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Introduction to "Solaris" Translated from Polish by Lech Keller Stanislaw Lem Is Unquestionably One of the Greatest Authors of SF in the Global History of This Genre
Acta Polonica Monashiensis Volume 2 Number 2 December 2002 Wojciech Kajtoch Introduction to "Solaris" Translated from Polish by Lech Keller Stanislaw Lem is unquestionably one of the greatest authors of SF in the global history of this genre. Thus inclusion of his works to the reading list1 is certainly a gesture, which acknowledges the reality. One could also regard this inclusion as an ennoblement of a genre, so far virtually ignored by the school administration because of its "lowly" origin (i.e. Verne's fantastic novels, targeted mostly for young people, and American "pulp" SF magazines of the 1930s). There are also different claims, namely that "Solaris" (and this novel is virtually unanimously regarded as the best work of Lem, the work, which introduced his works to the list of "must-read" books), is not really SF. The main reason is that "Solaris" can be read and interpreted as a psychological novel, thus in this context Lem is a "real", i.e. "mainstream" writer, actually not much interested in science and technology. In short: Lem is strictly speaking a "high brow" writer, rather than a "lowly" SF writer. It should be also noted the lack of regard to the cultural background (or its arbitrary selection), which was frequent in the interpretation of the post-Second World War literature, and common in the Polish secondary schools habit of reading every literary text as a direct reflection and appraisal of the real world. This way we have compiled a catalogue of the dangers threatening analysis of "Solaris', as it is done at the classes of Polish literature. -
Questioning the Techno-Savior
Questioning the Techno-Savior: Interpreting the Effects of Techno-Scientific Expansionism on Twentieth-Century Poland Through the Fiction of Stanislaw Lem Melika Hadziomerovic College of Liberal Arts and Sciences, University of Florida This project examines the fiction of Poland’s most renowned science fiction author, Stanislaw Lem, in order to gain a broader understanding of his interpretations of scientific modernity and technology. It argues that Lem focuses on the ideological properties of modernity in the twentieth century. Lastly, it further relates Poland’s exposure to the techno-scientific regimes of Nazi Germany and Soviet Russia to the genealogy of science fiction in order to gain a better understanding of Lem’s fiction. An inherent assumption of scientific modernity is that vulnerability to imperialistic fervor and its universalizing technology functions in the best and planned interests of approach to human experience. humanity. However, breakthroughs in the field also Lem’s admitted attempts to “reconcile the contradictory tellingly lead to dominion over natural and social orders. elements of realism and fantasy” suggest that a historical- This can be seen in the use of military technology during cultural analysis of his work is appropriate (“Reflections” the twentieth century that has complicated both the 1). We can think of Lem’s fiction as symbolizing historical assumption that scientific mastery always benefits events just as trauma memories (following Freud’s humanity, and the conviction that an invention’s design interpretations) fictionalize events in the traumatized equals its practical implementation. How, then, do cultures psyche. Furthermore, Lem’s intellectual fascination with forcefully introduced to scientific modernity through the hard sciences (both biological and physical) drives him military aggression interpret its instruments? Further, what to analyze the nature of technologically driven regimes and insights do the literary artifacts that discuss and/or human nature empirically. -
N O T I C E This Document Has Been Reproduced From
