A History of the Earth
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Fighting for France's Political Future in the Long Wake of the Commune, 1871-1880
University of Pennsylvania ScholarlyCommons Publicly Accessible Penn Dissertations 2013 Long Live the Revolutions: Fighting for France's Political Future in the Long Wake of the Commune, 1871-1880 Heather Marlene Bennett University of Pennsylvania, [email protected] Follow this and additional works at: https://repository.upenn.edu/edissertations Part of the European History Commons Recommended Citation Bennett, Heather Marlene, "Long Live the Revolutions: Fighting for France's Political Future in the Long Wake of the Commune, 1871-1880" (2013). Publicly Accessible Penn Dissertations. 734. https://repository.upenn.edu/edissertations/734 This paper is posted at ScholarlyCommons. https://repository.upenn.edu/edissertations/734 For more information, please contact [email protected]. Long Live the Revolutions: Fighting for France's Political Future in the Long Wake of the Commune, 1871-1880 Abstract The traumatic legacies of the Paris Commune and its harsh suppression in 1871 had a significant impact on the identities and voter outreach efforts of each of the chief political blocs of the 1870s. The political and cultural developments of this phenomenal decade, which is frequently mislabeled as calm and stable, established the Republic's longevity and set its character. Yet the Commune's legacies have never been comprehensively examined in a way that synthesizes their political and cultural effects. This dissertation offers a compelling perspective of the 1870s through qualitative and quantitative analyses of the influence of these legacies, using sources as diverse as parliamentary debates, visual media, and scribbled sedition on city walls, to explicate the decade's most important political and cultural moments, their origins, and their impact. -
Exomoon Habitability Constrained by Illumination and Tidal Heating
submitted to Astrobiology: April 6, 2012 accepted by Astrobiology: September 8, 2012 published in Astrobiology: January 24, 2013 this updated draft: October 30, 2013 doi:10.1089/ast.2012.0859 Exomoon habitability constrained by illumination and tidal heating René HellerI , Rory BarnesII,III I Leibniz-Institute for Astrophysics Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany, [email protected] II Astronomy Department, University of Washington, Box 951580, Seattle, WA 98195, [email protected] III NASA Astrobiology Institute – Virtual Planetary Laboratory Lead Team, USA Abstract The detection of moons orbiting extrasolar planets (“exomoons”) has now become feasible. Once they are discovered in the circumstellar habitable zone, questions about their habitability will emerge. Exomoons are likely to be tidally locked to their planet and hence experience days much shorter than their orbital period around the star and have seasons, all of which works in favor of habitability. These satellites can receive more illumination per area than their host planets, as the planet reflects stellar light and emits thermal photons. On the contrary, eclipses can significantly alter local climates on exomoons by reducing stellar illumination. In addition to radiative heating, tidal heating can be very large on exomoons, possibly even large enough for sterilization. We identify combinations of physical and orbital parameters for which radiative and tidal heating are strong enough to trigger a runaway greenhouse. By analogy with the circumstellar habitable zone, these constraints define a circumplanetary “habitable edge”. We apply our model to hypothetical moons around the recently discovered exoplanet Kepler-22b and the giant planet candidate KOI211.01 and describe, for the first time, the orbits of habitable exomoons. -
Lomonosov, the Discovery of Venus's Atmosphere, and Eighteenth Century Transits of Venus
