DOCSLIB.ORG

Stellar Structure and Compact Objects Before 1940: Towards Relativistic

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Stellar Structure and Compact Objects Before 1940: Towards Relativistic EPJ manuscript No. (will be inserted by the editor) Stellar structure and compact objects before 1940: Towards relativistic astrophysics⋆ Luisa Bonolis1,a Max Planck Institut für Wissenschaftsgeschichte, Boltzmannstraße 22, 14195 Berlin, Germany Abstract. Since the mid-1920s, different strands of research used stars as “physics laboratories” for investigating the nature of matter under extreme densities and pressures, impossible to realize on Earth. To trace this process this paper is following the evolution of the concept of a dense core in stars, which was important both for an understand- ing of stellar evolution and as a testing ground for the fast-evolving field of nuclear physics. In spite of the divide between physicists and astrophysicists, some key actors working in the cross-fertilized soil of overlapping but different scientific cultures formulated models and ten- tative theories that gradually evolved into more realistic and structured astrophysical objects. These investigations culminated in the first con- tact with general relativity in 1939, when J. Robert Oppenheimer and his students George Volkoff and Hartland Snyder systematically applied the theory to the dense core of a collapsing neutron star. This pioneer- ing application of Einstein’s theory to an astrophysical compact object can be regarded as a milestone in the path eventually leading to the emergence of relativistic astrophysics in the early 1960s. 1 Introduction Despite its enormous influence on scientific thought in its early years, general relativity experienced a so-called ‘low-watermark period’, going roughly from the mid-1920s to the mid-1950s [Eisenstaedt 1986, Eisenstaedt 1987, Eisenstaedt 2006], during which it remained cut off from the mainstream of physics and was perceived as a sterile, highly formalistic subject. Accompanied by a series of major astrophysical discoveries, the status of General Relativity definitely changed in the 1960s, when it became an extremely vital research stream of theoretical physics. Quasars, the cosmic microwave background radiation, and pulsars — soon identified as rotating neutron stars — led to the recognition that physical processes and astrophysical objects exist in the universe that are understandable only in terms of the general theory of relativity. In providing definitive proof of the existence of neutron stars, the discovery of pulsars arXiv:1703.09991v1 [physics.hist-ph] 29 Mar 2017 and binary X-ray sources, made even plausible the possibility of black holes, entities that had previously existed only in the minds of a few theorists. In raising new challenges to the emerging relativity community, these had of course an important ⋆ Article submitted to the European Physical Journal H a e-mail: [email protected] 2 The European Physical Journal H role in strengthening the process which turned general relativity into a “subdiscipline of physics” [Blum et al. 2015, Blum et al. 2016]. However, the view of a community of relativists magically awakened from its slum- ber by the new astrophysical discoveries is too one-dimensional. As Alexander Blum, Roberto Lalli, and Jürgen Renn have outlined in their historiographical framework exploring the main factors underlying the return of general relativity into the main- stream of physics, a complex series of elements underlying such process must be taken into account: intellectual developments, epistemological problems, technological ad- vances, the characteristics of post-World War II and Cold-War science, as well as the newly emerging institutional settings. Starting from the mid 1950s, further im- plications began to be explored and general relativity gradually came into focus as a physical theory. This framework, in which they propose to speak of a reinvention of general relativity, rather than a renewal, is leading to an understanding of the rein- vention as a result of two main factors: the recognition of the untapped potential of general relativity and an explicit effort at community-building. These two factors al- lowed this formerly dispersed field to benefit from the postwar changes in the science landscape. The dynamics underlined in [Blum et al. 2015] is actually independent from — and prior to — the major astrophysical discoveries of the 1960s. Up to that time, the view prevailed that general relativistic effects were significant only for cosmol- ogy. However, the violent events that seemed to occur in the core of radio galaxies involving enormous energies corresponding to a rest-mass energy of 106 solar masses (M⊙) [Burbidge 1959], the growing field of nuclear astrophysics [Burbidge et al. 1957, Cameron 1958, Burbidge 1962], and the eventful discovery of quasars, had prepared the stage for the emerging awareness at the beginning of the 1960s of physical pro- cesses in which general relativistic effects are dominant and that could release much larger fractions of the rest mass as energy than the small fraction provided by the binding energies of nuclei. Such processes that did seem possible in the framework of general relativity suggested the actual existence of astrophysical objects in the universe satisfying requirements that appeared to be beyond the scope of nuclear physics. The problem of finding the source of the tremendous energy stored in cosmic rays and magnetic fields of some powerful radio galaxies, led to a theory put forward by William Fowler and Fred Hoyle in January 1963. They suggested that exceedingly massive star-like objects probably could exist with masses up to 108 times