DOCSLIB.ORG

Commission 27 of the Iau Information Bulletin

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Commission 27 of the Iau Information Bulletin COMMISSION 27 OF THE I.A.U. INFORMATION BULLETIN ON VARIABLE STARS Nos. 2401 - 2500 1983 September - 1984 March EDITORS: B. SZEIDL AND L. SZABADOS, KONKOLY OBSERVATORY 1525 BUDAPEST, Box 67, HUNGARY HU ISSN 0374-0676 CONTENTS 2401 A POSSIBLE CATACLYSMIC VARIABLE IN CANCER Masaaki Huruhata 20 September 1983 2402 A NEW RR-TYPE VARIABLE IN LEO Masaaki Huruhata 20 September 1983 2403 ON THE DELTA SCUTI STAR BD +43d1894 A. Yamasaki, A. Okazaki, M. Kitamura 23 September 1983 2404 IQ Vel: IMPROVED LIGHT-CURVE PARAMETERS L. Kohoutek 26 September 1983 2405 FLARE ACTIVITY OF EPSILON AURIGAE? I.-S. Nha, S.J. Lee 28 September 1983 2406 PHOTOELECTRIC OBSERVATIONS OF 20 CVn Y.W. Chun, Y.S. Lee, I.-S. Nha 30 September 1983 2407 MINIMUM TIMES OF THE ECLIPSING VARIABLES AH Cep AND IU Aur Pavel Mayer, J. Tremko 4 October 1983 2408 PHOTOELECTRIC OBSERVATIONS OF THE FLARE STAR EV Lac IN 1980 G. Asteriadis, S. Avgoloupis, L.N. Mavridis, P. Varvoglis 6 October 1983 2409 HD 37824: A NEW VARIABLE STAR Douglas S. Hall, G.W. Henry, H. Louth, T.R. Renner 10 October 1983 2410 ON THE PERIOD OF BW VULPECULAE E. Szuszkiewicz, S. Ratajczyk 12 October 1983 2411 THE UNIQUE DOUBLE-MODE CEPHEID CO Aur E. Antonello, L. Mantegazza 14 October 1983 2412 FLARE STARS IN TAURUS A.S. Hojaev 14 October 1983 2413 BVRI PHOTOMETRY OF THE ECLIPSING BINARY QX Cas Thomas J. Moffett, T.G. Barnes, III 17 October 1983 2414 THE ABSOLUTE MAGNITUDE OF AZ CANCRI William P. Bidelman, D. Hoffleit 17 October 1983 2415 NEW DATA ABOUT THE APSIDAL MOTION IN THE SYSTEM OF RU MONOCEROTIS D.Ya. Martynov 18 October 1983 2416 V LIGHT CURVE OF CC COMAE G.V. Zhukov 18 October 1983 2417 SPECTROSCOPIC INVESTIGATION OF SZ Lyn AND SS Psc G.A. Garbuzov 18 October 1983 2418 INACTIVE STATE OF MV LYRAE I.L. Andronov, S.Yu. Shugarov 18 October 1983 2419 HD 34409 - A DELTA SCUTI VARIABLE R.K. Srivastava, A.K. Arya 19 October 1983 2420 TWO NEW VARIABLE STARS IN THE FIELD OF NGC 6946 G. Romano, M. Perissinotto 19 October 1983 2421 NOTE OF THE SEMI-REGULAR VARIABLE TT Scl P.S. The 24 October 1983 2422 FT LUPI: STUDY OF THE PERIOD AND LIGHT CURVE S.L. Lipari, R.F. Sistero 24 October 1983 2423 V1057 CYGNI Gunnar Welin 25 October 1983 2424 PHOTOELECTRIC MINIMA TIMES OF BX ANDROMEDAE P. Rovithis, H. Rovithis-Livaniou 1 November 1983 2425 DETERMINATION OF CEPHEID DISTANCES BY MEANS OF WESENHEIT FUNCTION Antoni Opolski 1 November 1983 2426 AD Leo FLARE MONITORING Richard B. Herr, J.D. Frank 2 November 1983 2427 PHOTOELECTRIC HalphaW OBSERVATIONS