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UNIVERSITÉ LIBRE DE BRUXELLES DIGITHÈQUE Université libre de Bruxelles ___________________________ Citation APA : Institut international de physique Solvay (1958). La structure et l'évolution de l'univers: onzième Conseil de physique tenu à l'Université de Bruxelles du 9 au 13 juin 1958. Bruxelles: R. Stoops. Disponible à / Available at permalink : https://dipot.ulb.ac.be/dspace/bitstream/2013/234812/3/DL2622637_000_f.pdf ___________________________ (English version below) Cette œuvre littéraire est soumise à la législation belge en matière de droit d’auteur. Elle a été éditée par l’Université libre de Bruxelles et les Instituts Internationaux de Physique et de Chimie Solvay, et numérisée par les Bibliothèques de l’ULB. Malgré tous leurs efforts, les Bibliothèques de l’ULB n’ont pu identifier le titulaire des droits sur l’œuvre ici reproduite. Dans l’hypothèse où le titulaire de droits sur celle-ci s’opposerait à sa mise en ligne, il est invité à prendre immédiatement contact avec la Direction des bibliothèques, à l’adresse [email protected], de façon à régulariser la situation. Les règles d’utilisation des copies numériques des œuvres sont visibles sur le site de DI-fusion http://difusion.ulb.ac.be L’ensemble des documents numérisés par les Bibliothèques de l’ULB sont accessibles à partir du site de la Digithèque http://digitheque.ulb.ac.be _________________________________________________________________________________ This work is protected by the Belgian legislation relating to authors’ rights. It has been edited by the Université libre de Bruxelles and the Solvay International Institutes of Physics and Chemistry, and has been digitized by the Libraries of ULB. Despite all their efforts, the ULB Libraries have not been able to identify the owner of the rights in the work reproduced herein. In the event that the rights holder over this work objects to its posting online, he/she is invited to immediately contact the Director of the Libraries at [email protected], in order to settle the situation. The general terms of use of the present digital copies are visible on DI-fusion website: http://difusion.ulb.ac.be All the documents digitized by the ULB Libraries are accessible from the website of the Digitheque http://digitheque.ulb.ac.be LA STRUCTURE ET L’ÉVOLUTION DE L’UNIVERS INSTITUT INTERNATIONAL DE PHYSIQUE SOLVAY ONZIÈME CONSEIL DE PHYSIQUE tenu à l’Université de Bruxelles du 9 au 13 juin 1958 lA STRUCTURE ET L’ÉVOlUTIOA DE TUNIVERS RAPPORTS ET DISCUSSIONS publiés sous les auspices du Comité Scientifique de l’Institut R. STÔOPS Editeur 76-78, COUDENBERG, BRUXELLES, BELGIQUE 1958 INTRODUCTION LE ONZIÈME CONSEIL DE PHYSIQUE SOLVAY Le XI® Conseil de Physique Solvay s’est tenu à Bruxelles, dans les locaux de l’Université, du lundi 9 au vendredi 13 juin 1958, suivant les dispositions arrêtées par la Commission Administrative, composée comme suit : Président : M. Jules BORDET, prix Nobel. Membres : MM. Ernest-J. SOLVAY, Paul DE GROOTE, Ilya PRIGOGINE. Secrétaire : M. Frans-H. van den DUNGEN. Le Comité Scientifique qui avait arrêté le programme des rapports était formé de : Président : Sir W. Lawrence BRAGG, prix Nobel. Membres : Prof. C.J. GORTER, Prof. C. M0LLER, Prof. J.R. OPPEN­ HEIMER, Prof. W. PAULI, prix Nobel, Prof. Fr. PERRIN. Le septième membre, M. MOTT, avait fait part de son regret de ne pouvoir être présent. Les membres rapporteurs du Conseil étaient : MM. V. A. AMBARTSUMIAN, Academy of Sciences of Armenia. W. BAADE, Mt Wilson and Palomar Observatories. F. HOYLE, St. John’s College. O.B. KLEIN, Stockholm University. G. LEMAITRE, Université de Louvain. A.C.B. LOVELL, Jodrell Bank Experimental Station. J.H. OORT, Sterrewacht te Leiden. A.T. SANDAGE, Mt Wilson and Palomar Observatories. H. C. VAN DE HULST, Sterrewacht te Leiden. VII Les communications de M. A. T. SANDAGE et M. W. BAADE étaient orales. Les membres invités étaient : MM. M. FIERZ, LFniversity of Basle. T. GOLD, Harvard University. O. HECKMANN, Observatory of Hamburg. B.V. KUKARKIN, Sternberg Institute of Moscow. P. LEDOUX, Université de Liège. W.H. Mac CREA, Royal Holloway College. W.W. MORGAN, Yerkes Observatory. L. ROSENFELD, Manchester University. E. SCHATZMAN, Faculté des Sciences de Paris. H. SHAPLEY, Harvard University. P. SWINGS, Université de Liège. J.A. WHEELER, University of Princeton. H. ZANSTRA, University of Amsterdam. H. BONDI, King’s College, London (Secretary) Les membres auditeurs, membres du corps professoral de l’Uni­ versité de Bruxelles étaient ; MM. J. COX, R. DEBEVER, M. DEMEUR, J. GEHENIAU. MM. GOLD, HECKMANN, MORGAN et WHEELER ont présenté des notes écrites. Le Prof. ROSSLAND. de l’Université d’Oslo, n’a pu se joindre aux invités. Le secrétaire a été aidé dans sa tâche par les secrétaires adjoints: Mmes R. PANKOWSKI-FERN, A. PEETERS-SPITAELS, M^e A. HULEUX, MM. Ch. LAFLEUR, J. HOUGARDY, R. VAN