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	Degenerate star - Wikipedia, the free encyclopedia
		A degenerate star is type of star which is composed of degenerate matter.
		It is the generic name of three types of stars, degenerate dwarf (commonly called white dwarf), neutron star and quark star.
		A star like this is composed of electron degenerate matter, supported against gravity only by the resistance of electrons to being squeezed into the same energy state around the nucleus (as described by the pauli exclusion principle).
	en.wikipedia.org /wiki/Degenerate_star (422 words)

	degenerate star (Site not responding. Last check: 2007-09-08)
		A degenerate star is type of star which is held up against gravity by the pressure of degenerate matter.
		If the matter consists of degenerate electrons, the degenerate star is called a degenerate dwarf or more commonly a white dwarf.
		If the matter consists of quarks, the degenerate star is called a quark star or more general a strange star.
	www.yourencyclopedia.net /Degenerate_star (320 words)

	Degenerate dwarf -- Facts, Info, and Encyclopedia article (Site not responding. Last check: 2007-09-08)
		A Degenerate dwarf is type of ((astronomy) a celestial body of hot gases that radiates energy derived from thermonuclear reactions in the interior) star, an alternative name for what is commonly called a (A faint star of enormous density) White dwarf (see this reference for a more complete article).
		In degenerate stars, the weight of the star is counterbalanced by the pressure of (additional info and facts about degenerate matter) degenerate matter, which is, in the case of a Degenerate dwarf supplied by degenerate electrons (electrons at such high density that quantum mechanical effects are dominant).
		The internal structure of degenerate stars in general, is therefore decoupled from the thermal structure.
	www.absoluteastronomy.com /encyclopedia/d/de/degenerate_dwarf.htm (287 words)

	Chapters 10 Review Question Answers (Site not responding. Last check: 2007-09-08)
		Degenerate matter is difficult to compress because nearly all of the energy levels (states) available to the electrons are filled.
		Red dwarfs, because of their small mass, cannot squeeze their cores sufficiently under their own weight to reach a temperature of 100 million K and ignite helium fusion which is necessary to cause the outer layers to expand to become a giant.
		Equations predict that the radius of a white dwarf is inversely proportional to its mass.
	www.snc.edu /physics/takahashi/AstronomyF05/Horizons/Chapter10/Ch10RevAns.html (1680 words)

	ch16
		For example, the analysis of the HEAO observations of the degenerate dwarf star AM Hercules shows that the mass of the star is about 70 percent that of the Sun, and the radius is about one-hundredth that of the Sun.
		As the gas is drawn near the surface of the degenerate dwarf, it falls ever faster because of the increasingly strong gravitational forces.
		The studies of the X-ray pulses from degenerate dwarf sources are just beginning, but with the data accumulated by the X-ray "eyes" of the HEAO instruments, we may eventually be able to "see," albeit indirectly, inside a degenerate dwarf.
	history.nasa.gov /SP-466/ch16.htm (1195 words)

	Chapter 10 Review Questions (Site not responding. Last check: 2007-09-08)
		Degenerate matter is difficult to compress because nearly all of the energy levels available to the electrons are filled.
		Therefore, since in a degenerate gas it is extremely difficult to change the energies of the electrons that compose the gas, and to compress the gas we must change the energies of the electrons, it is extremely difficult to compress the gas.
		Degenerate matter is difficult to compress because all of the low energy levels for the electrons are full.
	www.goshen.edu /nasc/NaSc200/ReviewQuestions/ch10review.html (814 words)

	White Dwarfs
		Since a white dwarf has no way to keep itself hot unless it is accreting matter from a nearby star (see Cataclysmic Variables), it cools down over the course of the next billion years or so.
		Because a white dwarf is no longer able to create internal pressure, gravity unopposedly crushes it down until even the very electrons that make up a white dwarf's atoms are mashed together.
		Degenerate matter has other unusual properties; for example, the more massive a white dwarf is, the smaller it is! This is because the more mass a white dwarf has, the more its electrons must squeeze together to maintain enough outward pressure to support the extra mass.
	imagine.gsfc.nasa.gov /docs/science/know_l2/dwarfs.html (765 words)

