The Proceedings of the 1St International Workshop O Laboratory Astrophysics Experiments with Large Lasers
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The Everchanging Pulsating White Dwarf GD358
Astronomy & Astrophysics manuscript no. gd358 January 23, 2003 (DOI: will be inserted by hand later) The Everchanging Pulsating White Dwarf GD358 S.O. Kepler1, R. Edward Nather2, Don E. Winget2, Atsuko Nitta3, S. J. Kleinman3, Travis Metcalfe2;4, Kazuhiro Sekiguchi5, Jiang Xiaojun6, Denis Sullivan7, Tiri Sullivan7, Rimvydas Janulis8, Edmund Meistas8, Romualdas Kalytis8, Jurek Krzesinski9, Waldemar OgÃloza9, Staszek Zola10, Darragh O’Donoghue11, Encarni Romero-Colmenero11, Peter Martinez11, Stefan Dreizler12, Jochen Deetjen12, Thorsten Nagel12, Sonja L. Schuh12, Gerard Vauclair13, Fu Jian Ning13, Michel Chevreton14, Jan-Erik Solheim15, Jose M. Gonzalez Perez15, Frank Johannessen15, Antonio Kanaan16, Jos´eEduardo Costa1, Alex Fabiano Murillo Costa1, Matt A. Wood17, Nicole Silvestri17, T.J. Ahrens17, Aaron Kyle Jones18;¤, Ansley E. Collins19;¤, Martha Boyer20;¤, J. S. Shaw21, Anjum Mukadam2, Eric W. Klumpe22, Jesse Larrison22, Steve Kawaler23, Reed Riddle23, Ana Ulla24, and Paul Bradley25 1 Instituto de F´ısicada UFRGS, Porto Alegre, RS - Brazil e-mail: [email protected] 2 Department of Astronomy & McDonald Observatory, University of Texas, Austin, TX 78712, USA 3 Sloan Digital Sky Survey, Apache Pt. Observatory, P.O. Box 59, Sunspot, NM 88349, USA 4 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 USA e-mail: [email protected] 5 Subaru National Astronomical Observatory of Japan e-mail: [email protected] 6 Beijing Astronomical Observatory, Academy of Sciences, Beijing 100080, China e-mail: [email protected] 7 University of Victoria, Wellington, New Zealand 8 Institute of Theoretical Physics and Astronomy, Gostauto 12, Vilnius 2600, Lithuania 9 Mt. Suhora Observatory, Cracow Pedagogical University, Ul. Podchorazych 2, 30-084 Cracow, Poland 10 Jagiellonian University, Krakow, Poland e-mail: [email protected] 11 South African Astronomical Observatory 12 Universitat T¨ubingen,Germany 13 Universit´ePaul Sabatier, Observatoire Midi-Pyr´en´ees,CNRS/UMR5572, 14 av. -
Arxiv:2001.10147V1
Magnetic fields in isolated and interacting white dwarfs Lilia Ferrario1 and Dayal Wickramasinghe2 Mathematical Sciences Institute, The Australian National University, Canberra, ACT 2601, Australia Adela Kawka3 International Centre for Radio Astronomy Research, Curtin University, Perth, WA 6102, Australia Abstract The magnetic white dwarfs (MWDs) are found either isolated or in inter- acting binaries. The isolated MWDs divide into two groups: a high field group (105 − 109 G) comprising some 13 ± 4% of all white dwarfs (WDs), and a low field group (B < 105 G) whose incidence is currently under investigation. The situation may be similar in magnetic binaries because the bright accretion discs in low field systems hide the photosphere of their WDs thus preventing the study of their magnetic fields’ strength and structure. Considerable research has been devoted to the vexed question on the origin of magnetic fields. One hypothesis is that WD magnetic fields are of fossil origin, that is, their progenitors are the magnetic main-sequence Ap/Bp stars and magnetic flux is conserved during their evolution. The other hypothesis is that magnetic fields arise from binary interaction, through differential rotation, during common envelope evolution. If the two stars merge the end product is a single high-field MWD. If close binaries survive and the primary develops a strong field, they may later evolve into the arXiv:2001.10147v1 [astro-ph.SR] 28 Jan 2020 magnetic cataclysmic variables (MCVs). The recently discovered population of hot, carbon-rich WDs exhibiting an incidence of magnetism of up to about 70% and a variability from a few minutes to a couple of days may support the [email protected] [email protected] [email protected] Preprint submitted to Journal of LATEX Templates January 29, 2020 merging binary hypothesis. -
Eyes for Gamma Rays” Though the Major Peaks Suggest a Periodic- Whether These Are Truly Gamma-Ray Bursts for a Description of This System)
sion of regularity and slow evolution in the They suggested that examination of the Vela exe-atmospheric nuclear detonation. Surpris- universe persisted into the 1960s. data might disclose evidence of bursts of ingly, however, the survey soon revealed that The feeling that transient cosmic events gamma rays at times close to the appearance the gamma-ray instruments on widely sepa- were rare was certainly prevalent in 1959 of supernovae. Such searches were con- rated satellites had sometimes responded when summit meetings were being held be- ducted; however, no distinctive signals were almost identically. Some of these events were tween England, the United States, and found. attributable to solar flare activity. However, Russia to discuss a nuclear test-ban treaty. On the other hand, there was evidence of one particularly distinctive event was dis- One key issue was the ability to detect treaty variability that had been ignored. For exam- covered for which a solar origin seemed violations unambiguously. A leading ple, the earliest x-ray data from small rocket inconsistent. Fortunately, the characteristics proposal for the detection of exo-at- probes and from satellites were often found of this event did not at all resemble those of a mospheric nuclear explosions was the use of to disagree significantly. The quality of the nuclear detonation, and thus the event did satellites with instruments that included de- data, rather than actual variations in the not create concern of a possible test-ban tectors sensitive to the gamma rays emitted sources, was suspected as the reason for treaty violation. by the explosion as well as those emitted these discrepancies. -