Journal of Astronomical History and Heritage, 15(1), 3-14 (2012). LOMONOSOV, THE DISCOVERY OF VENUS'S ATMOSPHERE, AND EIGHTEENTH CENTURY TRANSITS OF VENUS Jay M. Pasachoff Hopkins Observatory, Williams College, Williamstown, Mass. 01267, USA. E-mail: [email protected] and William Sheehan 2105 SE 6th Avenue, Willmar, Minnesota 56201, USA. E-mail: [email protected] Abstract: The discovery of Venus's atmosphere has been widely attributed to the Russian academician M.V. Lomonosov from his observations of the 1761 transit of Venus from St. Petersburg. Other observers at the time also made observations that have been ascribed to the effects of the atmosphere of Venus. Though Venus does have an atmosphere one hundred times denser than the Earth’s and refracts sunlight so as to produce an ‘aureole’ around the planet’s disk when it is ingressing and egressing the solar limb, many eighteenth century observers also upheld the doctrine of cosmic pluralism: believing that the planets were inhabited, they had a preconceived bias for believing that the other planets must have atmospheres. A careful re-examination of several of the most important accounts of eighteenth century observers and comparisons with the observations of the nineteenth century and 2004 transits shows that Lomonosov inferred the existence of Venus’s atmosphere from observations related to the ‘black drop’, which has nothing to do with the atmosphere of Venus. Several observers of the eighteenth-century transits, includ- ing Chappe d’Auteroche, Bergman, and Wargentin in 1761 and Wales, Dymond, and Rittenhouse in 1769, may have made bona fide observations of the aureole produced by the atmosphere of Venus. -
British Persian Studies and the Celebrations of the 2500Th Anniversary of the Founding of the Persian Empire in 1971
British Persian Studies and the Celebrations of the 2500th Anniversary of the Founding of the Persian Empire in 1971 A thesis submitted to The University of Manchester for the degree of Master of Philosophy in the Faculty of Humanities. 2014 Robert Steele School of Arts, Languages and Cultures Contents Abstract ........................................................................................................................................................................ 4 Declaration .................................................................................................................................................................. 5 Copyright Statement ................................................................................................................................................ 5 Acknowledgements .................................................................................................................................................. 6 Introduction .......................................................................................................................................................................... 7 Objectives and Structure ............................................................................................................................................. 8 Literature Review .......................................................................................................................................................... 9 Statement on Primary Sources............................................................................................................................... -
Lecture 6: Galaxy Dynamics (Basic) Elliptical Galaxy Dynamics
Lecture 6: Galaxy Dynamics (Basic) • Basic dynamics of galaxies – Ellipticals, kinematically hot random orbit systems – Spirals, kinematically cool rotating system • Key relations: – The fundamental plane of ellipticals/bulges – The Faber-Jackson relation for ellipticals/bulges – The Tully-Fisher for spirals disks • Using FJ and TF to calculate distances – The extragalactic distance ladder – Examples 1 Elliptical galaxy dynamics • Ellipticals are triaxial spheroids • No rotation, no flattened plane • Typically we can measure a velocity dispersion, σ – I.e., the integrated motions of the stars • Dynamics analogous to a gravitational bound cloud of gas (I.e., an isothermal sphere). • I.e., dp GM(r)ρ(r) HYDROSTATIC − = EQUILIBRIUM dr r2 Check Wikipedia “Hydrostatic PRESSURE FORCE GRAVITATIONAL FORCE Equilibrium” to see PER UNIT VOLUME PER UNIT VOLUME deriiation. € 2 1 Elliptical galaxy dynamics • For an isothermal sphere gas pressure is given by: 2 Reminder from p = ρ(r)σ Thermodynamics: P=nRT/V=ρT, 1 E=(3/2)kT=(1/2)mv^2 ρ(r) ∝ r2 σ 2 GM(r) 2 ⇒ 3 ∝ 4 2σ r r r M(r) = G M(r) ∝σ 2r € 3 € Elliptical galaxy dynamics • As E/S0s are centrally concentrated if σ is measured over sufficient area M(r)=>M, I.e., Total Mass ∝σ 2r • σ is measured from either: – Radial velocity distributions from individual stellar spectra – From line widths€ in integrated galaxy spectra [See Galactic Astronomy, Binney & Merrifield for details on how these are measured in practice] 4 2 Elliptical galaxy dynamices • We have three measureable quantities: – L = luminosity (or magnitude) – Re = effective or half-light radius – σ = velocity dispersion • From these we can derive Σο the central surface brightness (nb: one of these four is redundant as its calculable from the others.) • How are these related observationally and theoretically ? x y • I.e., what does: L ∝ Σ o σ ν look like ? Σο Log logL THE FUNDAMENTAL PLANE € Logσ 5 Fundamental Plane Theory 2 (I.e., stars behaving as if isothermal sphere) IF σν ∝ M Re 2 Surf. -
