Einstein, AlfredBiblio.com
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2019x-0691655847Princeton Univ Pr 2019. Paperback. New. reprint edition. 368 pages. 10.00x8.00x0.79 inches. Princeton Univ Pr paperback
2019x-0691655782Princeton Univ Pr 2019. Paperback. New. reprint edition. 448 pages. 9.75x8.00x1.00 inches. Princeton Univ Pr paperback
1949044767Princeton: Princeton University Press 1949. Translated by Alexander H. Krappe Roger H. Session and Oliver Strunk. 3 vols. xvi 887 3; xxx 333p. b/w illus. music burgundy cloth original publisher's stiff-board slipcase ex libiris Daniel Heartz with his occasional pencilled notes. Princeton University Press unknown
2007DADAX0548121761Kessinger Publishing 2007-07-25. hardcover. New. 6.00x1.19x9.00. Buy with confidence. Excellent Customer Service & Return policy. Kessinger Publishing hardcover
B9781018859484Hardback. New. hardcover
1330960890.Gpaperback. Good. Access codes and supplements are not guaranteed with used items. May be an ex-library book. paperback
0332566072.Ghardcover. Good. Access codes and supplements are not guaranteed with used items. May be an ex-library book. hardcover
B9781020300318Hardback. New. hardcover
B9781498089524Paperback / softback. New. paperback
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1945180350Lancaster Pennsylvania: American Physical Society 1945 & 1946. His most significant later contribution to cosmology First editions offprint issues of the papers that introduced the Swiss-cheese model of the universe. Einstein and Straus revised the FLRW metric by suggesting that the universe is in fact inhomogeneous. "In two ground-breaking papers Einstein and Straus showed how galaxies fit into a Universe with zero pressure. This model helps to describe the universe observed today" Harwit p. 573. Quarto pp. 5. Disbound wire-stitched as issued. Nicks and creasing to extremities short closed tears to outer margins pp. 120-1 of Influence detached rear blank almost detached: in very good condition. Boni 252 & 252.1; Weil 216. Martin Harwit Astrophysical Concepts 2010. unknown
19455054Lancaster PA: American Physical Society 1945. First edition. <p>First edition extremely rare offprints of Einstein & Straus's introduction of the 'Swiss-cheese' model of the universe. "By the spring of 1945 Einstein and Straus had found a new type of possible universe using Einstein's equations . This was a step towards a more realistic universe in which the matter was not smoothly spread with the same density everywhere but gathered up into lumps like galaxies which were spread about in empty space" Barrow The Book of Universes pp. 106-107.</p>. EINSTEIN'S 'SWISS-CHEESE' MODEL OF THE UNIVERSE - OFFPRINT ISSUE. <p>First edition extremely rare offprints of Einstein & Straus's introduction of the 'Swiss-cheese' model of the universe. "After a decade and a half of sometimes intense work on cosmology Einstein returned to the subject only occasionally in his later years. His most significant later contribution was a discussion of the impact of cosmological expansion on the gravitational field surrounding a star i.e. the offered papers . This was an important first step in understanding the impact of global cosmological expansion on local physics" Janssen & Lehner pp. 257-8. In the 1920s and 1930s a general relativistic model of the universe was developed called the Friedmann-Lemaître-Robertson-Walker FLRW model which correctly described the expansion of the universe discovered by Edwin Hubble. But the FLRW model was 'homogeneous' - it described a universe which looks the same wherever the observer is located. The actual universe however is manifestly inhomogeneous - it contains stars galaxies and clusters of galaxies. Einstein and Straus's papers represent the first serious attempt to model an inhomogeneous universe. "By the spring of 1945 Einstein and Straus had found a new type of possible universe using Einstein's equations. It described a universe which looked largely like one of the simple expanding universes of Friedmann and Lemaître containing material like galaxies which exerted no pressure. But it had spherical regions removed from it like bubbles in a Swiss cheese. Each empty hole then had a mass placed at its centre. The mass was equal in magnitude to what had been excavated to create the hole. This was a step towards a more realistic universe in which the matter was not smoothly spread with the same density everywhere but gathered up into lumps like galaxies which were spread about in empty space" Barrow pp. 106-107. Not on OCLC; no copies in auction records.