OF R CMa M.T. Edalati, B. Khalesse, N. Riazi 2 November 1983 2428 NEW OBSERVATIONS OF HZ Her V.V. Hambarian, G.H. Broutian CORRIGENDUM 8 November 1983 2429 PHOTOMETRIC STUDY OF IO ANDROMEDAE I.L. Andronov 9 November 1983 2430 ON THE CYCLE LENGTH OF THE CATACLYSMIC VARIABLE T LEONIS W. Wenzel 9 November 1983 2431 SUDDEN BRIGHTENING OF THE RECENTLY DISCOVERED Be STAR HR 7739 K. Pavlovski, H. Bozic, P. Harmanec, J. Horn, P. Koubsky 14 November 1983 2432 POLARIMETRY OF Be STARS IN THE OPEN CLUSTER NGC 6611 L.A.S. Reis, E. Janot-Pachecho 18 November 1983 2433 A NEW PROBABLE FLARE STAR N. Sanduleak 23 November 1983 2434 ANOTHER SEMI-REGULAR VARIABLE IN CYGNUS G. Auner, H. Hartl, R. Weinberger 25 November 1983 2435 ON THE VARIABILITY OF THE STAR SAO 072799 P.G. Niarchos 25 November 1983 2436 ON THE PERIOD OF BD Cir Silvano F. Marton, A. Grieco 28 November 1983 2437 PHOTOELECTRIC OBSERVATIONS OF UV CETI M.K. Tsvetkov, L.N. Mavridis, G.A. Asteriadis 29 November 1983 2438 PERIODIC LIGHT VARIABILITY OF PG1711+336 A.V. Mironov, V.G. Moshkalev, S.Yu. Shugarov 30 November 1983 2439 V417 AQUILAE: PHOTOELECTRIC OBSERVATIONS AND IMPROVED PERIOD Danny R. Faulkner 2 December 1983 2440 V3876 Sgr, A MIRA STAR, NOT A NOVA Emilia P. Belserene 5 December 1983 2441 PHOTOMETRIC VARIATIONS IN THE Ap STAR HD 215441 M. Corbin 5 December 1983 2442 PHOTOELECTRIC OBSERVATIONS OF R CrB D. Bohme 9 December 1983 2443 REMARKS ON THREE VARIABLE STARS Thomas Berthold 9 December 1983 2444 EPSILON AURIGAE Eugenio E. Mendoza V. 13 December 1983 2445 POLARIMETRIC OBSERVATIONS OF Be STARS L.A.S. Reis, E. Janot-Pachecho 14 December 1983 2446 THE HBeta EMISSION OF PU Vul Liu Zongli, Hao Xiangliang 16 December 1983 2447 THE Be BINARY HR 2142: NO 0.13m BRIGHTNESS DECREASE IN JANUARY 1983 P. Harmanec, J. Horn, P. Koubsky, K. Pavlovski, H. Bozic, J. Ziznovsky, J.R. Percy 16 December 1983 2448 A NOTE ON X TRIANGULI P. Rovithis, H. Rovithis-Livaniou 20 December 1983 2449 X-RAY VARIABLE STARS IN THE PLEIADES S. Sciortino, G. Micela, S. Serio, G.S. Vaiana, L. Golub, F.R. Harnden, Jr., R. Rosner 20 December 1983 2450 FLARE LIKE ACTIVITY IN AR LACERTAE R.K. Srivastava 23 December 1983 2451 PHOTOELECTRIC TIMES OF MINIMA OF ECLIPSING VARIABLES P.G. Niarchos 23 December 1983 2452 ACTIVE AND INACTIVE STATES OF THE X-RAY BINARY 4U 2129+47 = V1727 CYGNI W. Wenzel 27 December 1983 2453 VARIABLE STAR TIMINGS FROM ARIZONA Andrew P. Odell, F. Dorchak, K. Rogalski, S. Tapia, W.Z. Wisniewski, D.H. Smith 27 December 1983 2454 HD 104901B AN F-TYPE SUPERGIANT ECLIPSING BINARY Olin J. Eggen 28 December 1983 2455 Halpha VARIABILITY IN ALPHA LYRAE P.S. Goraya, M. Singh 30 