GEEN, membres du personnel scientifique de l’Université. Le Conseil Scientifique a chargé le Prof. J. GEHENIAU de diriger l’édition du volume contenant les rapports et discussions; il a été aidé dans cette tâche par M. R. VAN GEEN, assistant à l’Université de Bruxelles. Les Autorités de l’Université ont reçu les membres du Conseil le lundi 9 à 17 heures dans la salle du Conseil. Le jeudi 12, à 21 heures, un dîner a réuni les participants au Resturant de l’Atomium dans le cadre de l’Exposition Universelle de Bruxelles 1958. VIll ACKNOWLEDGEMENT. At the end of the general discussion of Friday, June 13, Dr. Harlow SHAPLEY made this speech : Mr. Chairman, may I hâve a moment for a bénédiction? I desire to assure you and your colleagues on the Solvay Committee that we, your guests, are indeed grateful for the opportunity of convening and conferring. We hâve, of course nothing but enthusiasm for the magical chemistry of Solvay cuisine — enthusiasm for the processing of potables and comestibles. We enjoyed the high living — especially last nights' high feeding in the uppermost bail of the Atomium. Our thanks are also due to Professor F. H. van den Dungen and his assistants for the organisation of the Congress. In particular, our thanks go to you. Sir Lawrence for your sympatheiic management, and for your skill in genially presiding over these sessions. You hâve maintained a neutral — I might say a neutron — pose during the turbulence, during the négative and positive charges and counter- charges, the explosions and implosions of gas and argument. We wish you. Sir Lawrence, you and your colleagues, many more pleasant and useful Solvay Conférences- IX RAPPORTS ET DISCUSSIONS I. GENERAL STATEMENT OF COSMOLOGICAL THEORY i I A à The Primaeval Atom Hypothesis and the problem of the Clusters of Galaxies by G. LEMAITRE This report is divided in three parts. In the first one, we discuss the general aspects of cosmology and point ont their relations with Geometry, quantum theory and even with their inévitable philosophical background. This is donc without any intention to polemize against other points of view than the one which we hâve adopted, but, simply to make clear what are our own assumptions. The second part is an exposition of the successive processes which arise in our cosmology and lead, in the order stated, from cosmic rays to gaseous clouds and then to proto-galaxies, with stars forma­ tion within them, and, finally, to the arrangement of the galaxies in clusters, with large peculiar velocities of their individual galaxies. This makes possible to define what we call the problem of the clusters of galaxies and the third part reports on some results which point towards its solution. 1. GENERAL ASPECTS Space. Cosmology is essentially related to Geometry, and, in fact geo­ metry in its deeper foundations : topology. We may therefore begin with its topogical aspects, both in space and in space-time. 1 The question is : Is physical space a « compact » ? Can it be covered by a finite number of «neighbourhoods » ? One of these neighbourhoods would be the 10® light year accessible to astronomi- cal observation. How can we infer that, beyond this observed neighbourhood there are other ones with similar properties and how can we know if these neighbourhoods are in finite number and so form a finite compact or closed space? One possible attitude of mind, in regard to this problem, is to rely on some « Cosmological Principle » which is dogmatically asserted and adhered to. Such principle would déclaré that any observer, at any place in the universe, would hâve essentially the same image of the universe around him. An opposite way of approaching the problem would be to infer the content of the invisible neighbourhoods, which presumably surround our own one, from indirect conséquences of observed facts. Matter is connected with curvature of space-time. Therefore any evidence that matter exists farther than what we directly know, results in producing the geometrical properties of our neighbour­ hood to larger régions and possibly far enough to close the whole space of finite and not too large radius inferred from the density in our neighbourhood. Some indirect observation of this kind may corne from the cosmic rays or from radio-waves coming from régions inaccessible to our télescopes. As far as I see, the inclination to rely on an a priori principle is related to Leibnitz philosophical attitude which made him to believe that there is some esthetical design in the Universe or even that the Universe is determined as being the best possible one. Of couse, this attitude would not necessary degenerate into mere idealism, with no contact with observation. Conséquences of the principle should be deduced with the hope that they may corne in agreement with observed facts, or, at least, not to be in contradic­ tion with them.