N O T I C E THIS DOCUMENT HAS BEEN REPRODUCED FROM MICROFICHE. ALTHOUGH IT IS RECOGNIZED THAT CERTAIN PORTIONS ARE ILLEGIBLE, IT IS BEING RELEASED IN THE INTEREST OF MAKING AVAILABLE AS MUCH INFORMATION AS POSSIBLE P993-198422 International Collogium on Atomic Spectra and Oscillator Strengths for Astrophysical and Laboratory Plasmas (4th) Held at the National institute of Standards and Technology Gaithersburg, Maryland on September 14-17, 1992 (U.S.) National inst. of Standards and Technology (PL) Gaithersburg, MD Apr 93 US. DEPARTMENT OF COMMERCE Ndioul Techcical IMermeNON Service B•11G 2-10i1A2 2 MIST-1 /4 U.S. VZPARTMENT OF COMMERCE (REV. NATIONAL INSTITUTE OF STANDARDS AND TECHNOLOGY M GONTSOLw1N^BENN O4" COMM 4M /. MANUSCRIPT REVIEW AND APPROVAL "KIST/ p-850 ^' THIS NSTRUCTWNS: ATTACH ORIGINAL OF FORM TO ONE (1) COPY OF MANUSCIIN IT AND SEINE TO: PUBLICATIOM OATS NUMBER PRINTED PAGES April 1993 199 HE SECRETAIIY, APPROPRIATE EDITO RIAL REVIEW BOARD. ITLE AND SUBTITLE (CITE NN PULL) 4rh International Colloquium on Atomic Spectra and Oscillator Strengths for Astrophysical and Laboratory Plasmas -- POSTER PAPERS :ONTIEACT OR GRANT NUMBER TYPE OF REPORT AND/OR PERIOD COMM UTHOR(S) (LAST %,TAME, POST NNITIAL, SECOND INITIAL) PERFORM" ORGANIZATION (CHECK (IQ ONE SOX) EDITORS XXX MIST/GAITHERSBUIIG Sugar, Jack and Leckrone, B:;vid INST/BODUM JILA BOIRDE11 "ORATORY AND DIVISION NAMES (FIRST MOST AUTHOR ONLY) Physics Laboratory/Atomic Physics Division 'PONSORING ORGANIZATION NAME AND COMPLETE ADDRESS TREET, CITY. STATE. ZNh ^y((S/ ,T AiL7A - -ASO IECOMMENDsO FOR MIST PUBLICATION JOVIAMAL OF RESEMICM (MIST JRES) CIONOGRAPK (MIST MN) LETTER CIRCULAR J. PHYS. A CHEM. -
The Very Young Resolved Stellar Populations Around Stripped-Envelope Supernovae
MNRAS 000,1– ?? (2016) Preprint 22 December 2017 Compiled using MNRAS LATEX style file v3.0 The very young resolved stellar populations around stripped-envelope supernovae Justyn R. Maund?y Department of Physics and Astronomy, University of Sheffield, Hicks Building, Hounsfield Road, Sheffield S3 7RH, U.K. Accepted XXX. Received YYY; in original form ZZZ ABSTRACT The massive star origins for Type IIP supernovae (SNe) have been established through direct detection of their red supergiants progenitors in pre-explosion observations; however, there has been limited success in the detection of the progenitors of H-deficient SNe. The final fate of more massive stars, capable of undergoing a Wolf-Rayet phase, and the origins of Type Ibc SNe remains debated, including the relative importance of single massive star progeni- tors or lower mass stars stripped in binaries. We present an analysis of the ages and spatial distributions of massive stars around the sites of 23 stripped-envelope SNe, as observed with the Hubble Space Telescope, to probe the possible origins of the progenitors of these events. Using a Bayesian stellar populations analysis scheme, we find characteristic ages for the pop- ulations observed within 150 pc of the target Type IIb, Ib and Ic SNe to be log¹tº = 7:20, 7:05 and 6:57, respectively. The Type Ic SNe in the sample are nearly all observed within 100 pc of young, dense stellar populations. The environment around SN 2002ap is an important ex- ception both in terms of age and spatial properties. These findings may support the hypothesis that stars with Minit > 30M produce a relatively large proportion of Type Ibc SNe, and that these SN subtypes arise from progressively more massive progenitors. -
Gone Without a Bang: an Archival HST Survey for Disappearing Massive Stars
MNRAS 453, 2885–2900 (2015) doi:10.1093/mnras/stv1809 Gone without a bang: an archival HST survey for disappearing massive stars Thomas M. Reynolds,1,2‹ Morgan Fraser1 and Gerard Gilmore1 1Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 2Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Vais¨ al¨ antie¨ 20, FI-21500 Piikkio,¨ Finland Downloaded from Accepted 2015 August 4. Received 2015 July 16; in original form 2015 May 27 ABSTRACT It has been argued that a substantial fraction of massive stars may end their lives without http://mnras.oxfordjournals.org/ an optically bright supernova (SN), but rather collapse to form a black hole. Such an event would not be detected by current SN surveys, which are focused on finding bright transients. Kochanek et al. proposed a novel survey for such events, using repeated observations of nearby galaxies to search for the disappearance of a massive