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Topic: Chandrasekhar limit

	Chandrasekhar limit - Wikipedia, the free encyclopedia
		The limit was first discovered and calculated by the Indian physicist Subrahmanyan Chandrasekhar in 1930, during his maiden voyage to Britain from India.
		The first scientific significance of this limit comes from the fact that he introduced/applied Einstein's special theory of relativity to study/deduce the end stage evolution of stars and the second significance comes from the fact that it prophesied the existence of fascinating stellar phenomena, albeit not characterized further.
		The Chandrasekhar limit arises from taking account of the effects of quantum mechanics in considering the behaviour of the electrons providing the degeneracy pressure supporting the white dwarf.
	en.wikipedia.org /wiki/Chandrasekhar_limit (745 words)

	Subrahamanyan Chandrasekhar, , Legends, Subrahamanyan Chandrasekhar profile, Chandrasekhar calculated his 'limit' ... (Site not responding. Last check: 2007-10-08)
		Chandrasekhar calculated his 'limit' purely on mathematical equations, astronomers have found that all the White Dwarf stars in the sky have masses within his prescribed limit...
		Chandrasekhar was born on October 10, 1910, in Lahore.
		Chandrasekhar has also made significant contributions to understanding the atmosphere of stars and the way matter and motion are distributed among the stars in a galaxy.
	www.4to40.com /legends/index.asp?article=legends_schandrasekhar (665 words)

	Chandra
		The numerical magnitude of the Chandrasekhar limit is expressed in the unit of mass of the Sun.
		The genius of Chandrasekhar was that using the special theory of relativity and the quantum statistical mechanics as keys he explored the physics of the white dwarf and discovered new features.
		As this article has been written with the limited purpose of giving a non-mathematical account of the fundamental work carried out by Chandrasekhar in the initial years of his scientific career, it is difficult to go further without bringing in the mathematics.
	www.geocities.com /Athens/Parthenon/2686/chandra.htm (1945 words)

	White Dwarf
		A white dwarf which exceeds this limit (known as the Chandrasekhar limit), typically by mass transfer from a companion star, may explode as a Type Ia supernova via a process known as "carbon detonation".
		When this limit is exceeded, the pressure exerted by electrons is no longer able to balance the force of gravity, and the star continues to contract, eventually forming a neutron star.
		Despite this limit, most stars end their lives as white dwarfs since they tend to eject most of their mass into space before the final collapse (often with spectacular results - see planetary nebula).
	www.juliantrubin.com /encyclopedia/astronomy/whitedwarf.html (1494 words)

	White Dwarfs and Electron Degeneracy
		Chandrasekhar was interested in the final states of collapsed stars as determined by electron degeneracy and had used the work of Arthur S. Eddington and Ralph H. Fowler to begin his calculations.
		Chandrasekhar himself had no idea what would happen when the limit of 1.44 solar masses was exceeded, except that the star would continue to collapse.
		But even that is not the ultimate limit, since neutron degeneracy can also be overcome by masses greater than 3 solar masses and the ultimate collapse is toward a fl hole.
	hyperphysics.phy-astr.gsu.edu /hbase/astro/whdwar.html (729 words)

	Dream 2047 : January 99 (Site not responding. Last check: 2007-10-08)
		Chandrasekhar's life as Kameshwar C. Wali wrote "stands out for its singular dedication to the pursuit of science, and for practicing the precepts of science and living up to its values to the closest possible limit in one's life." His prolific contributions spanned astrophysics, physics and applied mathematics.
		The formulation of the Chandrasekhar Limit led to the discovery of neutron stars and fl holes.
		Chandrasekhar was awarded (jointly with the nuclear astro_physicist W.A. Fowler) the Nobel Prize in Physics in 1983 While Chandrasekhar is best known for Chandrasekhar Limit, for him there was no limit.
	www.vigyanprasar.com /dream/May99/MAYArticle1.htm (1696 words)

	lokpriya!
		Chandrasekhar was educated at Presidency College, at the University of Madras, and at Trinity College, Cambridge.
		Chandrasekhar determined what is known as the Chandrasekhar limit - that a star having a mass more than 1.44 times that of the Sun does not form a white dwarf but instead continues to collapse, blows off its gaseous envelope in a supernova explosion, and becomes a neutron star.
		Chandrasekhar was awarded the Gold Medal of the Royal Astronomical Society in 1953 and the Royal Medal of the Royal Society in 1962.
	www.lokpriya.com /personalities/scientists/chandrasubh.html (184 words)

	Subrahmanyan Chandrasekhar (Site not responding. Last check: 2007-10-08)
		Subrahmanyan Chandrasekhar was one of the most brilliant theoretical astrophysics of the modern age.
		Chandrasekhar's most important contribution was his discovery of the upper bound for the mass of a white dwarf star.
		Chandrasekhar was one of the few scientists who was able to continue his rigorous research throughout most of his life while remaining on the forefront of the scientific community.
	www.usd.edu /phys/courses/phys300/gallery/clark/chand.html (544 words)

