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Topic: Eddington limit

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Arthur Eddington

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	Arthur Eddington Biography
		Eddington also investigated the interior of stars, and calculated their temperature based on what would be necessary to withstand the pressure of the higher-laying layers.
		In 1920, Eddington, on the basis of the precise measurements of atoms by F. Aston, was the first to suggest that stars obtained their energy from nuclear fusion of hydrogen to helium.
		Eddington at one time thought the fine structure constant α, which had been measured at approximately 1/137, should be exactly 1/137, based on aesthetic and numerological arguments.
	www.biographybase.com /biography/Eddington_Arthur.html (724 words)

	Arthur Eddington
		Eddington wrote an article, Report on the relativity theory of gravitation, which announced Einstein's theory of general relativity to the English-speaking world.
		After the war, Eddington travelled to the island of Principe near Africa to watch the solar eclipse of 29 May 1919.
		Eddington also investigated the interior of stars, and calculated their temperature based on what would be necessary to withstand the pressure of the higher-laying layers.
	www.ebroadcast.com.au /lookup/encyclopedia/ar/Arthur_Eddington.html (364 words)

	Eddington, Arthur Stanley (1882-1944)
		He contributed much to the introduction of Einstein’s general theory of relativity into cosmology, writing books on the new theory for both his fellow scientists and the public, and led one of the two 1919 solar eclipse expeditions that confirmed the predicted bending of starlight by gravity.
		Eddington’s greatest contributions concerned the astrophysics of stars.
		He dealt with the importance of radiation pressure, the transfer of energy by radiation, the mass-luminosity relation, pulsations in Cepheid variables, and the very high densities of white dwarfs, and was among the first to argue that subatomic reactions must power the stars.
	www.daviddarling.info /encyclopedia/E/Eddington_Arthur.html (195 words)

	Astrophysics and Mysticism: the life of Arthur Stanley Eddington
		Arthur Stanley Eddington was born on 28 Dec 1882 in Kendal, on the edge of the Lake District.
		Eddington thought he had a proof that the inverse of the fine structure constant (the dimensionless constant formed from the values h, c and e, that governs the strength of radiative interactions in atoms) is precisely 137.
		Eddington identifies three types of knowledge: (1) structural, with the approximate meaning of mathematical, but in Eddington's thinking the structure appears to be almost identified with Group theory, (2) direct awareness (approximately sensation) and (3) sympathetic understanding, which he argues is essential because a remembered sensation is sympathetic understanding of a past sensation.
	silas.psfc.mit.edu /eddington (4942 words)

	Eddington luminosity - Wikipedia, the free encyclopedia
		Eddington luminosity (sometimes also called the Eddington limit) is the largest luminosity that can pass through a layer of gas in hydrostatic equilibrium, supposing spherical symmetry.
		The exact value of Eddington luminosity depends on the chemical composition of the gas layer and the spectral energy distribution of the emission.
		The Eddington limit is not a true limit, and it is believed that photon-bubble instabilities (which remove the strict spherical symmetry) allow nature to have radiating flows with much higher luminosities.
	en.wikipedia.org /wiki/Eddington_limit (388 words)

	Eddington limit
		In physics, the Eddington Limit is a natural limit to the luminosity that can be radiated by accretion onto a compact object, like a fl hole.
		If luminosity exceeds the Eddington limit, there would be so much radiation pressure that the surrounding gas is pushed outward rather than inward.
		The Eddington limit calculates minimum mass of active galactic nuclei.
	www.ebroadcast.com.au /lookup/encyclopedia/ed/Eddington_limit.html (107 words)

	Arthur Stanley Eddington Biography
		Eddington showed that, to avoid collapse, the outward gas and radiation pressure of a star must equal its inward gravitational pull.
		Sir Arthur Stanley Eddington, OM (December 28, 1882 – November 22, 1944) was an astrophysicist of the early 20th century.
		The Eddington limit, the natural limit to the luminosity that can be radiated by accretion onto a compact object, is named in...
	www.bookrags.com /Arthur_Stanley_Eddington (186 words)

	The Reference Frame: Arthur Eddington died 63 years ago
		Eddington was once asked by a journalist whether it was true that only three people understood general relativity.
		Eddington started with the key assumption that the fine structure constant was exactly 1/136.
		While Sir Arthur Stanley Eddington attempts to derive alpha=1/137 mathematically may be considered to be a stretch, as correctly noted by Nobel laureate David Gross, in the meantime such a theoretical derivation is possible and feasible.
	motls.blogspot.com /2007/11/arthur-eddington-died-63-years-ago.html (1240 words)

	Sir Arthur Eddington
		Eddington severely criticized the work of Chandrasekhar although his own ideas were outdated and incorrect.
		However, his argument was incorrect, and the Chandrasekhar Limit for the mass of a white dwarf still stands today as the correct way of determining the upper bound for the mass of a white dwarf.
		Eddington was one of the earliest creators of the concept of relativity.
	www.usd.edu /phys/courses/phys300/gallery/clark/edd.html (624 words)

