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Oppenheimer
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LIVRE A L’ETAT DE NEUF. EXPEDIE SOUS 3 JOURS OUVRES. NUMERO DE SUIVI COMMUNIQUE AVANT ENVOI, EMBALLAGE RENFORCE. EAN:9782924898536
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5 book(s) with the same title
"FEYNMAN, R. P. (+) N. BOHR (+) J. A. WHEELER (+) J. R. OPPENHEIMER (+) H. SNYDER.
Reference : 46900
(1939)
Forces in molecules [Feynman] (+) The mechanism of nuclear fission [N. Bohr. & J. A. Wheeler] ""On continued gravitational contraction"" [J. R. Oppenheimer & H. Snyder]. - [FEYNMAN'S UNDERGRADUATE THESIS & THE FIRST THEORETICAL DESCRIPTION OF A SINGULARITY]
[Lancaster], American Institute of Physics, 1939. Royal8vo. Bound in contemporary full red cloth with gilt lettering to spine. Entire volume of ""The Physical Review"", Volume 56, Second Series, July 1 - December 15, 1939. ""Development Department"" in small gilt lettering to lower part of spine. A very fine and clean copy. [Feynman:] Pp. 340-43. [Bohr & Wheeler:] Pp. 426-50. [Oppenheimer & Snyder:] Pp. 455-59. [Entire volume: X, 1264 pp.].
First printing of three landmark papers, all of seminal importance in history of physics: Feynman's undergraduate thesis at MIT, the intricacies of the fission process, the groundwork for atomic and hydrogen bombs and the forgotten birth of black holes: The first theoretical description of a black hole, the production of a singularity when a sufficiently large neutron star collapses.First printing of ""FORCES IN MOLECULES"" - know known as Feynman-Hellmann theorem - is Feynman's undergraduate thesis at MIT, published when he was just twenty-one, which helped to establish his name in the world of physics. ""This work treated the problem of molecular forces from a thoroughly quantum-mechanical point of view, arriving at a simple means of calculating the energy of a molecular system that continues to guide quantum chemists."" (DSB). ""As Feynman conceived the structure of molecules, forces were the natural ingredients. He saw springlike bonds with varying stiffness, atoms attracting and repelling one another. The usual energy-accounting methods seemed secondhand and euphemistic: [He demonstrated that] the force on an atom's nucleus is no more or less than the electrical force from the surrounding field of charged electrons-the electrostatic force. Once the distribution of charge has been calculated quantum mechanically, then from that point forward quantum mechanics disappears from the picture. The problem becomes classical"" the nuclei can be treated as static points of mass and charge. Feynman's approach applies to all chemical bonds"" (Gleick, The Life and Science of Richard Feynman, P. 54).Oppenheimer and Snyder's ""ON CONTINUED GRAVITATIONAL CONTRACTION"" constitute the very first theoretical prediction of a singularity when a sufficiently large neutron star collapses. This phenomenon was later to be coined as a black hole. ""Had J. Robert Oppenheimer not led the US effort to build the atomic bomb, he might still have been remembered for figuring out how a black hole could form."" (American Physical Society). The paper has by several physics historians been described as the forgotten birth of black holes. ""Oppenheimer and his graduate student George Volkoff presented the first analysis of the formation of a neutron star in a 1939 Physical Review paper titled, ""On Massive Neutron Stars"". Oppenheimer wondered what would happen to a very massive neutron star. The Schwartzschild analysis of General Relativity has a theoretical limit, called the ""Schwartzschild limit"", when the ratio of mass-to-radius of a star is 236,000 times greater than the ratio for our sun. When this limit is exceeded, the Schwartzschild analysis does not yield a solution. Oppenheimer believed that a neutron star could have sufficient mass to exceed this limit. What would happen to it? Oppenheimer and his graduate student Hartland Snyder applied General Relativity theory to a star with sufficient mass