	The Astrophysics Spectator: Stars
		What separates a star from a brown dwarf or a gaseous planet is that the star passes through a phase of hydrogen fusion.
		The brown dwarf, despite undergoing a period of deuterium fusion, never approaches a star in brightness, and never changes it composition significantly from the composition of a Jupiter; once it depletes its deuterium, it behaves as a Jupiter.
		If the companion star is a degenerate dwarf, then the two stars eventually merge when the system loses enough energy through gravitational radiation.
	www.astrophysicsspectator.com /background/survey/galactic/stars.html (1469 words)

	Science News: Extremely magnetic degenerate dwarf. (white dwa... @ HighBeam Research (Site not responding. Last check: 2007-09-08)
		These white dwarfs do not lurk in dark alleys; they are a class of stars found in the distant reaches of our galaxy.
		One instance of such behavior is the almost unbelievable magnetic field of 700 million gauss (MG), recently found in the white dwarf PG 1031+234 by a group of astronomers led by Gary D. Schmidt of the University of Arizona's Steward Observatory in Tucson.
		In other words, it pays to be degenerate, but even among magnetic white dwarfs, where conditions are extreme, fields tend to run no higher than tens of millions of gauss.
	www.highbeam.com /library/doc0.asp?DOCID=1G1:4211084&refid=ip_encyclopedia_hf (725 words)

	Stellar Lives (Site not responding. Last check: 2007-09-08)
		Degenerate gas is still a gas, but it has the consistency of a solid.
		The matter in a white dwarf is degenerate matter.
		A white dwarf is supported, not by energy flowing outward, but by the refusal of its electrons to pack themselves into a smaller volume.
	www.goshen.edu /nasc/NaSc200/Notes/StarLives/starlife.html (5673 words)

	Meadhall of the Comitatus :: View topic - Degenerates (Site not responding. Last check: 2007-09-08)
		Degenerate elves stand between 4 and a half to five and a half feet tall.
		Degenerate dwarves stand between 4 and a half and 5 feet tall.
		Degenerate Gnomes are usually 2 to 3 feet tall and have skin that has a yellow or green caste to it.
	thecomitatus.com /archives/degenerates.htm (1487 words)

	Chapter 10 Summary (Site not responding. Last check: 2007-09-08)
		The electrons in degenerate matter are packed so closely together that nearly all of the “rungs” of their “energy ladder” are occupied (Figure 10-4); electrons cannot easily change their energy due to Pauli Exclusion Principle, which says that no two identical electrons can occupy the same energy level.
		Because increasing the temperature of degenerate matter increases the energy of the “heavy-weight” atomic nuclei but not of the electrons, the pressure does not increase with the rising temperature: no pressure-temperature thermostat for degenerate matter.
		The white dwarf accumulates an outer layer of hydrogen-rich gas that burns explosively in a thermonuclear runaway in the surface layers of the white dwarf.
	www.snc.edu /physics/takahashi/AstronomyS05/Horizons/Chapter10/Ch10Sum.html (2074 words)

	Degenerate dwarf (Site not responding. Last check: 2007-09-08)
		A Degenerate dwarf is type of star, an alternative name for what is commonly called a White dwarf (see this reference for a more complete article).
		In degenerate stars, the weight of the star is counterbalanced by the pressure of degenerate matter, which is, in the case of a Degenerate dwarf supplied by degenerate electrons (electrons at such high density that quantum mechanical effects are dominant).
		To avoid such oxymoronic names as a 'red white dwarf' (which is an entirely different object than a red dwarf), the name 'Degenerate dwarf' is preferred above 'White dwarf'.
	www.sciencedaily.com /encyclopedia/degenerate_dwarf (273 words)