December 1983 2456 CO Aur - DOUBLE MODE CHARACTER CONFIRMED B. Fuhrmann, R.H. Schult 2 January 1984 2457 NEW PHOTOELECTRIC MINIMA TIMES OF VW CEPHEI P. Rovithis, H. Rovithis-Livaniou 4 January 1984 2458 A DATABASE FOR RS CVn BINARY STAR SYSTEMS E. Nelson, M. Zeilik 6 January 1984 2459 THE LONG TIME BEHAVIOUR OF THE POLAR AM Her IN 1983 W. Gotz 10 January 1984 2460 ON THE DELTA SCUTI-LIKE VARIABILITY OF THE Ap STAR HD 10088 Tobias J. Kreidl 16 January 1984 2461 THE LIGHT CURVE OF FG Vul IN 1983 W. Gotz 18 January 1984 2462 ON THE SX Phe-TYPE STARS M.S. Frolov, B.N. Irkaev 20 January 1984 2463 NEW DATA ON THE MOST RECENT MINIMUM OF THE X-RAY SOURCE KR Aur Martha H. Liller, M.D. Popova 20 January 1984 2464 REVISED PHOTOMETRIC RESULTS OF SAO 072799 P.G. Niarchos 24 January 1984 2465 NARROW BAND PHOTOMETRY OF FG Vir P. Lopez de Coca, R. Garrido, V. Costa, A. Rolland 27 January 1984 2466 WEAKENING OF HBeta EMISSION OF PU Vul Liu Zongli, Hao Xiangliang 30 January 1984 2467 FURTHER OBSERVATIONS OF THE CENTRAL STAR IN THE PLANETARY NEBULA NGC 2346 Brian F. Marino, H.O. Williams, W.S.G. Walker 1 February 1984 2468 THE ORBITAL PERIOD AND PHOTOGRAPHIC LIGHT CURVE OF THE ECLIPSING BINARY V339 Per E.H. Geyer, F. Gieseking 3 February 1984 2469 PERIOD CHANGE OF THE ECLIPSING BINARY IM AURIGAE O. Gulmen, C. Sezer, N. Gudur 6 February 1984 2470 OUTBURST OF VY Aqr IN 1983 Masaaki Huruhata 6 February 1984 2471 POSSIBLE DISCOVERY OF REPEATING OSCILLATIONS IN THE BRIGHTNESS OF BY DRACONIS ON TIMESCALES OF 1-3 HOURS P.F. Chugainov 7 February 1984 2472 LACK OF DETECTION OF A 1.77 h -PERIODICITY IN THE CP STAR HD 32633 Tobias J. Kreidl 8 February 1984 2473 EPOCHS OF MINIMUM LIGHT, DISPLACED SECONDARY ECLIPSE OF SW LACERTAE Danny R. Faulkner, E.E. Evans III, D.H. Grossoehme, E.J. Moyer, Jr. 8 February 1984 2474 NEW OBSERVATIONS OF CN ANDROMEDAE E.J. Michaels, N.L. Markworth, J.B. Rafert 8 February 1984 2475 PERIODIC LIGHT CURVE VARIATIONS OF RT LACERTAE S. Evren, C. Ibanoglu, Z. Tunca, O. Tumer 9 February 1984 2476 NEW VARIABLE STARS IN THE Gamma CYGNI REGION Katya P. Tsvetkova 10 February 1984 2477 ON THE PERIOD OF BH CENTAURI Tibor J. Herczeg 13 February 1984 2478 ON THE PERIODS OFF RZ COMAE AND V1073 CYGNI Zeki Aslan, T.J. Herczeg 13 February 1984 2479 ON THE PERIOD OF THE W UMa SYSTEM Epsilon CrA J. Manfroid, M. Lunel, J. Bergeat, P. Bouchet 15 February 1984 2480 THE PHASE BEHAVIOUR OF THE GENEVA Z AND DELTA(V1-G) PARAMETERS FOR 41 Tau, 56 Tau AND 49 Cnc M. Muciek, J. Gertner, P. North, F.G. Rufener 17 February 1984 2481 ON THE NATURE OF THE CATACLYSMIC BINARY V2051 OPHIUCHI W. Wenzel 22 February 1984 2482 A FLARE-LIKE EVENT ON THE