Asteroseismology
Asteroseismology Gerald Handler Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland Email: [email protected] Abstract Asteroseismology is the determination of the interior structures of stars by using their oscillations as seismic waves. Simple explanations of the astrophysical background and some basic theoretical considerations needed in this rapidly evolving field are followed by introductions to the most important concepts and methods on the basis of example. Previous and potential applications of asteroseismology are reviewed and future trends are attempted to be foreseen. Introduction: variable and pulsating stars Nearly all the physical processes that determine the structure and evolution of stars occur in their (deep) interiors. The production of nuclear energy that powers stars takes place in their cores for most of their lifetime. The effects of the physical processes that modify the simplest models of stellar evolution, such as mixing and diffusion, also predominantly take place in the inside of stars. The light that we receive from the stars is the main information that astronomers can use to study the universe. However, the light of the stars is radiated away from their surfaces, carrying no memory of its origin in the deep interior. Therefore it would seem that there is no way that the analysis of starlight tells us about the physics going on in the unobservable stellar interiors. However, there are stars that reveal more about themselves than others. Variable stars are objects for which one can observe time-dependent light output, on a time scale shorter arXiv:1205.6407v1 [astro-ph.SR] 29 May 2012 than that of evolutionary changes. -
Weapons-Test Connection by Roger C
COMMENT The Weapons-Test Connection by Roger C. Eckhardt t the test ban summit meetings in 1959, Stirling Colgate from the gamma-ray detectors were searched for enhanced signals in watched the attention of the delegates drifting off the the vicinity of the times of reported supernovae in distant galaxies. technical discussion onto thoughts of wine and women. When these searches proved fruitless, the idea that an unknown and A He refocused their attention with one abrupt question: startlingly different phenomenon might be hiding in the data could Would the gamma rays from a supernova trigger the detectors in the not be examined with high priority by the people involved. During the proposed test-surveillance satellites? With this question, Colgate ten-year span they, instead, pursued an answer to a broader version connected the political goal of test surveillance with the scientific goal of Colgate’s original query: Could a natural background event mimic of understanding cosmic phenomena. In the satellite detection of the signal of an exe-atmospheric weapons test? Although this gamma rays this connection has persisted now for two decades. question was directed primarily toward the political goal, the natural However, it has been perceived in different ways with different scientific drive to eliminate even minor doubts resulted eventually in a consequences by different groups of people. surprise—the discovery of gamma-ray bursts. In truth, the time span At one extreme is the opinion represented by the National was due, not to classification, but to the fact that gamma-ray bursts Enquirer story that claimed gamma-ray bursts were evidence of were totally unexpected. -
CURRICULUM VITAE Name: Matthew A. Wood Address
CURRICULUM VITAE Name: Matthew A. Wood Address: Department of Physics and Astronomy Texas A&M University{Commerce Tel: 903-886-5488 Email: [email protected] Education: Ph.D., Astronomy: The University of Texas at Austin, May 1990 M.A., Astronomy: The University of Texas at Austin, Dec. 1985 B.Sci., Physics: Iowa State University, May 1983 Work Experience: 8/12 { Present Deptartment Head & Professor Department of Physics and Astronomy Texas A&M University{Commerce 8/04 { 7/12 Professor Department of Physics & Space Sciences Florida Institute of Technology 8/96 { 7/04 Associate Professor Florida Institute of Technology 6/91 { 7/96 Assistant Professor Florida Institute of Technology 6/90 { 5/91 NSF{NATO Postdoctoral Fellow D´epartement de Physique Universit´ede Montr´eal Societies: American Astronomical Society International Astronomical Union Royal Astronomical Society Sigma Pi Sigma Florida Academy of Sciences Visiting Scientist: International Ultraviolet Explorer Satellite (NASA/Goddard) Kitt Peak National Observatory Mauna Kea Observatory Keck Observatory Hubble Space Telescope McDonald Observatory Proposal Reviewer: NSF / NASA / NOAO / NOVA (Dutch NSF) Referee: The Astrophysical Journal (Main Journal and Letters) Monthly Notices of the Royal Astronomical Society Astronomy and Astrophysics SCIENCE Publications of the Astronomical Society of the Pacific Astrophysics and Space Science Matthew A. Wood Curriculum Vitae Page 2 Major Grants: PI on grants totaling USD $1.9 million. Selected recent: NASA Kepler Mission (PI) \Cataclysmic Variables -