</p> <br /> <p>In 1916 just a few months after Einstein had formulated his general theory of relativity Karl Schwarzschild had found a solution of Einstein's equations which described the gravitational field in the vicinity of a spherical distribution of mass such as a star or to anticipate later developments a black hole. This was in fact the first exact solution of Einstein's equations to be found - Einstein had earlier calculated an approximate solution which was enough to show that his theory correctly accounted for the advance of Mercury's perihelion. However at great distances from the star Schwarzschild's solution approaches the flat Minkowski spacetime with zero curvature and not the FLRW solution that represented an expanding universe. It seemed therefore that Schwarzschild's solution could not correctly describe the gravitational field of a star in an expanding FLRW universe. If the expansion of the universe meant that Schwarzschild's solution had to be modified this could make it possible to detect and measure the expansion of the universe by making local observations rather than by observing the motion of distant galaxies as Hubble had done. The problem of describing the gravitational field of a star in an expanding FLRW universe was addressed by Einstein and Straus in the offered papers.</p> <br /> <p>"In the early 1930s theorists began to develop a richer account of the evolution of the universe based on expanding models. Hubble's results qualitatively agreed with the redshift effect calculated in these models but the utility of the simple dynamical models depends on whether the universe is approximately uniform. The status of this assumption was the focus of lively debate . Relativistic cosmologists regarded the idealized uniformity of the FLRW models as a simplifying assumption . The unrelenting uniformity built into the FLRW models conflicts with the clear non-uniformity of the stars star clusters and galaxies of the local universe but the models might still serve as a useful approximation if the non-uniformities are negligible at larger scales" Janssen & Lehner p. 256.</p> <br /> <p>"By 1944 Einstein had recruited a new assistant at Princeton. His assistants were always talented young mathematicians who could make up for Einstein's self-confessed weakness in this area. Ernst Straus 1922-1983 was something of a mathematical prodigy . He was born in Munich but after the Nazis came to power in 1933 his family fled to Palestine where he was educated at high school and at the Hebrew University in Jerusalem. Straus didn't stay to take an undergraduate degree and instead while still a teenager moved to New York's Columbia University in 1941 to begin graduate research. In 1944 he found himself recruited as Einstein's new research assistant at the Institute for Advanced Study in Princeton. The young Straus had no background in physics and his mathematical inclinations were towards number theory and 'pure' mathematical topics but he lost no time in filling the gap left by the departures of Nathan Rosen 1935-45 and Leopold Infeld 1936-38" Barrow pp. 105-6.</p> <br /> <p>Einstein and Straus found an exact solution of the equations of general relativity in which a spherical 'hole' is cut out of an FLRW universe and the hole is replaced by a single mass point e.g. a star surrounded by a spherical cavity. The initially homogeneous matter within the cavity can be thought of as having been "condensed into the star". Einstein and Straus found that the interior of the cavity is described by the standard Schwarzschild solution. The radius of the hole is such that at its spherical boundary the outward pull from the cosmological masses is just balanced by the inward pull from the star. The cavity boundary expands according to the Hubble expansion of the whole universe. The universe outside the cavity is described by the standard expanding homogeneous FLRW solution. The possibility of exactly matching the Schwarzschild solution near the star to the FLRW solution outside it showed that it was not in fact possible to detect the expansion of the universe by making observations close to the star. There were similar solutions with more than one hole - Einstein said that this reminded him of the holes in Swiss cheese. The static vacuum region inside the cavity is now called an 'Einstein-Straus vacuole'.