	Eddington limit
		The theoretical limit at which the radiation pressure of a light-emitting body would exceed the body's gravitational attraction.
		This would happen, for example, to a star of more than about 120 solar masses, or to the Sun if its luminosity were increased by a factor of 30,000.
		The Eddington limit, named after Arthur Eddington, is given by
	www.daviddarling.info /encyclopedia/E/Eddington_limit.html (138 words)

	Grasslands Observatory - Essays - How Heavy Can a Star Get?
		The Eddington limit is a theoretical upper limit to the ratio of luminosity to mass for a star.
		At the Eddington limit, the outward pressure of a star’s energy from its central nuclear processes exceeds its inward gravitational pull.
		The observed limit of 150 Solar masses may reflect either a fundamental mass limit, or it may merely reflect an observational limitation of the data (Weidner, 2004).
	www.3towers.com /sGrasslands/Essays/HeavyStar/HeavyStar01.asp (570 words)

	Eddington Hook - Open University Stockist, Books For Students, Set Texts, OU Courses
		Eddington Hook undertake not to divulge to any third party any information concerning customers that would be in breach of the Data Protection Acts.
		This is a comprehensive limitation of liability that applies to all damages of any kind, including (without limitation) compensatory, direct, indirect or consequential damages, loss of data, income or profit, loss of or damage to property and claims of third parties.
		For the avoidance of doubt, Eddington Hook does not limit its liability for death or personal injury to the extent only that it arises as a result of the negligence of Eddington Hook, its affiliates, directors, employees or other representatives.
	www.eddington-hook.co.uk /ehook/termsofcondition.asp (515 words)

	ESA - Space Science - Studying the stars, testing relativity: Sir Arthur Eddington
		Eddington suspected that the chief source of a star's energy was sub-atomic and that hydrogen played a dominant role in supplying this energy.
		Later, Eddington became convinced that the fundamental constants of nature, such as the mass of the proton and the charge of the electron, were a 'natural and complete specification for constructing a Universe' and that their values were not accidental.
		Eddington died in 1944, without completing this line of research and his book, entitled Fundamental Theory (1946), was published after his death.
	www.esa.int /esaSC/SEMDYPXO4HD_index_0.html (756 words)

	AULIS Online – Different Thinking
		Arthur Eddington's selective presentation of data from the 1919 eclipse so that it supposedly supported "Einstein's" general relativity theory is surely one of the biggest scientific hoaxes of the 20th century.
		Eddington was less interested in testing a theory than he was in crowning Einstein the king of science.
		Eddington ceased to be a scientist and, instead, became an advocate for Einstein.
	www.aulis.com /albert_einstein.htm (3971 words)

	The New England Skeptical Society - Articles
		In the end, Eddington was wrong, and Chandrasekhar won the Nobel prize in 1983 for his discovery of what is now known as the Chandrasekhar Limit.
		Eddington, a true giant of physics, is now remembered for one of the great examples of the use of the Argument from Authority.
		Eddington was physics, and vice versa, and that gave him the ability and the right to pronounce on anything that impinged on his authority.
	www.theness.com /articles.asp?id=24 (1292 words)

	Active Galaxies and Quasistellar Objects, Accretion
		In the context of the fl hole model for quasars, this inward drift of matter is known as accretion and the rate and the manner of the accretion in individual active galactic nuclei is a major factor in determining the type of object we observe.
		There is a natural limit, known as the Eddington limit and named alter the famous astronomer, Sir Arthur Eddington, to the luminosity L that can be radiated by a compact object of mass M.
		This limit arises because both the attractive gravitational force acting on an electron-ion pair and the repulsive force due to radiation pressure decrease inversely with the square of the distance from the fl hole.
	nedwww.ipac.caltech.edu /level5/ESSAYS/Blandford/blandford.html (1527 words)

	The Astrophysics Spectator: The Capture of Winds by Sagitarrius A*
		The luminosity at which the radiative pressure on a fully-ionized plasma is precisely counteracted by the gravitational force at the photosphere of a star is called the Eddington limit.
		The Eddington limit is directly proportional to the mass of the star.
		The Eddington limit is not limited to stars; it sets the upper limit on the amount of radiation a fl hole can produce as it consumes gas.
	www.astrophysicsspectator.com /topics/milkyway/SagittariusAStarWindCapture.html (1518 words)

	Passing the Eddington limit without getting a ticket (cont.) \| ScienceBits
		In strange mode instabilities, the term arises because the temperature in the diffusion limit depends on the radial gradient of the opacity perturbations.
		This limit corresponds to the top layers of an atmosphere of a luminous object (yet deep enough for the inhomogeneities to remain opaque).
		When perturbations arising from the instabilities, which are expected to be of order the atmospheric scale height, lose their opaqueness, the effective opacity tends to the microscopic value and the effective Eddington limit tends to the classical value.
	www.sciencebits.com /SurpassingEddingtonPage2 (2035 words)