star. We present such a survey, using the first systematic analysis of archival Hubble Space Telescope images of nearby galaxies with the aim of identifying evolved massive stars which have disappeared, without an accompanying optically bright SN. We consider a sample of 15 galaxies, with at least three epochs of Hubble Space Telescope imaging taken between 1994 and 2013. Within this data, we find one candidate at CERN - European Organization for Nuclear Research on September 15, 2016 which is consistent with a 25–30 M yellow supergiant which has undergone an optically dark core-collapse. Key words: stars: evolution – stars: massive – supernovae: general. plosion, and Type IIL (Linear) SNe which have a steady decline 1 INTRODUCTION in luminosity from peak. -
Experiencing Hubble
PRESCOTT ASTRONOMY CLUB PRESENTS EXPERIENCING HUBBLE John Carter August 7, 2019 GET OUT LOOK UP • When Galaxies Collide https://www.youtube.com/watch?v=HP3x7TgvgR8 • How Hubble Images Get Color https://www.youtube.com/watch? time_continue=3&v=WSG0MnmUsEY Experiencing Hubble Sagittarius Star Cloud 1. 12,000 stars 2. ½ percent of full Moon area. 3. Not one star in the image can be seen by the naked eye. 4. Color of star reflects its surface temperature. Eagle Nebula. M 16 1. Messier 16 is a conspicuous region of active star formation, appearing in the constellation Serpens Cauda. This giant cloud of interstellar gas and dust is commonly known as the Eagle Nebula, and has already created a cluster of young stars. The nebula is also referred to the Star Queen Nebula and as IC 4703; the cluster is NGC 6611. With an overall visual magnitude of 6.4, and an apparent diameter of 7', the Eagle Nebula's star cluster is best seen with low power telescopes. The brightest star in the cluster has an apparent magnitude of +8.24, easily visible with good binoculars. A 4" scope reveals about 20 stars in an uneven background of fainter stars and nebulosity; three nebulous concentrations can be glimpsed under good conditions. Under very good conditions, suggestions of dark obscuring matter can be seen to the north of the cluster. In an 8" telescope at low power, M 16 is an impressive object. The nebula extends much farther out, to a diameter of over 30'. It is filled with dark regions and globules, including a peculiar dark column and a luminous rim around the cluster. -
Fundamental Properties of Core-Collapse Supernova and GRB Progenitors: Predicting the Look of Massive Stars Before Death
A&A 558, A131 (2013) Astronomy DOI: 10.1051/0004-6361/201321906 & c ESO 2013 Astrophysics Fundamental properties of core-collapse supernova and GRB progenitors: predicting the look of massive stars before death Jose H. Groh1, Georges Meynet1, Cyril Georgy2, and Sylvia Ekström1 1 Geneva Observatory, Geneva University, Chemin des Maillettes 51, 1290 Sauverny, Switzerland e-mail: [email protected] 2 Astrophysics group, EPSAM, Keele University, Lennard-Jones Labs, ST5 5BG Keele, UK Received 16 May 2013 / Accepted 20 August 2013 ABSTRACT We investigate the fundamental properties of core-collapse supernova (SN) progenitors from single stars at solar metallicity. For this purpose, we combine Geneva stellar evolutionary models with initial masses of Mini = 20−120 M with atmospheric and wind models using the radiative transfer code CMFGEN. We provide synthetic photometry and high-resolution spectra of hot stars at the pre-SN stage. For models with Mini = 9−20 M, we supplement our analysis using publicly available MARCS model atmospheres of RSGs to estimate their synthetic photometry. We employ well-established observational criteria of spectroscopic classification and find that, depending on their initial mass and rotation, massive stars end their lives as red supergiants (RSG), yellow hypergiants (YHG), luminous blue variables (LBV), and Wolf-Rayet (WR) stars of the WN and WO spectral types. For rotating models, we obtained the + following types of SN progenitors: WO1–3 (Mini ≥ 32 M), WN10–11 (25 < Mini < 32 M), LBV (20 ≤ Mini ≤ 25 M), G1 Ia (18 < Mini < 20 M), and RSGs (9 ≤ Mini ≤ 18 M). For non-rotating models, we found spectral types WO1–3 (Mini > 40 M), WN7–8 (25 < Mini ≤ 40 M), WN11h/LBV (20 < Mini ≤ 25 M), and RSGs (9 ≤ Mini ≤ 20 M). -