</p> <br /> <p>The methods introduced by Einstein and Straus in these papers have been used extensively to model inhomogeneities in the universe. For example in 1968 Martin Rees and Dennis Sciama investigated the effects of large-scale inhomogeneities such as superclusters of galaxies on the cosmic microwave background the so-called 'Rees-Sciama effect'. The Swiss-cheese model has also been used in the study of inflationary models of the early universe. According to this theory the universe expanded exponentially in the first tiny fraction of a second after the big bang with some parts of space-time expanding more quickly than others. This created 'bubbles' in space-time. The Swiss-cheese "embodies a natural way to model physical problems such as describing the boundary between a galaxy and intergalactic space or the relation between bubbles at the end of an inflationary era by taking two different regions where the behaviour is smooth and joining them at a surface of discontinuity" Ellis et al. p. 426.</p> <br /> <p>In the last decade several authors have suggested that Swiss-cheese models might solve a long-standing problem on the rate of expansion of the universe. Distant supernovas have been observed to be dimmer than expected on the basis of standard cosmological theories indicating that the universe is expanding faster than these theories predict. This has been explained by hypothesizing the existence of 'dark energy' although exactly what dark energy might be is a mystery. But if the light from distant supernovas had to cross large vacuoles in reaching an observer on the earth these would act like concave lenses making the supernovas appear dimmer and further away than they really are. Other authors have noted that the Milky Way is near the centre of a region that has fewer galaxies than other parts of the universe and that we might be living near the centre of a particularly large vacuole perhaps more than a billion light years in diameter see for example Bonnor.</p> <br /> <p>Weil 216. Barrow The Book of Universes 2011. Bonnor 'A generalisation of the Einstein-Straus vacuole' Classical and Quantum Gravity 17 2000 pp. 2739-2748. Ellis Maartens & MacCallum Relativistic Cosmology 2012. Janssen & Lehner eds. The Cambridge Companion to Einstein 2014.</p> <br/> <br/> Together two offprints 4to 267 x 200 mm pp. 120-124 & 148-149. Stapled as issued in original self-wrappers. American Physical Society unknown
125840849X.Gpaperback. Good. Access codes and supplements are not guaranteed with used items. May be an ex-library book. paperback
Features/Photos: Algeria - a cease-fire on paper but not in fact; Marlborough House restored and re-furbished; Princess Margaret is entertained by Cliff Richard; Einstein and the theory of relativity; Restorations at Petra, Jordan; France Nuyen; and more. Moderate wear. Clean and unmarked. Quality copy. Magazine
1330688503.Gpaperback. Good. Access codes and supplements are not guaranteed with used items. May be an ex-library book. paperback
026781416X.Ghardcover. Good. Access codes and supplements are not guaranteed with used items. May be an ex-library book. hardcover
0332493121.Ghardcover. Good. Access codes and supplements are not guaranteed with used items. May be an ex-library book. hardcover
1979202335New Jersey: Princeton University Press 1979. First Edition; First Printing. Hardcover. Near Fine in a Very Good price clipped dust jacket. Princeton University Press hardcover
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200227657New York, 2002. 290 S. mit zahlreichen Abbildungen. 4°. Orig.-Karton.