Isolated Elliptical Galaxies in the Local Universe
A&A 588, A79 (2016) Astronomy DOI: 10.1051/0004-6361/201527844 & c ESO 2016 Astrophysics Isolated elliptical galaxies in the local Universe I. Lacerna1,2,3, H. M. Hernández-Toledo4 , V. Avila-Reese4, J. Abonza-Sane4, and A. del Olmo5 1 Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Av. V. Mackenna 4860, Santiago, Chile e-mail: [email protected] 2 Centro de Astro-Ingeniería, Pontificia Universidad Católica de Chile, Av. V. Mackenna 4860, Santiago, Chile 3 Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany 4 Instituto de Astronomía, Universidad Nacional Autónoma de México, A.P. 70-264, 04510 México D. F., Mexico 5 Instituto de Astrofísica de Andalucía IAA – CSIC, Glorieta de la Astronomía s/n, 18008 Granada, Spain Received 26 November 2015 / Accepted 6 January 2016 ABSTRACT Context. We have studied a sample of 89 very isolated, elliptical galaxies at z < 0.08 and compared their properties with elliptical galaxies located in a high-density environment such as the Coma supercluster. Aims. Our aim is to probe the role of environment on the morphological transformation and quenching of elliptical galaxies as a function of mass. In addition, we elucidate the nature of a particular set of blue and star-forming isolated ellipticals identified here. Methods. We studied physical properties of ellipticals, such as color, specific star formation rate, galaxy size, and stellar age, as a function of stellar mass and environment based on SDSS data. We analyzed the blue and star-forming isolated ellipticals in more detail, through photometric characterization using GALFIT, and infer their star formation history using STARLIGHT. -
Reginald Victor Jones CH FRS (1911-1997)
Catalogue of the papers and correspondence of Reginald Victor Jones CH FRS (1911-1997) by Alan Hayward NCUACS catalogue no. 95/8/00 R.V. Jones 1 NCUACS 95/8/00 Title: Catalogue of the papers and correspondence of Reginald Victor Jones CH FRS (1911-1997), physicist Compiled by: Alan Hayward Description level: Fonds Date of material: 1928-1998 Extent of material: 230 boxes, ca 5000 items Deposited in: Churchill Archives Centre, Churchill College, Cambridge CB3 0DS Reference code: GB 0014 2000 National Cataloguing Unit for the Archives of Contemporary Scientists, University of Bath. NCUACS catalogue no. 95/8/00 R.V. Jones 2 NCUACS 95/8/00 The work of the National Cataloguing Unit for the Archives of Contemporary Scientists, and the production of this catalogue, are made possible by the support of the Research Support Libraries Programme. R.V. Jones 3 NCUACS 95/8/00 NOT ALL THE MATERIAL IN THIS COLLECTION MAY YET BE AVAILABLE FOR CONSULTATION. ENQUIRIES SHOULD BE ADDRESSED IN THE FIRST INSTANCE TO: THE KEEPER OF THE ARCHIVES CHURCHILL ARCHIVES CENTRE CHURCHILL COLLEGE CAMBRIDGE R.V. Jones 4 NCUACS 95/8/00 LIST OF CONTENTS Items Page GENERAL INTRODUCTION 6 SECTION A BIOGRAPHICAL A.1 - A.302 12 SECTION B SECOND WORLD WAR B.1 - B.613 36 SECTION C UNIVERSITY OF ABERDEEN C.1 - C.282 95 SECTION D RESEARCH TOPICS AND SCIENCE INTERESTS D.1 - D.456 127 SECTION E DEFENCE AND INTELLIGENCE E.1 - E.256 180 SECTION F SCIENCE-RELATED INTERESTS F.1 - F.275 203 SECTION G VISITS AND CONFERENCES G.1 - G.448 238 SECTION H SOCIETIES AND ORGANISATIONS H.1 - H.922 284 SECTION J PUBLICATIONS J.1 - J.824 383 SECTION K LECTURES, SPEECHES AND BROADCASTS K.1 - K.495 450 SECTION L CORRESPONDENCE L.1 - L.140 495 R.V. -
Warfare in a Fragile World: Military Impact on the Human Environment