Sismologie Solaire Et Stellaire Pascal Lambert
Sismologie solaire et stellaire Pascal Lambert To cite this version: Pascal Lambert. Sismologie solaire et stellaire. Astrophysique [astro-ph]. Université Paris-Diderot - Paris VII, 2007. Français. tel-00140766v3 HAL Id: tel-00140766 https://tel.archives-ouvertes.fr/tel-00140766v3 Submitted on 7 Dec 2009 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. École Doctorale d’Astronomie et d’Astrophysique d’Ile-de-France Universite´ Paris VII - Denis Diderot These` de Doctorat présentée pour obtenir le grade de Docteur de l’Université Paris VII - Denis Diderot Spécialité : Astrophysique et Méthodes Associées par Pascal Lambert Sismologie solaire et stellaire Thèse dirigée par Sylvaine TURCK-CHIEZE Soutenue publiquement le 21 mars 2007 devant le jury composé de : Pr. Cécile Ferrari ..........................................Présidente du jury Dr. Rafael A. Garc´ia ..................................... CorrespondantCEA Dr. Eric Michel .................................................Examinateur Dr. Pere L. Palle´ .................................................Rapporteur -
Signature Redacted %
EXAMINATION OF THE UNITED STATES DOMESTIC FUSION PROGRAM ARCHW.$ By MASS ACHUSETTS INSTITUTE Lauren A. Merriman I OF IECHNOLOLGY MAY U6 2015 SUBMITTED TO THE DEPARTMENT OF NUCLEAR SCIENCE AND ENGINEERING I LIBR ARIES IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF BACHELOR OF SCIENCE IN NUCLEAR SCIENCE AND ENGINEERING AT THE MASSACHUSETTS INSTITUTE OF TECHNOLOGY FEBRUARY 2015 Lauren A. Merriman. All Rights Reserved. - The author hereby grants to MIT permission to reproduce and to distribute publicly Paper and electronic copies of this thesis document in whole or in part. Signature of Author:_ Signature redacted %. Lauren A. Merriman Department of Nuclear Science and Engineering May 22, 2014 Signature redacted Certified by:. Dennis Whyte Professor of Nuclear Science and Engineering I'l f 'A Thesis Supervisor Signature redacted Accepted by: Richard K. Lester Professor and Head of the Department of Nuclear Science and Engineering 1 EXAMINATION OF THE UNITED STATES DOMESTIC FUSION PROGRAM By Lauren A. Merriman Submitted to the Department of Nuclear Science and Engineering on May 22, 2014 In Partial Fulfillment of the Requirements for the Degree of Bachelor of Science in Nuclear Science and Engineering ABSTRACT Fusion has been "forty years away", that is, forty years to implementation, ever since the idea of harnessing energy from a fusion reactor was conceived in the 1950s. In reality, however, it has yet to become a viable energy source. Fusion's promise and failure are both investigated by reviewing the history of the United States domestic fusion program and comparing technological forecasting by fusion scientists, fusion program budget plans, and fusion program budget history. -
The Oppenheimer Years 1943-1945 6
" . .When you come right down to it the reason that we did this job is because it was an organic necessity. If you are a scientist you cannot stop such a thing . You believe that it is good to find out how the world works . [and] to turn over to mankind at large the greatest possible power to control the world and to deal with it according to its lights and its values. " . I think it is true to say that atomic weapons are a peril which affect everyone in the world, and in that sense a completely common problem . I think that in order to handle this common problem there must be a complete sense of community responsibility. " . The one point I want to hammer home is what an enormous change in spirit is involved. There are things which we hold very dear, and I think rightly hold very dear; I would say that the word democracy perhaps stood for some of them as well as any other word. There are many parts of the world in which there is no democracy . And when I speak of a new spirit in international affairs I mean that even to these deepest of things which we cherish, and for which Americans have been willing to die—and certainly most of us would be willing to die—even in these deepest things, we realize that there is something more profound than that; namely the common bond with other men everywhere . .“ J. Robert Oppenheimer speech to the Association of Los Alamos Scientists Los Alamos November 2, 1945 Excerpts from a speech to the Association of Los Alamos Scientists in Los Alamos, New Mexico, on November 2, 1945. -
Cover and Contents