	Chandrasekhar limit - QuickSeek Encyclopedia (Site not responding. Last check: 2007-10-08)
		The Chandrasekhar limit is the maximum mass of a white dwarf, a type of star, and is approximately 3 × 10
		The limit was first calculated by and thus named after the Indian physicist Subrahmanyan Chandrasekhar.
		If the star has a mass below the Chandrasekhar limit this collapse is limited by electron degeneracy pressure, which results in a stable white dwarf.
	chandrasekharlimit.quickseek.com (449 words)

	Black Holes (Site not responding. Last check: 2007-10-08)
		Chandrasekhar calculated and found out that this mass limit is 140% the mass of the sun.
		From this limit, and up to the mass limit of two solar masses, the self gravitational pull will exceed the anti-force provided by the electrons, and will make them collide with the protons in the nucleus of the atom, to make neutrons.
		Chandrasekhar was able to prove that the anti-force caused by "Ekron Ha'Isur", won't be able to stop a star with a mass bigger than the mass limit of a neutron star.
	www.leyada.jlm.k12.il /proj/black/black.htm (1372 words)

	ScienceWeek
		Chandrasekhar calculated that a cold star of more than about one and a half times the mass of the sun would not be able to support itself against its own gravity.
		Note #1: Chandrasekhar limit: The remnant mass after the blow-off during the terminal stage of the life of a star determines the ultimate fate of the star.
		In 1930, Subramaynyan Chandrasekhar realized that in order to provide the incredible pressures required to maintain more massive stars, the electrons supplying that support would have to move at greater than the speed of light, which was known from the special theory of relativity to be an impossibility.
	scienceweek.com /2003/sw030110.htm (3768 words)

	[No title] (Site not responding. Last check: 2007-10-08)
		Chandrasekhar's work on dwarf stars led to what is known today as the Chandrasekhar limit which states that any stars whose mass is in excess of 1.44 times that of the sun continues to collapse while blowing off its gaseous envelope resulting in a supernova explosion.
		The Chandrasekhar limit goes on to say that a star having an extremely excessive mass continues to collapse and eventually becomes a fl hole.
		Chandrasekhar's most important work was entitled, An Introduction to the Study of Stellar Structure, written in 1939 and served as a compilation of investigations on stellar interiors and models.
	www.upei.ca /~xliu/multi-culture/chan.htm (412 words)

	chandra
		Chandrasekhar's life as Kameshwar C. Wali wrote " stands out for its singular dedication to the pursuit of science, and for practicing the precepts of science and living up to its values to the closest possible limit in one's life.
		To his great surprise, he found that this combination predicted that white dwarfs could only exist up to a certain limiting mass which depended chiefly on fundamental constants such as h, G and the mass of the hydrogen atom; the mass was about 1.45 times the mass of the Sun.
		When the iron core grows to the Chandrasekhar mass, it collapses by gravitation into a neutron star, and the rest of the star is expelled, giving a type II supernova.
	www.galcit.caltech.edu /~bobba/chandra.html (1583 words)

	webindia123-Indian personalities-Scientists-Subrahmanyan Chandrasekhar
		Chandrasekhar was noted for his work in the field of stellar evolution, and in the early 1930s he was the first to theorize that a collapsing massive star would become an object so dense that not even light could escape it; now known as the Black hole.
		He demonstrated that there is an upper limit (known as 'Chandrasekhar Limit') to the mass of a White dwarf star.
		Chandrasekhar was a creative, prolific genius whose ability to combine mathematical precision with physical insight changed humanity's view of stellar physics.
	www.webindia123.com /personal/scientist/chandra.htm (460 words)

	Schonberg-Chandrasekhar limit
		The maximum mass of a star's helium-filled core that can support the overlying layers against gravitational collapse, once the core hydrogen is exhausted; it is believed to be 10 to 15% of the total stellar mass.
		If this limit is exceeded, as can only happen in massive stars, the core collapses, releasing energy that causes the outer layers of the star to expand to become a red giant.
		It is named after Subrahmanyan Chandrasekhar and the Brazilian astrophysicist Mario Schönberg (1916-).
	www.daviddarling.info /encyclopedia/S/Schonberg-Chandrasekhar_limit.html (153 words)

	[No title]
		Chandrasekhar Limit --- A white dwarf can't have indefinitely high mass.
		The mass at which this happens is the Chandrasekhar Limit, about 1.4 solar masses for a white dwarf of normal composition.
		In contrast, the progenitors of type II supernovae are massive stars that differ in their properties (mass, chemical composition, rotation rate,...) and this heterogeneity is reflected in their light curves.
	www.ifa.hawaii.edu /~acowie/class99b/class_20.html (929 words)