Recent Slprt•• books World Armaments and Disarmament: SIPRI Yearbook 1979 World Armaments and Disarmament: SIPRI Yearbooks 1968-1979, Cumulative Index Nuclear Energy and Nuclear Weapon Proliferation Other related •• 8lprt books Ecological Consequences of the Second Ihdochina War Weapons of Mass Destruction and the Environment Publish~d on behalf of SIPRI by Taylor & Francis Ltd 10-14 Macklin Street London WC2B 5NF Distributed in the USA by Crane, Russak & Company Inc 3 East 44th Street New York NY 10017 USA and in Scandinavia by Almqvist & WikseH International PO Box 62 S-101 20 Stockholm Sweden For a complete list of SIPRI publications write to SIPRI Sveavagen 166 , S-113 46 Stockholm Sweden Stoekholol International Peace Research Institute Warfare in a Fragile World Military Impact onthe Human Environment Stockholm International Peace Research Institute SIPRI is an independent institute for research into problems of peace and conflict, especially those of disarmament and arms regulation. It was established in 1966 to commemorate Sweden's 150 years of unbroken peace. The Institute is financed by the Swedish Parliament. The staff, the Governing Board and the Scientific Council are international. As a consultative body, the Scientific Council is not responsible for the views expressed in the publications of the Institute. Governing Board Dr Rolf Bjornerstedt, Chairman (Sweden) Professor Robert Neild, Vice-Chairman (United Kingdom) Mr Tim Greve (Norway) Academician Ivan M£ilek (Czechoslovakia) Professor Leo Mates (Yugoslavia) Professor -
Planets Transiting Non-Eclipsing Binaries
A&A 570, A91 (2014) Astronomy DOI: 10.1051/0004-6361/201323112 & c ESO 2014 Astrophysics Planets transiting non-eclipsing binaries David V. Martin1 and Amaury H. M. J. Triaud2;? 1 Observatoire Astronomique de l’Université de Genève, Chemin des Maillettes 51, CH-1290 Sauverny, Switzerland e-mail: [email protected] 2 Kavli Institute for Astrophysics & Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA Received 22 November 2013 / Accepted 28 August 2014 ABSTRACT The majority of binary stars do not eclipse. Current searches for transiting circumbinary planets concentrate on eclipsing binaries, and are therefore restricted to a small fraction of potential hosts. We investigate the concept of finding planets transiting non-eclipsing binaries, whose geometry would require mutually inclined planes. Using an N-body code we explore how the number and sequence of transits vary as functions of observing time and orbital parameters. The concept is then generalised thanks to a suite of simulated circumbinary systems. Binaries are constructed from radial-velocity surveys of the solar neighbourhood. They are then populated with orbiting gas giants, drawn from a range of distributions. The binary population is shown to be compatible with the Kepler eclipsing binary catalogue, indicating that the properties of binaries may be as universal as the initial mass function. These synthetic systems produce transiting circumbinary planets occurring on both eclipsing and non-eclipsing binaries. Simulated planets transiting eclipsing binaries are compared with published Kepler detections. We find 1) that planets transiting non-eclipsing binaries are probably present in the Kepler data; 2) that observational biases alone cannot account for the observed over-density of circumbinary planets near the stability limit, which implies a physical pile-up; and 3) that the distributions of gas giants orbiting single and binary stars are likely different. -
Is a Global Identity Possible? the Relevance of Big History to Self-Other Relations”, Refugee Watch, (13):36, 2010, Pp.53-77
On The Possibility of a Global Political Community: The Enigma of ‘Small Local Differences’ within Humanity1 Heikki Patomäki Introduction Is anything like a global political community – and thereby ideals such as global democracy and justice – achievable? This is a key question not only for political theory but also for contemporary political practices. For instance, a call for global solidarity in the face of rapid global warming (UNDP 2007), which seems ever more urgent in 2017, assumes a shared planetary identity across the currently prevailing differences and divisions. It seems that there can be no solidarity without a common identity at some level of human being. Environmentalists maintain that all humans share an important thing in common, namely planet Earth and its sphere of life, to which we essentially belong. In contrast, many political realists believe that humans are essentially tribal beings, or at least will remain so in the