that of the sun at the center of those galaxies. The gravitational collapse of such supermassive stars could be the driving force behind the great amount of energy emitted by those strong radio sources [Fowler and Hoyle 1963a]. Their opinion was that in the process 7 8 of contraction of a mass of 10 − 10 M⊙ “general relativity must be used” in order to obtain the energies of the strongest “stellar-type” sources [Fowler and Hoyle 1963b, p. 535]. A few months after this proposal, new objects were discovered, having apparently masses of this order of magnitude, dimensions of about a light week, and having a luminosity two orders of magnitude larger than the luminosity of a large galaxy having dimensions a million times larger and containing something like 1011 stars. In particular, the crucial identification of the high redshift of the already known radio source 3C273 [Hazard et al. 1963, Schmidt 1963, Oke 1963] and of the source 3C48 [Greenstein and Matthews 1963], made now even more pressing the problem to explain the mechanism whereby these and other sources that were masquerading as a star and were thus identified as “quasi-stellar” objects, managed to radiate away the energy equivalent of five hundred thousand suns at a very fast rate. The “supermassive stars” suggested by Fowler and Hoyle immediately became an attractive explanation for these new peculiar astrophysical objects, that appeared to Will be inserted by the editor 3 be farther away than most known galaxies but were luminous enough to be observed by optical telescopes. Their enormous luminosity could also sharply change in the course of one week, as analysis of historical plate material of Harvard Observatory showed [Smith and Hoffleit 1963]. As such enormous energies must be emitted by regions less than one light-week across, collapsed objects became candidates for the engine of quasi-stellar radio sources. The intriguing discovery of quasi-stellar radio sources — soon renamed quasars [Chiu 1964, p. 21] — with their large red-shifts and corresponding unprecedented- large radio and optical luminosities, opened up the discussion on a series of exciting questions. Among the problems raised were the following: Were these objects the debris of a gravitational implosion? By what machinery could gravitational energy be converted into radio waves? Would gravitational collapse lead to indefinite contraction and a singularity in space time? If so, how should theoretical assumptions be changed to avoid this catastrophe? [Robinson et al. 1965, Preface]. “The topic was just right for reporting and sorting out observations as well as for theoretical analysis” [Schucking 1989, p. 51]: during the summer 1963, three rel- ativists in Dallas, Ivor Robinson, Alfred Schild, Engelbert Schucking, realized that a conference bridging the gap between the still exotic world of general relativity and the realm of astrophysics, might be well timed, and it would be a perfect occasion to make known the recently created Southwest Center for Advanced Studies. They immediately involved Peter Bergmann, an influential relativist who had been asso- ciated with Einstein at the Institute for Advanced Study in Princeton since 1936, and sent out letters of invitation. Three hundred relativists, optical and radio as- tronomers, and theoretical astrophysicists attended the International Symposium on Quasi-Stellar Sources and Gravitational Collapse [Robinson et al. 1965], the first of the long series of Texas Symposia, which set up the stage merging two seemingly distant fields: general relativity and astrophysics, so distant that the organizers had to invent a new label for this brand new field: “The suspicion existed that quasars might have something to do with relativity and thus might fit into an imaginary discipline combining astronomy with relativity. One of us — Alfred, Ivor or I? — in- vented a catch phrase for this new field of science: relativistic astrophysics [emphasis added]” [Schucking 1989, p. 50]. Robert Oppenheimer was asked to chair the first
Load more

Recommended publications
  • On the Concept of Degenerate Stars: the Case of White Dwarfs
    On the concept of degenerate stars: the case of white dwarfs Michael Rotondo - Istituto di Istruzione Superiore Statale “Pacinotti-Archimede”, Roma - [email protected] Abstract: In this work we briefly review the history of degenerate stars from the first introduction of Fermi-Dirac quantum statistics to the first unified approach of white dwarfs, based on the relativistic generalization of the Feynman-Metropolis-Teller of compressed atoms, which takes into account consistently the gravitational, the weak, the strong and the electromagnetic interactions. Keywords:History of astrophysics, Compact stars, Degenerate Fermi gas 1. Prologue: Adams and Eddington Exactly one century ago Walter S. Adams published a paper entitled “The Spectrum of the Companion of Sirius” in which he concludes that: …the companion of Sirius has a color index not appreciably different from that of the principal star (Adams 1915, p. 237). This conclusion would lead to a dramatic consequence as summarized by Arthur S. Ed- dington: …a ton of [companion of Sirius] material would be a little nugget that you could put in a match-box. What reply can one make to such a message? The reply which most of us made in 1914 was - ‘Shut up. Don’t talk nonsense’ (Eddington 1927, p. 50). Nine years later, in 1924, Eddington published a paper entitled “On the Relation be- tween the Masses and Luminosities of the Stars” in which he suggested a new test to confirm (or reject) the exceptionally high density of the companion of Sirius: …the question could probably be settled by measuring Einstein shift of the spec- trum… (Eddington 1924, p.
