users/mce/A1/lect16.html (1897 words)

	Black Holes and Neutron Stars (Site not responding. Last check: 2007-10-23)
		Even a neutron star rotating at that rate is near the limit of breaking apart.
		The rapid rotation is due to the spinning up of the neutron star due to the infall of matter from a companion.
		The equations of GR were confirmed by two astrophysicists who used them to explain the loss of energy due to gravitational radiation from a neutron star binary pair.
	www.astro.queensu.ca /~waugh/q2lecture13.html (3120 words)

	ast105review4fall2003
		E) Gravity is not able to overcome neutron degeneracy pressure.
		E) they are supported by electron degeneracy pressure.
		degeneracy of the core, the core will be compressed until it becomes a fl hole.
	www.physics.sfasu.edu /friedfeld/ast105/ast105review4fall2003.htm (1774 words)

	The Stellar Life Cycle: Black Hole (Site not responding. Last check: 2007-10-23)
		Neutron degeneracy pressure cannot support an object having mass greater than 2-3 solar masses.
		Sometimes not all the matter outside the 1.4 solar mass core gets blown away in the type II supernova.
		Once the neutron degeneracy pressure is overcome, there is no force that can halt the collapse.
	cse.ssl.berkeley.edu /bmendez/ay10/2000/cycle/blackhole.html (130 words)

	neutron stars and colour force
		If neutrons stay intact and get closer together than 10^-15 metres in a neutron star, would the exchange of mesons between neutrons stop and be replaced by the exchange of gluons, and would the gluons cause an attractive or repulsive force between neutrons?
		A repulsive force could stop the collapse of the neutron star in place of neutron degeneracy pressure.
		Under the high density assumption, the formula for classical graviational pressure may have to be replaced by the GR equivalent.
	www.physicsforums.com /showthread.php?p=295124 (996 words)

	Degeneracy Pressure (Site not responding. Last check: 2007-10-23)
		The Pauli Exclusion Principle in quantum mechanics forbids electrons (and all fermions with half integer spin including neutron) occupying the same state.
		This pressure is known as electron degeneracy pressure and it is the force that supports white dwarf stars against their own gravity.
		If the electrons disappear this way, the star collapses suddenly down to a size for which the degeneracy pressure of the neutrons stops the collapse (with quite a shock).
	universe-review.ca /R08-04-degeneracy.htm (318 words)

	The Chandrasekhar Limit (Site not responding. Last check: 2007-10-23)
		, it is no longer able to support itself by electron degeneracy pressure.
		This limit is called the Chandrasekhar limit, after the physicist who derived it in terms of fundamental constants.
		A white dwarf that exceeds this mass must continue its collapse until a new source of pressure, neutron degeneracy pressure, is able to stop the collapse.
	www.atnf.csiro.au /people/Tony.Wong/ay10b/evol/node5.html (465 words)

	[No title]
		White dwarfs are supported by electron degeneracy which occurs at a density of matter that is 10
		If the mass of the core exceeds 1.4 solar masses, electron degeneracy breaks and the core would collapse until its supported by neutron degeneracy which occurs at nuclear densities of 10
		Neutron degeneracy pressure would fail and nothing can stop its gravitational collapse.
	zebu.uoregon.edu /disted/ph122/lec18.html (1020 words)

	Chandra :: Resources :: Q&A: Supernova Remnants and Neutron Stars
		A white dwarf is supported by electron degeneracy pressure, a neutron star by neutron degeneracy pressure
		A neutron star has a stronger gravitational field -about 400,000 times
		Neutron stars have higher temperatures at birth, spin faster, and have stronger magnetic fields, among other things.
	chandra.harvard.edu /resources/faq/sources/snr/snr-16.html (98 words)

	Lives and Deaths of Stars
		How does electron degeneracy pressure keep the white dwarf from collapsing any further?
		How does neutron degeneracy pressure keep the neutron star from collapsing to a point at the center?
		What is the upper bound for the mass of a neutron star?
	www.astronomynotes.com /evolutn/s14.htm (299 words)

	ASTR 1025 Spring 2001: Study Guide for Quiz #4 (Site not responding. Last check: 2007-10-23)
		Alpha Particle; Electron/Neutron Degeneracy Pressure; Pauli Exclusion Principle; Triple-Alpha Reaction; Red Giant; Horizontal Branch Stars; Planetary Nebula; White Dwarf; Chandrasekhar limit; CNO Cycle; Alpha-Capture Reactions; Neutron Degeneracy Pressure; Supernova Type I and II; Supernova Remnant; Neutron Star; Pulsar; Angular Momentum Conservation; Synchrotron Radiation; Nova; Mass-Transfer Binary; Supernova Types I and II; X-ray Burster.
		Linear momentum = mass times velocity; angular momentum is proportional to mass times velocity times size.
		The steps in the triple-alpha reaction; the life stages of a one solar mass star; the life stages in a high mass star; why a neutron star is spinning fast; the `lighthouse model' of a pulsar; where different chemical elements are produced.
	www.etsu.edu /physics/bsmith/spring01/hw+q+s/study4.html (155 words)

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