Monthly Newsletter of the Durban Centre - March 2018
Page 1 Monthly Newsletter of the Durban Centre - March 2018 Page 2 Table of Contents Chairman’s Chatter …...…………………….……….………..….…… 3 Andrew Gray …………………………………………...………………. 5 The Hyades Star Cluster …...………………………….…….……….. 6 At the Eye Piece …………………………………………….….…….... 9 The Cover Image - Antennae Nebula …….……………………….. 11 Galaxy - Part 2 ….………………………………..………………….... 13 Self-Taught Astronomer …………………………………..………… 21 The Month Ahead …..…………………...….…….……………..…… 24 Minutes of the Previous Meeting …………………………….……. 25 Public Viewing Roster …………………………….……….…..……. 26 Pre-loved Telescope Equipment …………………………...……… 28 ASSA Symposium 2018 ………………………...……….…......…… 29 Member Submissions Disclaimer: The views expressed in ‘nDaba are solely those of the writer and are not necessarily the views of the Durban Centre, nor the Editor. All images and content is the work of the respective copyright owner Page 3 Chairman’s Chatter By Mike Hadlow Dear Members, The third month of the year is upon us and already the viewing conditions have been more favourable over the last few nights. Let’s hope it continues and we have clear skies and good viewing for the next five or six months. Our February meeting was well attended, with our main speaker being Dr Matt Hilton from the Astrophysics and Cosmology Research Unit at UKZN who gave us an excellent presentation on gravity waves. We really have to be thankful to Dr Hilton from ACRU UKZN for giving us his time to give us presentations and hope that we can maintain our relationship with ACRU and that we can draw other speakers from his colleagues and other research students! Thanks must also go to Debbie Abel and Piet Strauss for their monthly presentations on NASA and the sky for the following month, respectively. -
Orbital Elements of Double Stars
Orbital elements of double stars: ADS 1548 Marco Scardia, Jean-Louis Prieur, Luigi Pansecchi, Robert Argyle, Josefina Ling, Eric Aristidi, Alessio Zanutta, Lyu Abe, Philippe Bendjoya, Jean-Pierre Rivet, et al. To cite this version: Marco Scardia, Jean-Louis Prieur, Luigi Pansecchi, Robert Argyle, Josefina Ling, et al.. Orbital elements of double stars: ADS 1548. 2018, pp.1. hal-02357208 HAL Id: hal-02357208 https://hal.archives-ouvertes.fr/hal-02357208 Submitted on 23 Nov 2019 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. INTERNATIONAL ASTRONOMICAL UNION COMMISSION G1 (BINARY AND MULTIPLE STAR SYSTEMS) DOUBLE STARS INFORMATION CIRCULAR No. 194 (FEBRUARY 2018) NEW ORBITS ADS Name P T e Ω(2000) 2018 Author(s) α2000δ n a i ! Last ob. 2019 1548 A 819 AB 135y4 2011.06 0.548 153◦8 39◦7 000161 SCARDIA 01570+3101 2◦6587 000424 50◦5 189◦7 2017.833 49.4 0.163 et al. (*) - HDS 333 49.54 1981.14 0.60 252.6 253.8 0.542 TOKOVININ 02332-5156 7.2665 0.413 57.4 150.9 2018.073 255.7 0.519 - COU 691 61.76 1964.53 0.059 68.6 276.2 0.109 DOCOBO 03423+3141 5.8290 0.160 -
Arxiv:0908.2624V1 [Astro-Ph.SR] 18 Aug 2009
Astronomy & Astrophysics Review manuscript No. (will be inserted by the editor) Accurate masses and radii of normal stars: Modern results and applications G. Torres · J. Andersen · A. Gim´enez Received: date / Accepted: date Abstract This paper presents and discusses a critical compilation of accurate, fun- damental determinations of stellar masses and radii. We have identified 95 detached binary systems containing 190 stars (94 eclipsing systems, and α Centauri) that satisfy our criterion that the mass and radius of both stars be known to ±3% or better. All are non-interacting systems, so the stars should have evolved as if they were single. This sample more than doubles that of the earlier similar review by Andersen (1991), extends the mass range at both ends and, for the first time, includes an extragalactic binary. In every case, we have examined the original data and recomputed the stellar parameters with a consistent set of assumptions and physical constants. To these we add interstellar reddening, effective temperature, metal abundance, rotational velocity and apsidal motion determinations when available, and we compute a number of other physical parameters, notably luminosity and distance. These accurate physical parameters reveal the effects of stellar evolution with un- precedented clarity, and we discuss the use of the data in observational tests of stellar evolution models in some detail. Earlier findings of significant structural differences between moderately fast-rotating, mildly active stars and single stars, ascribed to the presence of strong magnetic and spot activity, are confirmed beyond doubt. We also show how the best data can be used to test prescriptions for the subtle interplay be- tween convection, diffusion, and other non-classical effects in stellar models. -