    [Show full text]
  • 2019 in the Academic Ranking of World Universities (ARWU)
    THE UNIVERSITY OF MANCHESTER FACTS AND FIGURES 2020 2 The University 4 World ranking 6 Academic pedigree 8 World-class research CONTENTS 10 Students 12 Making a difference 14 Global challenges, Manchester solutions 16 Stellify 18 Graduate careers 20 Staff 22 Faculties and Schools 24 Alumni 26 Innovation 28 Widening participation UNIVERSITY OF MANCHESTER 30 Cultural institutions UNIVERSITY OF MANCHESTER 32 Income 34 Campus investment 36 At a glance 1 THE UNIVERSITY OF MANCHESTER Our vision is to be recognised globally for the excellence of our people, research, learning and innovation, and for the benefits we bring to society and the environment. Our core goals and strategic themes Research and discovery Teaching and learning Social responsibility Our people, our values Innovation Civic engagement Global influence 2 3 WORLD RANKING The quality of our teaching and the impact of our research are the cornerstones of our success. We have risen from 78th in 2004* to 33rd – our highest ever place – in 2019 in the Academic Ranking of World Universities (ARWU). League table World ranking European ranking UK ranking 33 8 6 ARWU 33 8 6 WORLD EUROPE UK QS 27 8 6 Times Higher Education 55 16 8 *2004 ranking refers to the Victoria University of Manchester prior to the merger with UMIST. 4 5 ACADEMIC PEDIGREE 1906 1908 1915 1922 1922 We attract the highest-calibre researchers and teachers, with 25 Nobel Prize winners among J Thomson Ernest Rutherford William Archibald V Hill Niels Bohr Physics Chemistry Larence Bragg Physiology or Medicine Physics our current and former staff and students.
    [Show full text]
  • Rutherford's Nuclear World: the Story of the Discovery of the Nuc
    Rutherford's Nuclear World: The Story of the Discovery of the Nuc... http://www.aip.org/history/exhibits/rutherford/sections/atop-physic... HOME SECTIONS CREDITS EXHIBIT HALL ABOUT US rutherford's explore the atom learn more more history of learn about aip's nuclear world with rutherford about this site physics exhibits history programs Atop the Physics Wave ShareShareShareShareShareMore 9 RUTHERFORD BACK IN CAMBRIDGE, 1919–1937 Sections ← Prev 1 2 3 4 5 Next → In 1962, John Cockcroft (1897–1967) reflected back on the “Miraculous Year” ( Annus mirabilis ) of 1932 in the Cavendish Laboratory: “One month it was the neutron, another month the transmutation of the light elements; in another the creation of radiation of matter in the form of pairs of positive and negative electrons was made visible to us by Professor Blackett's cloud chamber, with its tracks curled some to the left and some to the right by powerful magnetic fields.” Rutherford reigned over the Cavendish Lab from 1919 until his death in 1937. The Cavendish Lab in the 1920s and 30s is often cited as the beginning of modern “big science.” Dozens of researchers worked in teams on interrelated problems. Yet much of the work there used simple, inexpensive devices — the sort of thing Rutherford is famous for. And the lab had many competitors: in Paris, Berlin, and even in the U.S. Rutherford became Cavendish Professor and director of the Cavendish Laboratory in 1919, following the It is tempting to simplify a complicated story. Rutherford directed the Cavendish Lab footsteps of J.J. Thomson. Rutherford died in 1937, having led a first wave of discovery of the atom.