	White dwarf starrs (Site not responding. Last check: 2007-10-08)
		Chandrasekhar realized that since, as radius decreases with increasing mass, a regime will be reached where the electron speeds (momenta) approach the speed of light, the gas becomes relativistically degenerate, and the equation of state changes to the form
		As the fully catalyzed core mass increases beyond the Chandrasekhar limit the density increases and higher and higher electron momentum states are occupied.
		The above limit is an upper limit, ignoring the fact that neutrons are attracted by the strong nuclear force while electrons are repelled by Coulomb forces and at high densities the neutrons may no longer be neutrons, rather a quark "soup".
	www.physics.uq.edu.au /people/ross/ph3080/whitey.htm (1253 words)

	Neutronium - TheBestLinks.com - Atom, Black hole, Chandrasekhar limit, Electron, ... (Site not responding. Last check: 2007-10-08)
		Neutronium is a colloquial and often misused term for an extremely dense phase of matter that occurs in the intense pressure found in the core of neutron stars and is currently not well understood.
		There is a limit beyond which a neutron star can no longer support itself via neutron degeneracy pressure and would collapse all the way into a fl hole.
		The exact limit depends on the equation of state which is used but estimates range from 1.4 to 3 solar masses.
	www.thebestlinks.com /Neutronium.html (555 words)

	White Lies about Black Holes
		Chandrasekhar believed that a “non-relativistic gas” at the center of a white dwarf could always adjust itself until the gravitational forces compressing the star are countered.
		The limiting mass, termed the Chandrasekhar limit, has been calculated to be 1.2 solar masses.
		The cores of these galaxies are thus in the same condition as the white dwarf stars and quasars; their densiiy is abnormally high because the introduction of the time displacement of the ultra high speeds reduces the equivalent space occupied by the central portion of the galaxy.
	www.reciprocalsystem.com /rs/satz/whiteblack.htm (1379 words)

	Chandrasekhar Limit - Search Results - MSN Encarta (Site not responding. Last check: 2007-10-08)
		Chandrasekhar Limit - Search Results - MSN Encarta
		Chandrasekhar Limit, upper limit to the mass that a white dwarf star can have, about 1.4 times the mass of the Sun.
		Chandrasekhar, Subrahmanyan (1910-1995), Indian-born American theoretical astrophysicist and Nobel laureate, who contributed greatly to the current...
	uk.encarta.msn.com /Chandrasekhar_Limit.html (108 words)

	A Tribute To Subrahmanyan Chandrasekhar - 1983 Physics Nobelist
		Subrahmanyan Chandrasekhar, a winner of the 1983 Nobel Prize in physics whose theories about the evolution of stars led to the concept of fl holes, died of heart failure on August 21 at the University of Chicago Hospitals.
		Subrahmanyan Chandrasekhar was born in October of 1910 in Lahore, which is now in Pakistan rather than India as it was at the time of his birth.
		Chandrasekhar was a brilliant student, and while at Cambridge he worked with two of the leading astrophysicists of the time, Edward Milne and Arthur Eddington.
	www.tamil.net /people/andrew/subra.htm (5375 words)

	Sea and Sky's Cosmic Wonders: Pulsars
		A physicist named Chandrasekhar Subrahmanyan theorized that if the mass of the core of the collapsing star was 1.4 times the mass of the star itself, the protons and electrons would combine to form neutrons in a neutron star.
		If this limit is not achieved by the collapsing core, a white dwarf star will be produced instead.
		If the limit is much greater, a fl hole may be the result.
	www.seasky.org /cosmic/sky7a08.html (927 words)

	white_dwarfs (Site not responding. Last check: 2007-10-08)
		In 1931 Chandrasekhar showed that as a white dwarf became more massive, and the electrons that supported its weight became relativistic, there would be a point beyond which the degeneracy pressure would be insufficient to support the star.
		This mass is approximately 1.4 times the mass of the sun, it is known as the Chandrasekhar limit.
		In this paper I will discuss the history of the discovery, and its importance in astrophysics, then derive in detail the Chandrasekhar limit, including some of the refinements that have been made since Chandrasekhar's original paper.
	www.davegentile.com /thesis/white_dwarfs.html (199 words)

	The Telegraph - Calcutta : KnowHOW (Site not responding. Last check: 2007-10-08)
		The scientist was speaking about the model of the Chandrasekhar Limit exhibited during the Indian Festival of Science at the museum.
		Chandrasekhar had predicted that a star is a white dwarf if its mass is less than 1.44 times the mass of the sun.
		This figure of 1.44 is known as the Chandrasekhar Limit.
	www.telegraphindia.com /1060508/asp/knowhow/story_6190555.asp (1165 words)

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