All the animal species surrounding the AIDS virus (center) are targets of AIDS-like diseases. The slow viruses, or Ientiviruses, responsible for these diseases attack the cells of the host’s immune system. In the background are T4 cells, the primary target of the AIDS virus. The cells are stained with toluidine blue to identify nucleoproteins. The black dots, produced by radioactive probes, show the location of viral RNA in these infected cells. hy AIDS research at Los outlines the basic dynamics governing models are sadly lacking and often hard Alamos? In 1981 when the the epidemic in the United States. The to collect. Moreover, some data that wfirst AIDS cases were pub- model is based on two unique features have been collected are unavailable. licized, Stirling Colgate, a physicist of the AIDS case data from the Centers Seeing this deficiency, the Los Alamos at Los Alamos, was among those who for Disease Control (CDC). First, the group suggested in a commentary in Na- foresaw that a disease that undermines number of AIDS cases has not grown ture that a national database of complete the human immune system and is trans- exponentially with time (as happens and unfiltered information from diverse mitted through sexual contact could ex- when all members of a population are sources be established and made avail- pand into a worldwide pandemic. The equally at risk) but rather as the cube able to researchers and health officials threat seemed to him nearly as serious of time. Steady cubic growth between involved in surveying and forecasting as the threat of nuclear war, requiring 1982 and 1987 has occurred not only the course of the AIDS epidemic. -
A Brief History of the Co-Evolution of Supernova Theory with Neutrino Physics
A Brief History of the Co-evolution of Supernova Theory with Neutrino Physics Adam Burrows Department of Astrophysical Sciences, Princeton University, Princeton, NJ USA 08544 The histories of core-collapse supernova theory and of neutrino physics have paralleled one another for more than seventy years. Almost every development in neutrino physics necessi- tated modifications in supernova models. What has emerged is a complex and rich dynamical scenario for stellar death that is being progressively better tested by increasingly sophisiti- cated computer simulations. Though there is still much to learn about the agency and details of supernova explosions, whatever final theory emerges will have the neutrino at its core. I summarize in this brief contribution some of the salient developments in neutrino physics as they related to supernova theory, while avoiding any attempt to review the hundreds of pivotal papers that have pushed supernova theory forward. My goal has been merely to highlight the debt of supernova astrophysics to neutrino physics. 1 Introduction The theory of the violent deaths of massive stars in what are called supernova explosions has a long pedigree that spans more than half a century, has engaged hundreds of researchers, and has proven more elusive than anticipated. However, with the advent of numerically and physically sophisticated codes with which to simulate the onset of explosion in three spatial dimensions, the theoretical community now seems to be zeroing in on the mechanism of explosion. Central to this emerging theory are the neutrinos of all species produced copiously at the high densities and temperatures achieved during and after the collapse of the unstable Chandrasekhar core created in the center of the massive star at the end of its life. -
Peculiar Variations of White Dwarf Pulsation Frequencies And
PECULIAR VARIATIONS OF WHITE DWARF PULSATION FREQUENCIES AND MAESTRO by James Ruland Dalessio A dissertation submitted to the Faculty of the University of Delaware in partial fulfillment of the requirements for the degree of Doctor of Philosophy in Physics Spring 2013 c 2013 James Ruland Dalessio All Rights Reserved PECULIAR VARIATIONS OF WHITE DWARF PULSATION FREQUENCIES AND MAESTRO by James Ruland Dalessio Approved: Edmund R. Novak, Ph.D. Chair of the Department of Physics and Astronomy Approved: George H. Watson, Ph.D. Dean of the College of Arts and Sciences Approved: James G. Richards, Ph.D. Vice Provost for Graduate and Professional Education I certify that I have read this dissertation and that in my opinion it meets the academic and professional standard required by the University as a dissertation for the degree of Doctor of Philosophy. Signed: Henry L. Shipman, Ph.D. Professor in charge of dissertation I certify that I have read this dissertation and that in my opinion it meets the academic and professional standard required by the University as a dissertation for the degree of Doctor of Philosophy. Signed: Judith L. Provencal, Ph.D. Member of dissertation committee I certify that I have read this dissertation and that in my opinion it meets the academic and professional standard required by the University as a dissertation for the degree of Doctor of Philosophy. Signed: James MacDonald, Ph.D. Member of dissertation committee I certify that I have read this dissertation and that in my opinion it meets the academic and professional standard required by the University as a dissertation for the degree of Doctor of Philosophy.