    [Show full text]
  • The Development of Military Nuclear Strategy And
    The Development of Military Nuclear Strategy and Anglo-American Relations, 1939 – 1958 Submitted by: Geoffrey Charles Mallett Skinner to the University of Exeter as a thesis for the degree of Doctor of Philosophy in History, July 2018 This thesis is available for Library use on the understanding that it is copyright material and that no quotation from the thesis may be published without proper acknowledgement. I certify that all material in this thesis which is not my own work has been identified and that no material has previously been submitted and approved for the award of a degree by this or any other University. (Signature) ……………………………………………………………………………… 1 Abstract There was no special governmental partnership between Britain and America during the Second World War in atomic affairs. A recalibration is required that updates and amends the existing historiography in this respect. The wartime atomic relations of those countries were cooperative at the level of science and resources, but rarely that of the state. As soon as it became apparent that fission weaponry would be the main basis of future military power, America decided to gain exclusive control over the weapon. Britain could not replicate American resources and no assistance was offered to it by its conventional ally. America then created its own, closed, nuclear system and well before the 1946 Atomic Energy Act, the event which is typically seen by historians as the explanation of the fracturing of wartime atomic relations. Immediately after 1945 there was insufficient systemic force to create change in the consistent American policy of atomic monopoly. As fusion bombs introduced a new magnitude of risk, and as the nuclear world expanded and deepened, the systemic pressures grew.
    [Show full text]
  • A SURVEY of the YEAR 5687* I. Years, the Question of Compulsory
    A SURVEY OF THE YEAR 5687* BY H. S. LINFIELD, PH.D. I. SPIRITUAL AND INTELLECTUAL LIFE SABBATH AND HOLIDAY OBSERVANCE.—As in previous years, the question of compulsory Sunday observance, a mat- ter of great importance to Jews, continued in 5687 to engage the attention of the Jews in many countries. In the United States, the agitation for compulsory Sunday rest, headed by the Lord's Day Alliance, was apparently on a smaller scale during 1926 than during 1925. In the preceding year, accord- ing to information collected during 1926, the agitation suf- fered a great check. In 1925 two bills providing for com- pulsory Sunday rest were introduced in the Congress and 67 similar bills were introduced in 28 state legislatures. The former died in the committees to which they were referred, and not a single bill introduced in the state legislatures at the instance of the Lord's Day Alliance or of the National Reform Association to Strengthen Existing Sunday Laws passed. On the other hand, some of the states repealed and others liberalized their Sunday laws. A summary of the status of Sunday legislation during 1926 has not yet been published. But the Sixty-ninth Congress had before it six compulsory Sunday Bills, two in the Senate and four in the House, and it is said that about forty bills were introduced in the various state legislatures during 1926. The Sixty- ninth Congress closed without enacting a compulsory Sun- day rest bill for the District of Columbia; this bill, had it been enacted, was to have served as a model Sunday com- pulsory rest bill for all the states.