foreseeable future. This belief may be grounded on anything from speculative philosophical accounts of the human nature to sociobiological theories 1 This paper has been in progress for a decade. I first wrote it in 2007 and presented it in a few conferences, workshops and the like, including the Calcutta Research Group Winter School in December 2007. That presentation led eventually to a limited-circulation publication “Is a Global Identity Possible? The Relevance of Big History to Self-Other Relations”, Refugee Watch, (13):36, 2010, pp.53-77. A couple of years later I used the last two sections of this paper in a revised form in “The Problems of Legitimation and Potential Conflicts in a World Political Community”, Cooperation & Conflict, (47):2, 2012, pp.239-59. -
Modeling and Interpretation of the Ultraviolet Spectral Energy Distributions of Primeval Galaxies
Ecole´ Doctorale d'Astronomie et Astrophysique d'^Ile-de-France UNIVERSITE´ PARIS VI - PIERRE & MARIE CURIE DOCTORATE THESIS to obtain the title of Doctor of the University of Pierre & Marie Curie in Astrophysics Presented by Alba Vidal Garc´ıa Modeling and interpretation of the ultraviolet spectral energy distributions of primeval galaxies Thesis Advisor: St´ephane Charlot prepared at Institut d'Astrophysique de Paris, CNRS (UMR 7095), Universit´ePierre & Marie Curie (Paris VI) with financial support from the European Research Council grant `ERC NEOGAL' Composition of the jury Reviewers: Alessandro Bressan - SISSA, Trieste, Italy Rosa Gonzalez´ Delgado - IAA (CSIC), Granada, Spain Advisor: St´ephane Charlot - IAP, Paris, France President: Patrick Boisse´ - IAP, Paris, France Examinators: Jeremy Blaizot - CRAL, Observatoire de Lyon, France Vianney Lebouteiller - CEA, Saclay, France Dedicatoria v Contents Abstract vii R´esum´e ix 1 Introduction 3 1.1 Historical context . .4 1.2 Early epochs of the Universe . .5 1.3 Galaxytypes ......................................6 1.4 Components of a Galaxy . .8 1.4.1 Classification of stars . .9 1.4.2 The ISM: components and phases . .9 1.4.3 Physical processes in the ISM . 12 1.5 Chemical content of a galaxy . 17 1.6 Galaxy spectral energy distributions . 17 1.7 Future observing facilities . 19 1.8 Outline ......................................... 20 2 Modeling spectral energy distributions of galaxies 23 2.1 Stellar emission . 24 2.1.1 Stellar population synthesis codes . 24 2.1.2 Evolutionary tracks . 25 2.1.3 IMF . 29 2.1.4 Stellar spectral libraries . 30 2.2 Absorption and emission in the ISM . 31 2.2.1 Photoionization code: CLOUDY ....................... -
Arxiv:1704.01678V2 [Astro-Ph.GA] 28 Jul 2017 Been Notoriously Difficult, Resulting Mostly in Upper Lim- Highest Escape Fractions Measured to Date Among Low- Its (E.G
Submitted: 3 March 2017 Preprint typeset using LATEX style AASTeX6 v. 1.0 MRK 71 / NGC 2366: THE NEAREST GREEN PEA ANALOG Genoveva Micheva1, M. S. Oey1, Anne E. Jaskot2, and Bethan L. James3 (Accepted 24 July 2017) 1University of Michigan, 311 West Hall, 1085 S. University Ave, Ann Arbor, MI 48109-1107, USA 2Department of Astronomy, Smith College, Northampton, MA 01063, USA 3STScI, 3700 San Martin Drive, Baltimore, MD 21218, USA ABSTRACT We present the remarkable discovery that the dwarf irregular galaxy NGC 2366 is an excellent analog of the Green Pea (GP) galaxies, which are characterized by extremely high ionization parameters. The similarities are driven predominantly by the giant H II region Markarian 71 (Mrk 71). We compare the system with GPs in terms of morphology, excitation properties, specific star-formation rate, kinematics, absorption of low-ionization species, reddening, and chemical abundance, and find consistencies throughout. Since extreme GPs are associated with both candidate and confirmed Lyman continuum (LyC) emitters, Mrk 71/NGC 2366 is thus also a good candidate for LyC escape. The spatially resolved data for this object show a superbubble blowout generated by mechanical feedback from one of its two super star clusters (SSCs), Knot B, while the extreme ionization properties are driven by the . 1 Myr-old, enshrouded SSC Knot A, which has ∼ 10 times higher ionizing luminosity. Very massive stars (> 100 M ) may be present in this remarkable object. Ionization-parameter mapping indicates the blowout region is optically thin in the LyC, and the general properties also suggest LyC escape in the line of sight.