and density to exceed the Schwartzschild limit. The Schwartzschild analysis assumed that the size of the star stays constant with time. Oppenheimer and Snyder found that they could achieve a real solution from General Relativity when the Schwartzschild limit is exceeded by assuming that the diameter of the star decreases with time. They presented their analysis in a 1939 Physical Review paper, titled, ""On Continual Gravitational Contraction,"" which concluded with: ""When all thermonuclear sources of energy are exhausted, a sufficiently heavy star will collapse. Unless fission due to rotation, the radiation of mass, or the blowing off of mass by radiation, reduce the star's mass to the order of that of the sun, this contraction will continue indefinitely."" This analysis concluded that when the Schwartzschild limit is exceeded, the star must collapse indefinitely until it reaches a singularity having an infinite density of matter"" (Bjornson, Singularity Predictions of General Relativity, P. 4).The Chandrasekhar / Eddington controvery in the mid 30ies did discuss the fate of neutron stars but the first thoroughly theoretical desciption was first published here. ""THE MECHANISM OF NUCLEAR FISSION"" is the first fully worked out theory of nuclear fission, which laid the groundwork for atomic and hydrogen bombs.""Wheeler's technical mastery of physics is best seen in the classic paper of Bohr and Wheeler. Bohr and Wheeler wrote the paper in Princeton, where Bohr was visiting in the spring of 1939, a few months after the discovery of fission. The paper is a masterpiece of clear thinking and lucid writing. It reveals, at the center of the mystery of fission, a tiny world where everything can be calculated and everything understood. The tiny world is a nucleus of uranium 236, formed when a neutron is freshly captured by a nucleus of uranium 235. The uranium 236 nucleus sits precisely on the border between classical and quantum physics. Seen from the classical point of view, it is a liquid drop composed of a positively charged fluid. The electrostatic force that is trying to split it apart is balanced by the nuclear surface tension that is holding it together. The energy supplied by the captured neutron causes the drop to oscillate in various normal modes that can be calculated classically. Seen from the quantum point of view, the nucleus is a superposition of a variety of quantum states leading to different final outcomes. The final outcome may be a uranium 235 nucleus with a re-emitted neutron, or a uranium 236 nucleus with an emitted gamma-ray, or a pair of fission-fragment nuclei with one or more free neutrons. Bohr and Wheeler calculate the cross-section for fission of uranium 235 by a slow neutron and get the right answer within a factor of two. Their calculation is a marvelous demonstration of the power of classical mechanics and quantum mechanics working together. By studying this process in detail, they show how the complementary views provided by classical and quantum pictures are both essential to the understanding of nature. Without the combined power of classical and quantum concepts, the intricacies of the fission process could never have been understood. Bohr's notion of complementarity is triumphantly vindicated"" (John Archibald Wheeler, Proceedings of the American Philosophical Society 154 (2010)).
"BOHR, N. (+) J. A. WHEELER (+) J. R. OPPENHEIMER (+) H. SNYDER.
Reference : 54015
(1939)
The mechanism of nuclear fission [N. Bohr. & J. A. Wheeler] ""On continued gravitational contraction"" [J. R. Oppenheimer & H. Snyder]. - [THE FIRST THEORETICAL DESCRIPTION OF A SINGULARITY]
Lancaster, American Institute of Physics, 1939. Royal8vo. In the original green printed wrappers. In ""The Physical Review"", Volume 56, Second Series, Number 5, September 1. With cloth back-strip. A quire, affecting both papers, detached but without any loss of paper. A few minor tear throughout, far from affecting text. [Bohr & Wheeler:] Pp. 426-50. [Oppenheimer & Snyder:] Pp. 455-59. [Entire volume: Pp. 387-486].