    [Show full text]
  • USCOURTS-Ca9-07-17209-0.Pdf
    Case: 07-17209 12/09/2008 ID: 6732413 DktEntry: 31-1 Page: 1 of 16 FOR PUBLICATION UNITED STATES COURT OF APPEALS FOR THE NINTH CIRCUIT SOCIETE CIVILE SUCCESSION RICHARD GUINO, a french trust, Plaintiff-Appellee, v. No. 07-15582 JEAN-EMMANUEL RENOIR, an individual, D.C. No. Defendant-Appellant, CV-03-01310-MHM and BESEDER INC., doing business as Rima Fine Art; DROR DAREL, husband; TRACY L. PENWELL, wife, Defendants. SOCIETE CIVILE SUCCESSION RICHARD GUINO, a french trust, Plaintiff-Appellee, v. No. 07-15583 JEAN-EMMANUEL RENOIR, an individual, D.C. No. Defendant, CV-03-01310-MHM and BESEDER INC., doing business as Rima Fine Art; DROR DAREL, husband; TRACY L. PENWELL, wife, Defendants-Appellants. 16111 Case: 07-17209 12/09/2008 ID: 6732413 DktEntry: 31-1 Page: 2 of 16 16112 SOCIETE CIVILE SUCCESSION v. RENOIR SOCIETE CIVILE SUCCESSION RICHARD GUINO, a french trust, Plaintiff-Appellant, RICHARD W. MORRIS; MORRIS LAW FIRM, PLLC, No. 07-17209 Appellants, D.C. No. v. CV-03-01310-MHM JEAN-EMMANUEL RENOIR, an OPINION individual; BESEDER INC., doing business as Rima Fine Art; DROR DAREL, husband; TRACY L. PENWELL, wife, Defendants-Appellees. Appeal from the United States District Court for the District of Arizona Mary H. Murguia, District Judge, Presiding Argued and Submitted October 20, 2008—San Francisco, California Filed December 9, 2008 Before: Mary M. Schroeder, Dorothy W. Nelson and Stephen Reinhardt, Circuit Judges. Opinion by Judge D. W. Nelson Case: 07-17209 12/09/2008 ID: 6732413 DktEntry: 31-1 Page: 3 of 16 16116 SOCIETE CIVILE SUCCESSION v. RENOIR COUNSEL David Steiner and Michael Hambly, Steiner & Associates, PLC, Los Angeles, California, for defendant-appellant- plaintiff-cross-appellee Jean-Emmanuel Renoir.
    [Show full text]
  • Electron-Positron Pairs in Physics and Astrophysics
    Electron-positron pairs in physics and astrophysics: from heavy nuclei to black holes Remo Ruffini1,2,3, Gregory Vereshchagin1 and She-Sheng Xue1 1 ICRANet and ICRA, p.le della Repubblica 10, 65100 Pescara, Italy, 2 Dip. di Fisica, Universit`adi Roma “La Sapienza”, Piazzale Aldo Moro 5, I-00185 Roma, Italy, 3 ICRANet, Universit´ede Nice Sophia Antipolis, Grand Chˆateau, BP 2135, 28, avenue de Valrose, 06103 NICE CEDEX 2, France. Abstract Due to the interaction of physics and astrophysics we are witnessing in these years a splendid synthesis of theoretical, experimental and observational results originating from three fundamental physical processes. They were originally proposed by Dirac, by Breit and Wheeler and by Sauter, Heisenberg, Euler and Schwinger. For almost seventy years they have all three been followed by a continued effort of experimental verification on Earth-based experiments. The Dirac process, e+e 2γ, has been by − → far the most successful. It has obtained extremely accurate experimental verification and has led as well to an enormous number of new physics in possibly one of the most fruitful experimental avenues by introduction of storage rings in Frascati and followed by the largest accelerators worldwide: DESY, SLAC etc. The Breit–Wheeler process, 2γ e+e , although conceptually simple, being the inverse process of the Dirac one, → − has been by far one of the most difficult to be verified experimentally. Only recently, through the technology based on free electron X-ray laser and its numerous applications in Earth-based experiments, some first indications of its possible verification have been reached. The vacuum polarization process in strong electromagnetic field, pioneered by Sauter, Heisenberg, Euler and Schwinger, introduced the concept of critical electric 2 3 field Ec = mec /(e ).