	Supernova
		If the matter is deposited slowly then the white dwarf surface remains cool enough for the surface of the star (including the deposited material) to remain degenerate*.
		This states that when a white dwarf becomes more than 1.4 times the mass of the Sun, the laws of Quantum mechanics prohibit the matter at the center of the white dwarf from being any denser.
		In a normal less massive star, this increase in energy would expand the size of the core, but, because the gas at the surface of the white dwarf is degenerate, it only increases the temperature.
	www.astronomyinfo.pwp.blueyonder.co.uk /Supernova.htm (2627 words)

	Nat' Academies Press, Astronomy and Astrophysics for the 1980's, Volume 2: Reports of the Panels (1983)
		Cataclysmic Variable Stars and Magnetic White Dwarfs One of the most exciting prospects for E W astronomy is the study of cataclysmic variables, which are close binary systems containing a degenerate dwarf and a late-type non- degenerate star.
		Alternatively, the E W flux may be produced by cyclotron cooling of the shock-heated accretion flow in the magnetic field of the degenerate dwarf, with addi- tional E W radiation emitted from the heated surface.
		White dwarfs are the end products of the evolution of stars with initial masses less than about 5 solar masses, which includes the vast majority of stars, yet we know surprisingly little of their own evolution and properties.
	www.nap.edu /books/0309033349/html/38.html (2068 words)

	sciforums.com - dwarf stars (Site not responding. Last check: 2007-09-08)
		A brown dwarf is in essence a star which did not have enough mass to ingite hydrogen fusion in its nucleous.
		White dwarfs is the end stage of a main class star (like our sun) when it has burned up all its hydrogen and doesn't have enough mass to begin buring helium.
		A brown dwarf is nothing more then an oversized planet however a white dwarf has degenerate matter.
	www.sciforums.com /showthread.php?t=311 (338 words)

	Dwarf Novae (Site not responding. Last check: 2007-09-08)
		The mass of the secondary star is continually falling and it is possible that some very faint dwarf novae may infact have a degenerate brown dwarf like secondary star that is no longer nuclear burning.
		Quasi-periodically the accretion disk partially collapses and material is deposited onto the white dwarf, the resulting release of gravitational energy is heats the disk material and we see a dwarf nova outburst that lasts from 1 day to several weeks.
		What causes the disk to collapse is a matter of debate, it is undoubtedly due to an increase in the disk viscosity, though the cause of the viscosity and the reasons why the viscosity can have two values in not really known.
	star-www.st-and.ac.uk /~ws9/dwarfnovae.html (324 words)

	The Astrophysics Spectator: The Structure of Keplerian Accretion Disks
		The accretion disks we encounter around degenerate dwarfs, neutron stars, and the smaller (several solar masses) fl hole candidates that are in compact binary systems are thin steady-state Keplerian disks, as are the accretion disks around newly-formed stars.
		The free-fall velocities at the surfaces of degenerate dwarfs, neutron stars, and fl holes are extremely high.
		The lowest velocities are associated with degenerate dwarfs, which are stellar remnants held up by electron degeneracy pressure that are about the mass of the Sun the radius of the Earth; the free-fall velocity for these stars is about 2% of the speed of light, which releases 1.5×10
	www.astrophysicsspectator.com /background/survey/galactic/DisksAccretionKeplerianStructure.html (1168 words)

	One Hundred Tamils - Subrahmanyan Chandrasekhar - The Man who “Dwarfed” the Stars
		His results showed that the, the radius of the white dwarf is proportional to the cube root of the mass; density is proportional to the square of the mass.
		During his voyage he realized that his results on a white dwarf were limited to the case where the star's electron gas was moving with non relativistic speed (speed much less than the velocity of light).
		Considering the case that a white dwarf is completely degenerate and relativistic, Chandra went on to discover one of the most intriguing results in astrophysics.
	www.tamilnation.org /hundredtamils/chandrasekhar.htm (7483 words)

	White Dwarfs (Site not responding. Last check: 2007-09-08)
		Degenerate electron pressure halts the collapse so the white dwarf maintains a constant radius.
		Once a white dwarf has radiated off all of its residual heat, it emits no light and is referred to as a fl dwarf.
		The more massive a white dwarf is, the smaller its radius will be (since a more massive star has a higher gravity and is therefore compressed to a smaller size).
	www.astro.umd.edu /education/astro/stev/wdwarf.html (439 words)