First printing of two landmark papers, all of seminal importance in history of physics: The intricacies of the fission process, the groundwork for atomic and hydrogen bombs and the forgotten birth of black holes: The first theoretical description of a black hole, the production of a singularity when a sufficiently large neutron star collapses.Oppenheimer and Snyder's ""ON CONTINUED GRAVITATIONAL CONTRACTION"" constitute the very first theoretical prediction of a singularity when a sufficiently large neutron star collapses. This phenomenon was later to be coined as a black hole. ""Had J. Robert Oppenheimer not led the US effort to build the atomic bomb, he might still have been remembered for figuring out how a black hole could form."" (American Physical Society). The paper has by several physics historians been described as the forgotten birth of black holes. ""Oppenheimer and his graduate student George Volkoff presented the first analysis of the formation of a neutron star in a 1939 Physical Review paper titled, ""On Massive Neutron Stars"". Oppenheimer wondered what would happen to a very massive neutron star. The Schwartzschild analysis of General Relativity has a theoretical limit, called the ""Schwartzschild limit"", when the ratio of mass-to-radius of a star is 236,000 times greater than the ratio for our sun. When this limit is exceeded, the Schwartzschild analysis does not yield a solution. Oppenheimer believed that a neutron star could have sufficient mass to exceed this limit. What would happen to it? Oppenheimer and his graduate student Hartland Snyder applied General Relativity theory to a star with sufficient mass and density to exceed the Schwartzschild limit. The Schwartzschild analysis assumed that the size of the star stays constant with time. Oppenheimer and Snyder found that they could achieve a real solution from General Relativity when the Schwartzschild limit is exceeded by assuming that the diameter of the star decreases with time. They presented their analysis in a 1939 Physical Review paper, titled, ""On Continual Gravitational Contraction,"" which concluded with: ""When all thermonuclear sources of energy are exhausted, a sufficiently heavy star will collapse. Unless fission due to rotation, the radiation of mass, or the blowing off of mass by radiation, reduce the star's mass to the order of that of the sun, this contraction will continue indefinitely."" This analysis concluded that when the Schwartzschild limit is exceeded, the star must collapse indefinitely until it reaches a singularity having an infinite density of matter"" (Bjornson, Singularity Predictions of General Relativity, P. 4).The Chandrasekhar / Eddington controvery in the mid 30ies did discuss the fate of neutron stars but the first thoroughly theoretical desciption was first published here. ""THE MECHANISM OF NUCLEAR FISSION"" is the first fully worked out theory of nuclear fission, which laid the groundwork for atomic and hydrogen bombs.""Wheeler's technical mastery of physics is best seen in the classic paper of Bohr and Wheeler. Bohr and Wheeler wrote the paper in Princeton, where Bohr was visiting in the spring of 1939, a few months after the discovery of fission. The paper is a masterpiece of clear thinking and lucid writing. It reveals, at the center of the mystery of fission, a tiny world where everything can be calculated and everything understood. The tiny world is a nucleus of uranium 236, formed when a neutron is freshly captured by a nucleus of uranium 235. The uranium 236 nucleus sits precisely on the border between classical and quantum physics. Seen from the classical point of view, it is a liquid drop composed of a positively charged fluid. The electrostatic force that is trying to split it apart is balanced by the nuclear surface tension that is holding it together. The energy supplied by the captured neutron causes the drop to oscillate in various normal modes that can be calculated classically. Seen from the quantum point of view, the nucleus is a superposition of a variety of quantum states leading to different final outcomes. The final outcome may be a uranium 235 nucleus with a re-emitted neutron, or a uranium 236 nucleus with an emitted gamma-ray, or a pair of fission-fragment nuclei with one or more free neutrons. Bohr and Wheeler calculate the cross-section for fission of uranium 235 by a slow neutron and get the right answer within a factor of two. Their calculation is a marvelous demonstration of the power of classical mechanics and quantum mechanics working together. By studying this process in detail, they show how the complementary views provided by classical and quantum pictures are both essential to the understanding of nature. Without the combined power of classical and quantum concepts, the intricacies of the fission process could never have been understood. Bohr's notion of complementarity is triumphantly vindicated"" (John Archibald Wheeler, Proceedings of the American Philosophical Society 154 (2010)).
Note on the Transmutation Function for Deutrons. [In ""The Physical Review, Volume 48, Second Series, Number 6, September, 1935]. - [FIRST PUBLICATION OF THE OPPENHEIMER-PHILLIPS PROCESS]
Lancaster, American Physical Society, 1935. Lex8vo. Entire volume in the original printed blue/grey wrappers. Minor miscolouring and soiling to extremities. A fine and clean copy. Pp. 500-2. [Entire issue: Pp. 491-572].
First printing of this important paper in which the Oppenheimer-Phillips process was presented for the first time - Oppenheimer's ""most important contribution in this area"" (Oppenheimer. A Life. P. 29).A deuteron, entering a heavy nucleus, is split into proton plus neutron, one of these particles being retained by the nucleus while the other is re-emitted. After the second world war this became a fundamental tool in the study of nuclear energy levels and their properties. Phillips was Oppenheimer's research associate in 1933-4.In ""The Physical Review - The First Hundred Years. A Selection of Seminal Papers and Commentaries"".