LIGHT CURVE OF V351 Ori G.U. Kovalchuk 24 February 1984 2483 FO And - PROBABLY A NEW MEMBER OF THE SU UMa SUB-GROUP OF DWARF NOVAE L. Meinunger 29 February 1984 2484 PHOTOELECTRIC OBSERVATIONS OF THE FLARE STAR UV Cet IN OCTOBER 1983 I.V. Ilyin 1 March 1984 2485 THE ECLIPSE OF THE SYMBIOTIC ECLIPSING BINARY SYSTEM CI CYGNI IN 1982 T.S. Belyakina 5 March 1984 2486 THE DISCOVERY OF A W URSAE MAJORIS VARIABLE IN THE VISUAL BINARY SYSTEM ADS 9019 R.L. Walker 6 March 1984 2487 PHOTOELECTRIC OBSERVATIONS OF THE EW-VARIABLE VZ Psc E. Poretti 6 March 1984 2488 IMPROVED POSITIONS FOR 15 CATACLYSMIC VARIABLE STARS Alan L. Kiplinger 7 March 1984 2489 NEW DOUBLE-LINED ECLIPSING BINARIES FOUND WITH RETICON, DIGICON, AND CCD DETECTORS Claud H. Lacy 7 March 1984 2490 IMPROVED OUTBURST LIGHT CURVES OF THE NOVAE EY Aql, BC Cas, MT Cen, AND V745 Sco H.W. Duerbeck 7 March 1984 2491 HIGHLY EXCITED EMISSION LINES IN BX Mon AND ZZ CMi T. Iijima 13 March 1984 2492 A CLOSE ECLIPSING BINARY SYSTEM IN CYGNUS S.Yu.
Load more

Recommended publications
  • The Dunhuang Chinese Sky: a Comprehensive Study of the Oldest Known Star Atlas
    25/02/09JAHH/v4 1 THE DUNHUANG CHINESE SKY: A COMPREHENSIVE STUDY OF THE OLDEST KNOWN STAR ATLAS JEAN-MARC BONNET-BIDAUD Commissariat à l’Energie Atomique ,Centre de Saclay, F-91191 Gif-sur-Yvette, France E-mail: [email protected] FRANÇOISE PRADERIE Observatoire de Paris, 61 Avenue de l’Observatoire, F- 75014 Paris, France E-mail: [email protected] and SUSAN WHITFIELD The British Library, 96 Euston Road, London NW1 2DB, UK E-mail: [email protected] Abstract: This paper presents an analysis of the star atlas included in the medieval Chinese manuscript (Or.8210/S.3326), discovered in 1907 by the archaeologist Aurel Stein at the Silk Road town of Dunhuang and now held in the British Library. Although partially studied by a few Chinese scholars, it has never been fully displayed and discussed in the Western world. This set of sky maps (12 hour angle maps in quasi-cylindrical projection and a circumpolar map in azimuthal projection), displaying the full sky visible from the Northern hemisphere, is up to now the oldest complete preserved star atlas from any civilisation. It is also the first known pictorial representation of the quasi-totality of the Chinese constellations. This paper describes the history of the physical object – a roll of thin paper drawn with ink. We analyse the stellar content of each map (1339 stars, 257 asterisms) and the texts associated with the maps. We establish the precision with which the maps are drawn (1.5 to 4° for the brightest stars) and examine the type of projections used.