	Eddington and Einstein \| Astronomy Blog
		Eddington was an accomplished astrophysicist who had been chief assistant to the Astronomer Royal at Greenwich and was made director of the Cambridge Observatory (located a few miles from the more recent Mullard Radio Astronomy Observatory) in 1914.
		Amongst his achievements he showed that radiation pressure was necessary to keep stars from collapsing under their own gravity and the Eddington Limit now appears in most undergraduate astronomy texts.
		One of Eddington's other famous contributions were his observations taken on Principe during the total solar eclipse of May 1919.
	www.strudel.org.uk /blog/astro/000817.shtml (455 words)

	The laws list: E
		The theoretical limit at which the photon pressure would exceed the gravitational attraction of a light-emitting body.
		A hypothetical drive exploiting the peculiarities of quantum mechanics by restricting allowed wavelengths of virtual photons on one side of the drive (the bow of the ship); the pressure generated from the unrestricted virtual photons toward the aft generates a net force and propels the drive.
		The region around a rotating fl hole, between the event horizon and the static limit, where rotational energy can be extracted from the fl hole.
	www.alcyone.com /max/physics/laws/e.html (647 words)

	Subramaniam Chandrasekar
		Eddington's arguments were somewhat qualitative and did not include the results of special relativity and quantum physics.
		This upper limit of 1.44 time the mass of the Sun on white dwarfs is now known as Chandrashekhar limit By 1933, Chandrashekhar formed a complete theory of white dwarfs and decided to report the results at a meeting of the Royal Astronomical Society.
		He realized that the argument between him and Eddington was essentially in what kind of physics to apply to these compressing stars at end of their life cycle.
	www.iasf.org /subraman.htm (1888 words)

	Arthur Stanley Eddington - Wikipedia, the free encyclopedia
		Eddington received an MA in 1915 and did not have a doctorate or doctoral advisor.
		Later that year, Robert Ball, holder of the theoretical Lowndean chair also died, and Eddington was named the director of the entire Cambridge Observatory the next year.
		Eddington's observations published next year (Dyson, F.W., Eddington, A.S., and Davidson, C.R. A Determination of the Deflection of Light by the Sun's Gravitational Field, from Observations Made at the Total Eclipse of May 29, 1919 Mem.
	en.wikipedia.org /wiki/Arthur_Stanley_Eddington (1762 words)

	[No title]
		Sir Arthur Stanley Eddington (December 28, 1882 - November 22, 1944) was arguably the most important astrophysicist from the early 20th century.
		This same war caused problems for Eddington himself when he was called up for military service.
		The Eddington limit is named in his honour.
	www.famous-astrophysicists.com /astrophysicists/eddington.htm (374 words)

	Passing the Eddington limit without getting a ticket \| ScienceBits
		Under the classical picture, one cannot surpass the Eddington limit while keeping the system in steady state, because nothing could balance the net force outwards, and gas will necessarily be accelerated outwards, thereby "evaporating" the system.
		But in systems which remain intact for durations much longer than their dynamical time scale, the limit should be relevant, at least according to the classical picture.
		This is because as the Eddington Luminosity is approached, convection (i.e., the transport of heat using macroscopic flow, such as water in a boiling pot) is always excited, and is efficient enough to keep the bulk of the star sub-Eddington.
	www.sciencebits.com /SurpassingEddington (1543 words)

	The Astrophysics Spectator: Energetics of Keplerian Accretion Disks
		This lower limit is set solely by the rate at which mass flows through the disk.
		The lower limit on temperature arises because there is an upper limit on how much light a body of a given temperature can radiate.
		For a neutron star, we see that accretion at close to the Eddington limit produces a disk with a surface temperature at its inner edge of over 1 keV, which places its radiation in the soft x-ray band.
	www.astrophysicsspectator.com /topics/disks/AccretionKeplerianEnergetics.html (857 words)

	Possible Mechanisms
		The classical Eddington limit, where opacity is due to electron scattering only, has already been explained to depict an LBV's tenuous hold on its outer layers.
		In this limit, opacity is taken to be density and temperature dependent.
		For a star that is already near the Eddington limit, this increase in opacity could cause radiation pressure to overwhelm gravity.
	www.pha.jhu.edu /~ericpeng/seminar/node8.html (476 words)

	Chandrasekhar-Schonberg limit concept from the Astronomy knowledge base
		The limit is now reckoned as 10 to 15 per cent of the star's total mass.
		In order to maintain its luminosity by hydrogen burning just outside the isothermal core, the star must keep a high temperature and a high pressure at the surface of the core.
		When the helium core exceeds about 12% of the star's total mass, the star can no longer adjust by small changes, but must drastically increase in radius and move rapidly from the main sequence.
	www.site.uottawa.ca:4321 /astronomy/Chandrasekhar-Schonberglimit.html (139 words)

	News August 2002: Nearby interacting galaxy pair has a rich set of ultra-luminous X-ray sources
		The outer limits of the optical galaxies are shown as ellipses.
		However, for an X-ray binary to shine the gas has to reach the collapsed star, and at very high luminosities, above the so-called 'Eddington limit', the force imparted on the in-falling gas by the emitted radiation is greater than the gravitational attraction.
		For such massive fl holes the Eddington limit is high enough to avoid the paradox, but they take around a billion years to grow to this size, much too long to be associated with active star formation.
	www.star.le.ac.uk /news/0802.html (833 words)

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