	February 24, 1995 (Site not responding. Last check: 2007-09-08)
		White dwarfs radiate because they are born hot and because they slowly contract releasing gravitational energy as they cool.
		This can be understood by noting the size of the degenerate pressure depends on the density of the gas in the sense that the pressure is greater, the greater the density.
		Since the radius of a white dwarf must be small for a massive white dwarf, for a very massive white dwarf, the radius must be tiny.
	zebu.uoregon.edu /~imamura/122/lecture-9a/lecture-9a.html (538 words)

	astr201 (Site not responding. Last check: 2007-09-08)
		White dwarfs are the “burnt-out relics of a star’s former glory”.
		White dwarfs can be either a carbon-oxygen core or a helium core of a dead star.
		After it has left the main sequence and preceded to core helium burning, a star that is less massive than about 4 solar masses is never able to redevelop the necessary conditions to use the carbon, oxygen, and helium it has created for thermonuclear energy in the core.
	www.owlnet.rice.edu /~maranda/astr201.html (1121 words)

	AS102 Modern Astronomy
		The pressure in a degenerate gas depends only on the speed of the degenerate particles NOT the temperature of the gas.
		A white dwarf must be less than about 1.4 solar masses, beyond which the resistance of electrons to compression cannot support the core against its own gravity.
		The white dwarf must be in a binary system with a main sequence companion so that the amount the total shift due to the ordinary doppler effect can be determined and subtracted out.
	www.butler.edu /physics/as102/homework/homework10/Hwk10sol.htm (4182 words)

	The Forging of Baruk
		The other dwarf reminded him too much of gully dwarves, the groveling, pathetic garbage dwellers who made their filthy lairs where even the orcs did not.
		The elf's slanted green eyes regarded the dwarf coolly and by the way he held his brilliantly crafted longbow, Baruk was sure he was ready to let loose another arrow before the dwarf could raise his axe.
		Only it pained the dwarf to see how little the human cared for his beard, for it was dirty and had not seen oil in weeks, if ever.
	dndworld.com /kb/adventures/baruk2.html (2848 words)

	ASTR 498N Lecture 19
		Thus, a white dwarf is about the size of the Earth. This mass-radius relationship is only approximate since it is based on nonrelativistic degeneracy. Accounting for relativistic degeneracy modifies the relationship for the more massive white dwarfs; and, of course, the relationship terminates at the Chandrasekhar mass.
		To estimate the properties of the skin, make the idealization that the boundary between the interior and the skin occurs where the degenerate electron pressure and the classical electron pressure are equal. Outside this point, we assume that the gas is classical.
		The energy source for the luminosity of a white dwarf is the thermal energy of the classical ions in the interior (the contribution of gravitational contraction is minor). That is,
	www.astro.umd.edu /~drabin/Lecture19.htm (891 words)

	Astronomy Lecture Number 20
		The core is made of electron degenerate matter (all available electron energy states are filled, nuclei are in tightly packed "crystalline-lattice-like" state), with a very thin atmosphere of non-degenerate matter over the surface.
		T are seen in a few percent of white dwarfs, especially those in binary systems, due to enhancement as star collapses (conservation of magnetic flux, as we saw during the collapse of protostars).
		The state of matter is a neutron degenerate gas, with same temperature-independent pressure as for electron degeneracy.
	physics.njit.edu /~dgary/202/Lecture20.html (1874 words)

	Classification of white dwarfs (Site not responding. Last check: 2007-09-08)
		As white dwarfs were discovered after non-degenerate stars, their classification has tended to follow the stellar classification system.
		Nearly all white dwarf stars appeared upon discovery to have either mono-elemental hydrogen or helium atmospheres (H and He are the only elements whose absorption lines were visible in the optical spectra).
		White dwarfs, as any other type of star, can be divided into two further categories: those found as isolated objects, and those occurring in binary or multiple star systems.
	www.star.ucl.ac.uk /~cmj/thesis/node11.html (716 words)

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