    [Show full text]
  • UC Berkeley Electronic Theses and Dissertations
    UC Berkeley UC Berkeley Electronic Theses and Dissertations Title The Ambivalence of Resistance: West German Antiauthoritarian Performance after the Age of Affluence Permalink https://escholarship.org/uc/item/2c73n9k4 Author Boyle, Michael Shane Publication Date 2012 Peer reviewed|Thesis/dissertation eScholarship.org Powered by the California Digital Library University of California The Ambivalence of Resistance West German Antiauthoritarian Performance after the Age of Affluence By Michael Shane Boyle A dissertation submitted in partial satisfaction of the requirements for the degree of Doctor of Philosophy in Performance Studies in the Graduate Division of the University of California, Berkeley Committee in charge: Professor Shannon Jackson, Chair Professor Anton Kaes Professor Shannon Steen Fall 2012 The Ambivalence of Resistance West German Antiauthoritarian Performance after the Age of Affluence © Michael Shane Boyle All Rights Reserved, 2012 Abstract The Ambivalence of Resistance West German Antiauthoritarian Performance After the Age of Affluence by Michael Shane Boyle Doctor of Philosophy in Performance Studies University of California, Berkeley Professor Shannon Jackson, Chair While much humanities scholarship focuses on the consequence of late capitalism’s cultural logic for artistic production and cultural consumption, this dissertation asks us to consider how the restructuring of capital accumulation in the postwar period similarly shaped activist practices in West Germany. From within the fields of theater and performance studies, “The Ambivalence of Resistance: West German Antiauthoritarian Performance after the Age of Affluence” approaches this question historically. It surveys the types of performance that decolonization and New Left movements in 1960s West Germany used to engage reconfigurations in the global labor process and the emergence of anti-imperialist struggles internationally, from documentary drama and happenings to direct action tactics like street blockades and building occupations.
    [Show full text]
  • Appendix E • Nobel Prizes
    Appendix E • Nobel Prizes All Nobel Prizes in physics are listed (and marked with a P), as well as relevant Nobel Prizes in Chemistry (C). The key dates for some of the scientific work are supplied; they often antedate the prize considerably. 1901 (P) Wilhelm Roentgen for discovering x-rays (1895). 1902 (P) Hendrik A. Lorentz for predicting the Zeeman effect and Pieter Zeeman for discovering the Zeeman effect, the splitting of spectral lines in magnetic fields. 1903 (P) Antoine-Henri Becquerel for discovering radioactivity (1896) and Pierre and Marie Curie for studying radioactivity. 1904 (P) Lord Rayleigh for studying the density of gases and discovering argon. (C) William Ramsay for discovering the inert gas elements helium, neon, xenon, and krypton, and placing them in the periodic table. 1905 (P) Philipp Lenard for studying cathode rays, electrons (1898–1899). 1906 (P) J. J. Thomson for studying electrical discharge through gases and discover- ing the electron (1897). 1907 (P) Albert A. Michelson for inventing optical instruments and measuring the speed of light (1880s). 1908 (P) Gabriel Lippmann for making the first color photographic plate, using inter- ference methods (1891). (C) Ernest Rutherford for discovering that atoms can be broken apart by alpha rays and for studying radioactivity. 1909 (P) Guglielmo Marconi and Carl Ferdinand Braun for developing wireless telegraphy. 1910 (P) Johannes D. van der Waals for studying the equation of state for gases and liquids (1881). 1911 (P) Wilhelm Wien for discovering Wien’s law giving the peak of a blackbody spectrum (1893). (C) Marie Curie for discovering radium and polonium (1898) and isolating radium.
    [Show full text]
  • Facts and Figures 2013
    Facts and Figures 201 3 Contents The University 2 World ranking 4 Academic pedigree 6 Areas of impact 8 Research power 10 Spin-outs 12 Income 14 Students 16 Graduate careers 18 Alumni 20 Faculties and Schools 22 Staff 24 Estates investment 26 Visitor attractions 28 Widening participation 30 At a glance 32 1 The University of Manchester Our Strategic Vision 2020 states our mission: “By 2020, The University of Manchester will be one of the top 25 research universities in the world, where all students enjoy a rewarding educational and wider experience; known worldwide as a place where the highest academic values and educational innovation are cherished; where research prospers and makes a real difference; and where the fruits of scholarship resonate throughout society.” Our core goals 1 World-class research 2 Outstanding learning and student experience 3 Social responsibility 2 3 World ranking The quality of our teaching and the impact of our research are the cornerstones of our success. 5 The Shanghai Jiao Tong University UK Academic Ranking of World ranking Universities assesses the best teaching and research universities, and in 2012 we were ranked 40th in the world. 7 World European UK European Year Ranking Ranking Ranking ranking 2012 40 7 5 2010 44 9 5 2005 53 12 6 2004* 78* 24* 9* 40 Source: 2012 Shanghai Jiao Tong University World Academic Ranking of World Universities ranking *2004 ranking refers to the Victoria University of Manchester prior to the merger with UMIST. 4 5 Academic pedigree Nobel laureates 1900 JJ Thomson , Physics (1906) We attract the highest calibre researchers and Ernest Rutherford , Chemistry (1908) teachers, boasting 25 Nobel Prize winners among 1910 William Lawrence Bragg , Physics (1915) current and former staff and students.