    [Show full text]
  • Galaxies – AS 3011
    Galaxies – AS 3011 Simon Driver [email protected] ... room 308 This is a Junior Honours 18-lecture course Lectures 11am Wednesday & Friday Recommended book: The Structure and Evolution of Galaxies by Steven Phillipps Galaxies – AS 3011 1 Aims • To understand: – What is a galaxy – The different kinds of galaxy – The optical properties of galaxies – The hidden properties of galaxies such as dark matter, presence of black holes, etc. – Galaxy formation concepts and large scale structure • Appreciate: – Why galaxies are interesting, as building blocks of the Universe… and how simple calculations can be used to better understand these systems. Galaxies – AS 3011 2 1 from 1st year course: • AS 1001 covered the basics of : – distances, masses, types etc. of galaxies – spectra and hence dynamics – exotic things in galaxies: dark matter and black holes – galaxies on a cosmological scale – the Big Bang • in AS 3011 we will study dynamics in more depth, look at other non-stellar components of galaxies, and introduce high-redshift galaxies and the large-scale structure of the Universe Galaxies – AS 3011 3 Outline of lectures 1) galaxies as external objects 13) large-scale structure 2) types of galaxy 14) luminosity of the Universe 3) our Galaxy (components) 15) primordial galaxies 4) stellar populations 16) active galaxies 5) orbits of stars 17) anomalies & enigmas 6) stellar distribution – ellipticals 18) revision & exam advice 7) stellar distribution – spirals 8) dynamics of ellipticals plus 3-4 tutorials 9) dynamics of spirals (questions set after
    [Show full text]
  • A Concise Dictionary of Middle English
    A Concise Dictionary of Middle English A. L. Mayhew and Walter W. Skeat A Concise Dictionary of Middle English Table of Contents A Concise Dictionary of Middle English...........................................................................................................1 A. L. Mayhew and Walter W. Skeat........................................................................................................1 PREFACE................................................................................................................................................3 NOTE ON THE PHONOLOGY OF MIDDLE−ENGLISH...................................................................5 ABBREVIATIONS (LANGUAGES),..................................................................................................11 A CONCISE DICTIONARY OF MIDDLE−ENGLISH....................................................................................12 A.............................................................................................................................................................12 B.............................................................................................................................................................48 C.............................................................................................................................................................82 D...........................................................................................................................................................122
    [Show full text]
  • The Solar System
    5 The Solar System R. Lynne Jones, Steven R. Chesley, Paul A. Abell, Michael E. Brown, Josef Durech,ˇ Yanga R. Fern´andez,Alan W. Harris, Matt J. Holman, Zeljkoˇ Ivezi´c,R. Jedicke, Mikko Kaasalainen, Nathan A. Kaib, Zoran Kneˇzevi´c,Andrea Milani, Alex Parker, Stephen T. Ridgway, David E. Trilling, Bojan Vrˇsnak LSST will provide huge advances in our knowledge of millions of astronomical objects “close to home’”– the small bodies in our Solar System. Previous studies of these small bodies have led to dramatic changes in our understanding of the process of planet formation and evolution, and the relationship between our Solar System and other systems. Beyond providing asteroid targets for space missions or igniting popular interest in observing a new comet or learning about a new distant icy dwarf planet, these small bodies also serve as large populations of “test particles,” recording the dynamical history of the giant planets, revealing the nature of the Solar System impactor population over time, and illustrating the size distributions of planetesimals, which were the building blocks of planets. In this chapter, a brief introduction to the different populations of small bodies in the Solar System (§ 5.1) is followed by a summary of the number of objects of each population that LSST is expected to find (§ 5.2). Some of the Solar System science that LSST will address is presented through the rest of the chapter, starting with the insights into planetary formation and evolution gained through the small body population orbital distributions (§ 5.3). The effects of collisional evolution in the Main Belt and Kuiper Belt are discussed in the next two sections, along with the implications for the determination of the size distribution in the Main Belt (§ 5.4) and possibilities for identifying wide binaries and understanding the environment in the early outer Solar System in § 5.5.