195056788New York: Didier 1950. good fair to good. 175 DJ somewhat worn and soiled: edge tears creases and small pieces missing DJ in plastic sleeve. Contributors include Stewart Alsop Robert Bacher Hanson W. Baldwin Hans Bethe David E. Lilienthal Walter Lippman Brien McMahon Hans Morgenthau Leo Szilard Harold Urey and Richard K. Winslow. Topics covered include the political significance of the Hydrogen Bomb the military value of the Hydrogen Bomb the scientific problems of building a Hydrogen Bomb and how those problems may be solved and a bold plan for world atomic peace. Didier unknown
1940180281Princeton: Princeton University Press 1940. Elucidating the Einstein-Infeld-Hoffman equations First edition offprint issue of Einstein's last major contribution to the general theory of relativity. It formed part of his mathematical investigations into the structure of the theory which he spent the latter part of his life refining. "During the development of the general theory Einstein had intended to hold fast to the conservation of energy and momentum in the usual special relativistic sense as far as possible. At the same time he was driven by other considerations toward the idea that the laws should be generally covariant. These two desires proved mutually incompatible. The problem of the equation of motion of bodies is the following. The 1916 theory had a classical structure in the sense that there were both field equations the curvature of space-time is determined by the mass and motion of bodies in space-time and equation of motion of bodies the world line of small mass is a geodesic. Einstein showed that if matter is represented by a point singularity of the metric field these singularities are located on world lines that are geodesics of space time provided its metric satisfies the equation of general relativity" DSB IV p. 329. The first part of the paper was published in 1938. Large octavo pp. 10. Original wrappers wire-stitched as issued front cover printed in black. Wrappers gently toned: a near-fine copy. Boni 236.1; Weil 205. unknown
193846954Baltimore Princeton University Press 1938 a.1940. Royal8vo. Bound in 2 full cloth gilt lettering to spines. In: Annals of Mathematics" Series 2 Vol. 39 and vol. 40. Entire volumes offered. The papers: pp. 65-100 a. pp. 455-464. Clean and fine.også on a generalization. pais p. 496 <br/><br/><em>First appearance of these two importent papers on the General theory of Relativity in which is shown that the equation of motion follows directly from the field equation that defined the geometry."Einstein's last importent contribution to general relativity deals again with the problem of motion. It is the work done with Leopold Indfeld and Banesh Hoffmann on the N-body problem of motion. In these papers the gravitational field is no longer treated as external. Instead it and the motion of its singular sources are treated simultaneously. A new approximation scheme is introduced in which the fields are no longer necessarily weak but in which the source velocities are small compared with the light velocity. These equations are widely used in analyses of planetary orbits in the solar system."Pais "Subtle is the Lord" pp. 290-91.Weil: 202 a. 205 both with an asterix denoting a major paper. - Boni: 236 a. 236.1. </em> hardcover
193846475Princeton NJ. Annals of Mathematics 1938 a. 1940. Both papers in orig. printed wrappers. Offprints from "Annals of Mathematics" Vol. 39 No. 1 january 1938 and Vol. 41 No. 2 April 1940. Pp. 65-100 and pp. 455-464. Both clean and fine. This copy has belonged to Abraham Pais 1918-2000 - the famous Einstein scholar theoretical physicist and Einsteins collegue at Princeton - and having his name on top of both frontwrappers "A Pais". <br/><br/><em>First editions in the scarce offprint versions of Einstein's last and highly important contributions to General relativity and in which is shown that the equation of motion follows directly from the field equation that defined the geometry."Einstein's last importent contribution to general relativity deals again with the problem of motion. It is the work done with Leopold Infeld and Banash Hoffmann on the N-body problem of motion. In these papers the gravitational field is no longer treated as external. Instead it and the motion of its singular sources are treated simultaneously. Anew approximationscheme is introduced in which the fields are no longer necessarily weak but in which the source velocities are small compared with the light velocity . The equations obtained have found use in situations where Newtonian interaction must be included. 'These equations are widely used in analyses of planetary orbits in the solarsystem. For example the Cal Tech Jet Propulsion Laboratory uses them in modified form to calculate ephmerides for high-precision tracking of planets and spacecraft."Pais "Subtle is the Lord" p. 290-91."The problem of the equation of motion of bodies is the following. The 1916 theory had a classical structure in the sense that there were both field equations the curvature of space-time is determined by the mass and motion of bodies in space-time and equations of motion of bodies the world line of small mass is a geodesic. Are these two statements really separate If the field equations were linear they indeed would be. They are not linear however and Einstein showed in the papers offered that if matter is represented by a point singularity of the metric field these singularities are located on world lines that are geodesics of space-time provided its metric satisfies the equation of general relativity."DSB.Weil: 202 a. 295 both with an asterix denoting a major paper. - Boni: 236 a. 236.1. </em> unknown
B9781715276942Hardback. New. hardcover