"BETHE, H. A. (+) J. R. OPPENHEIMER (+) G. M. VOLKOFF (+) RICHARD TOLMAN.
Reference : 46901
(1939)
Energy Production in Stars (+) On Massive Neutron Cores (+) Neutron Stars and the Tolman-Oppenheimer-Volkov Limit. - [HANS BETHE'S NOBEL PRIZE WINNING PAPER AND GENERAL RELATIVISTIC THEORY OF STELLAR STRUCTURE]
[Lancaster], American Institute of Physics, 1939. Royal8vo. Bound in contemporary full red cloth with gilt lettering to spine. Entire volume of ""The Physical Review"", Volume 55, Second Series, January 1 - June 15, 1939. ""Development Department"" in small gilt lettering to lower part of spine. A very fine and clean copy. [Bethe:] Pp. 434-456. [Oppenheimer & Volkoff:] Pp. 374-381. [Entire volume: 1300 pp.].
First printing of ""ENERGY PRODUCTION IN STARS"", Hans Bethe's seminal Nobel Prize winning paper on neucleosynthesis. It was the first time an astrophysical subject was recognized by the Nobel Committee. Bethe's work on nuclear reactions led him to discover the reactions that supply the energy in stars. In this paper, Bethe shows that ""the most important source of energy in ordinary stars is the reactions of carbon and nitrogen with protons"" (Bethe, Energy Production in Stars). Bethe began by analyzing the different possibilities for reactions by which hydrogen is fused into helium. He showed two processes to be the sources of energy generation capable of keeping stars hot. The first, the proton-proton chain, is the dominant energy source in stars with masses up to about the mass of the Sun. The second, the carbon-nitrogen-oxygen cycle, is the most important in more massive stars. ""ON MASSIVE NEUTRON CORES"" and NEUTRON STARS AND THE TOLMAN-OPPENHEIMER-VOLKOV LIMIT, two landmark papers which ""for the first time laid a general relativistic theory of stellar structure"" (Pais, Subtle is the Lord), thereby proving Einstein wrong in his conclusion that no star could collapse indefinitely.In the paper they addressed the question that Landau's paper, and also Oppenheimer and Serber's, had failed to consider: what is the maximum mass for stable neutron-star? This paper applied Tolman's method to calculate the gravitational equilibrium of a neutron star and predict the conditions under which it will continue collapsing into a black hole (the Tolman-Oppenheimer-Volkov Limit). The issue contain several other papers of interest: 1. Tolman, Richard. ""Static Solutions of Einstein's Field Equations for Spheres of Fluid"" - This paper developed a method for applying Einstein's field equations to static spheres of fluid in such a manner as to facilitate the development of exact solutions using known analytic functions)"" Jenkins and Segre's ""Quadratic Zeeman Effect"" and ""Zeeman Effect of the Forbidden Lines of Potassium"" .2. Gamow & Teller. ""On the Origin of Great Nebulae"". 3. Seaborg & Segre. ""Nuclear Isomerism in Element 43"" 4. Gentner & Segre. ""Appendix on the Calibration of the Ionization Chamber"". 5. Bethe. ""On the Absence of Polarization in Electron Scattering"" & ""Meson Theory of Nuclear Forces.""
Zur Quantentheorie der Molekeln. - [THE BORN-OPPENHEIMER APPROXIMATION]
Leipzig, Ambrosius Barth, 1927. 8vo. In contemporary full cloth with gilt lettering to spine. In ""Annalen der Physik"", Vierte Folge, Band 84. Entire volume offered. Library labels pasted on the pasted down front free end paper. Traces after a label to lower part of spine. Stamp to title page. Internally fine and clean. Pp. 457-484. [Entire volume: 1080, VIII pp.].
First printing of Born and Oppenheimer's famous paper in which the Born-Oppenheimer approximation which is the computation of the energy and the wavefunction of an average-size molecule. It is still an indispensable part of quantum chemistry today.