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    Draft version August 10, 2016 Preprint typeset using LATEX style AASTeX6 v. 1.0 FIRST RESULTS FROM THE MADCASH SURVEY: A FAINT DWARF GALAXY COMPANION TO THE LOW MASS SPIRAL GALAXY NGC 2403 AT 3.2 MPC 1 Jeffrey L. Carlin2, David J. Sand3, Paul Price4, Beth Willman2, Ananthan Karunakaran5, Kristine Spekkens5,6, Eric F. Bell7, Jean P. Brodie8, Denija Crnojevic´3, Duncan A. Forbes9, Jonathan Hargis10, Evan Kirby11, Robert Lupton4, Annika H. G. Peter12, Aaron J. Romanowsky8, 13, and Jay Strader14 1Based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. 2LSST and Steward Observatory, 933 North Cherry Avenue, Tucson, AZ 85721, USA; Haverford College, Department of Astronomy, 370 Lancaster Avenue, Haverford, PA 19041, USA; jeff[email protected] 3Texas Tech University, Physics Department, Box 41051, Lubbock, TX 79409-1051, USA 4Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA 5Department of Physics, Engineering Physics and Astronomy, Queen’s University, Kingston, Ontario, Canada, K7L 3N6 6Department of Physics, Royal Military College of Canada, P.O. Box 17000, Station Forces, Kingston, ON K7L 7B4, Canada 7Department of Astronomy, University of Michigan, 1085 South University Ave, Ann Arbor, MI 48109, USA 8University of California Observatories, 1156 High Street, Santa Cruz, CA 95064, USA 9Centre for Astrophysics and Supercomputing, Swinburne University, Hawthorn VIC 3122, Australia 10Space Telescope Science Institute, 3700 San Martin Drive,
  • Astronomy Astrophysics

    Astronomy Astrophysics

    A&A 449, 1233–1242 (2006) Astronomy DOI: 10.1051/0004-6361:20054284 & c ESO 2006 Astrophysics Simulating observable comets III. Real stellar perturbers of the Oort cloud and their output P. A. Dybczynski´ Astronomical Observatory of the A. Mickiewicz University, Słoneczna 36, 60-286 Poznan,´ Poland e-mail: [email protected] Received 30 September 2005 / Accepted 15 November 2005 ABSTRACT Context. This is the third of a series of papers on simulating the mechanisms acting currently on the Oort cloud and producing the observed long-period comets. Aims. In this paper we investigate the influence of current stellar perturbers on the Oort cloud of comets under the simultaneous galactic disk tide. We also analyse the past motion of the observed long-period comets under the same dynamical model to verify the widely used definition of dynamically new comets. Methods. The action of nearby stars and the galactic disk tide on the Oort cloud was simulated. The original orbital elements of all 386 long- period comets of quality classes 1 and 2 were calculated, and their motion was followed numerically for one orbital revolution into the past, down to the previous perihelion. We also simulated the output of the close future pass of GJ 710 through the Oort cloud. Results. The simulated flux of the observable comets resulting from the current stellar and galactic perturbations, as well as the distribution of perihelion direction, was obtained. The same data are presented for the future passage of GJ 710. A detailed description is given of the past evolution of aphelion and perihelion distances of the observed long-period comets.