    [Show full text]
  • Alfred O. C. Nier
    CHEMICAL HERITAGE FOUNDATION ALFRED O. C. NIER Transcript of Interviews Conducted by Michael A. Grayson and Thomas Krick at University of Minnesota Minneapolis, Minnesota on 7, 8, 9, and 10 April 1989 (With Subsequent Corrections and Additions) ACKNOWLEDGMENT This oral history is one in a series initiated by the Chemical Heritage Foundation on behalf of the American Society for Mass Spectrometry. The series documents the personal perspectives of individuals related to the advancement of mass spectrometric instrumentation, and records the human dimensions of the growth of mass spectrometry in academic, industrial, and governmental laboratories during the twentieth century. This project is made possible through the generous support of the American Society for Mass Spectrometry Upon Alfred O.C. Nier’s death in 1994, this oral history was designated Free Access. Please note: Users citing this interview for purposes of publication are obliged under the terms of the Chemical Heritage Foundation Oral History Program to credit CHF using the format below: Alfred O.C. Nier, interview by Michael A. Grayson and Thomas Krick at the University of Minnesota, Minneapolis, Minnesota, 7-10 April 1989 (Philadelphia: Chemical Heritage Foundation, Oral History Transcript # 0112). Chemical Heritage Foundation Oral History Program 315 Chestnut Street Philadelphia, Pennsylvania 19106 The Chemical Heritage Foundation (CHF) serves the community of the chemical and molecular sciences, and the wider public, by treasuring the past, educating the present, and inspiring the future. CHF maintains a world-class collection of materials that document the history and heritage of the chemical and molecular sciences, technologies, and industries; encourages research in CHF collections; and carries out a program of outreach and interpretation in order to advance an understanding of the role of the chemical and molecular sciences, technologies, and industries in shaping society.
    [Show full text]
  • Subrahmanyan Chandrasekhar – Geniaalne Astrofüüsik
    Subrahmanyan Chandrasekhar – geniaalne astrofüüsik Sissejuhatus Kuulsin Chandrasekhari nime esimest korda, kui mu sõber ja hilisem kolleeg Tiit Nilson oli saanud veel ülikooliajal – 1962. aastal - oma juhendajaks Juhan Rossi. Tiit näitas mulle Juhani käest saadud vene keelde tõlgitud Chandrasekhari raamatut kiirguslevist, mis oli täis salapäraseid valemeid. Hiljem sai see raamat mullegi väga oluliseks ja 1977. a ostsin selle – inglisekeelsena – Lõuna-California ülikooli raamatupoest Los Angeleses. Sellest ajast on see mu töölauaraamat, ja minuni jõudis arusaamine sellest, et see mees on haruldaselt mitmekülgne suur teadlane. Mingi tõsise probleemi ettevõtnuna avaldas ta terve seeria artikleid probleemi lahenduse kohta ja siis järgnes artikleid kokkuvõttev monograafia. Nii said põhjaliku ülevaate ja lahenduse tähe siseehitus, sh valgete kääbuste ehitus, stellaardünaamika, stohhastilised protsessid, kiirguslevi, negatiivse vesiniku iooni kvantteooria, hüdrodünaamika ja hüdromagnetiline stabiilsus, turbulents, tasakaaluliste objektide tasakaal, üldine relatiivsusteooria, mustade aukude matemaatiline teooria ja põrkuvate gravitatsioonilainete teooria. Lisaks veel Newtoni kuulsa Principia „tõlkimine“ autori geomeetrilisest keelest tänapäevasesse keelde. Mida rohkemat veel ühelt inimeselt nõuda võiks! Lapsepõlv ja perekond Chandrasekhar sündis tolleaegses Briti India (nüüd Pakistani) Punjabi provintsi linnas Lahores 19. oktoobril 1910 Chandrasekhara Subrahmanyan Ayyari (1885-1960) ja tema abikaasa Sitalakshmi (1891-1931) esimese pojana. Kokku
    [Show full text]