Three Editions of the Star Catalogue of Tycho Brahe*
A&A 516, A28 (2010) Astronomy DOI: 10.1051/0004-6361/201014002 & c ESO 2010 Astrophysics Three editions of the star catalogue of Tycho Brahe Machine-readable versions and comparison with the modern Hipparcos Catalogue F. Verbunt1 andR.H.vanGent2,3 1 Astronomical Institute, Utrecht University, PO Box 80 000, 3508 TA Utrecht, The Netherlands e-mail: [email protected] 2 URU-Explokart, Faculty of Geosciences, Utrecht University, PO Box 80 115, 3508 TC Utrecht, The Netherlands 3 Institute for the History and Foundations of Science, PO Box 80 000, 3508 TA Utrecht, The Netherlands Received 6 January 2010 / Accepted 3 February 2010 ABSTRACT Tycho Brahe completed his catalogue with the positions and magnitudes of 1004 fixed stars in 1598. This catalogue circulated in manuscript form. Brahe edited a shorter version with 777 stars, printed in 1602, and Kepler edited the full catalogue of 1004 stars, printed in 1627. We provide machine-readable versions of the three versions of the catalogue, describe the differences between them and briefly discuss their accuracy on the basis of comparison with modern data from the Hipparcos Catalogue. We also compare our results with earlier analyses by Dreyer (1916, Tychonis Brahe Dani Scripta Astronomica, Vol. II) and Rawlins (1993, DIO, 3, 1), finding good overall agreement. The magnitudes given by Brahe correlate well with modern values, his longitudes and latitudes have error distributions with widths of 2, with excess numbers of stars with larger errors (as compared to Gaussian distributions), in particular for the faintest stars. Errors in positions larger than 10, which comprise about 15% of the entries, are likely due to computing or copying errors. -
Université De Montréal Étude De L'étoile Wolf-Rayet Variable WR 46 Dans L'ultraviolet Lointain Et Les Rayons X Par Vince
Université de Montréal Étude de l’étoile Wolf-Rayet variable WR 46 dans l’ultraviolet lointain et les rayons X par Vincent Hénault-Brunet Département de physique Faculté des arts et des sciences Mémoire présenté à la Faculté des études supérieures en vue de l’obtention du grade de Maître ès sciences (M.Sc.) en physique Août, 2009 c Vincent Hénault-Brunet, 2009 ! Université de Montréal Faculté des études supérieures Ce mémoire intitulé: Étude de l’étoile Wolf-Rayet variable WR 46 dans l’ultraviolet lointain et les rayons X présenté par: Vincent Hénault-Brunet a été évalué par un jury composé des personnes suivantes: Pierre Bergeron, président-rapporteur Nicole St-Louis, directrice de recherche Claude Carignan, membre du jury Mémoire accepté le: 11 septembre 2009 i «Il me semble que ce qui est requis est un délicat équilibre entre deux tendances : celle qui nous pousse à scruter de manière inlassablement sceptique toutes les hypothèses qui nous sont soumises et celle qui nous invite à garder une grande ouverture aux idées nouvelles.» - Carl Sagan ii Sommaire L’étoile Wolf-Rayet WR 46 est connue pour sa variabilité complexe sur des échelles de temps relativement courtes de quelques heures et sur des échelles de temps plus longues de plusieurs mois. Des décalages périodiques mais intermittents en vitesse radiale ont déjà été observés dans ses raies d’émission optiques. Plusieurs périodes photométriques ont aussi été mesurées dans le passé. Des pulsations non-radiales, une modulation liée à la rotation rapide, ou encore la présence d’un compagnon de faible masse dont la présence reste à confirmer ont été proposées pour expliquer le comportement de l’étoile sur des échelles de temps de quelques heures.