    [Show full text]
  • 10. Scientific Programme 10.1
    10. SCIENTIFIC PROGRAMME 10.1. OVERVIEW (a) Invited Discourses Plenary Hall B 18:00-19:30 ID1 “The Zoo of Galaxies” Karen Masters, University of Portsmouth, UK Monday, 20 August ID2 “Supernovae, the Accelerating Cosmos, and Dark Energy” Brian Schmidt, ANU, Australia Wednesday, 22 August ID3 “The Herschel View of Star Formation” Philippe André, CEA Saclay, France Wednesday, 29 August ID4 “Past, Present and Future of Chinese Astronomy” Cheng Fang, Nanjing University, China Nanjing Thursday, 30 August (b) Plenary Symposium Review Talks Plenary Hall B (B) 8:30-10:00 Or Rooms 309A+B (3) IAUS 288 Astrophysics from Antarctica John Storey (3) Mon. 20 IAUS 289 The Cosmic Distance Scale: Past, Present and Future Wendy Freedman (3) Mon. 27 IAUS 290 Probing General Relativity using Accreting Black Holes Andy Fabian (B) Wed. 22 IAUS 291 Pulsars are Cool – seriously Scott Ransom (3) Thu. 23 Magnetars: neutron stars with magnetic storms Nanda Rea (3) Thu. 23 Probing Gravitation with Pulsars Michael Kremer (3) Thu. 23 IAUS 292 From Gas to Stars over Cosmic Time Mordacai-Mark Mac Low (B) Tue. 21 IAUS 293 The Kepler Mission: NASA’s ExoEarth Census Natalie Batalha (3) Tue. 28 IAUS 294 The Origin and Evolution of Cosmic Magnetism Bryan Gaensler (B) Wed. 29 IAUS 295 Black Holes in Galaxies John Kormendy (B) Thu. 30 (c) Symposia - Week 1 IAUS 288 Astrophysics from Antartica IAUS 290 Accretion on all scales IAUS 291 Neutron Stars and Pulsars IAUS 292 Molecular gas, Dust, and Star Formation in Galaxies (d) Symposia –Week 2 IAUS 289 Advancing the Physics of Cosmic
    [Show full text]
  • A Magnetar Model for the Hydrogen-Rich Super-Luminous Supernova Iptf14hls Luc Dessart
    A&A 610, L10 (2018) https://doi.org/10.1051/0004-6361/201732402 Astronomy & © ESO 2018 Astrophysics LETTER TO THE EDITOR A magnetar model for the hydrogen-rich super-luminous supernova iPTF14hls Luc Dessart Unidad Mixta Internacional Franco-Chilena de Astronomía (CNRS, UMI 3386), Departamento de Astronomía, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chile e-mail: [email protected] Received 2 December 2017 / Accepted 14 January 2018 ABSTRACT Transient surveys have recently revealed the existence of H-rich super-luminous supernovae (SLSN; e.g., iPTF14hls, OGLE-SN14-073) that are characterized by an exceptionally high time-integrated bolometric luminosity, a sustained blue optical color, and Doppler- broadened H I lines at all times. Here, I investigate the effect that a magnetar (with an initial rotational energy of 4 × 1050 erg and 13 field strength of 7 × 10 G) would have on the properties of a typical Type II supernova (SN) ejecta (mass of 13.35 M , kinetic 51 56 energy of 1:32 × 10 erg, 0.077 M of Ni) produced by the terminal explosion of an H-rich blue supergiant star. I present a non-local thermodynamic equilibrium time-dependent radiative transfer simulation of the resulting photometric and spectroscopic evolution from 1 d until 600 d after explosion. With the magnetar power, the model luminosity and brightness are enhanced, the ejecta is hotter and more ionized everywhere, and the spectrum formation region is much more extended. This magnetar-powered SN ejecta reproduces most of the observed properties of SLSN iPTF14hls, including the sustained brightness of −18 mag in the R band, the blue optical color, and the broad H I lines for 600 d.
    [Show full text]
  • Scientific Papers of Lizhi Fang Chinese-English Bilingual Subject List
    Scientific Papers of Lizhi Fang Chinese-English Bilingual Subject List 方勵之先生科學論文中外對照目錄* 編者1：楊建 王樹軍 漢譯審校者1：馮瓏瓏 1961 1. 用變形的傳播函數計算核子電荷半徑,王允然(方勵之),《物理學報》,1961, 17(1):57-60 . Calculation of nucleon electric radius by corrected propagation function, Y.R. Wang (i.e. L.Z. Fang), Acta Physica Sinica(ISSN 1000-3290), 1961, 17, 57 1963 2. 鐵磁體中缺陷對自旋波的影響,李蔭遠,方勵之,顧世傑,《物理學報》,1963, 19 (9):599-612 . Effect of imperfections on spin waves in ferromagnetic, Y.Y. Li, L.Z. Fang and S.J. Gu, Acta Physica Sinica (ISSN 1000-3290), 1963, 19, 599 3. 有缺陷鐵磁體的中子非彈性散射,方勵之,顧世傑,《物理學報》, 1963, 19(10):673-681 . Inelastic scattering of neutrons in ferromagnetics with imperfections, L. Z. Fang and S.J. Gu, Acta Physica Sinica (ISSN 1000-3290), 1963, 19, 673 1964 4. 論三能級變頻器,方勵之,李鐵城,《物理學報》,1964, 20(12):1199-1209 . Theory of three-level frequency converters, L.Z. Fang and T.C. Li, Acta Physica Sinica (ISSN 1000-3290), 1964, 20, 1199 5. 分子在失調腔中的輻射行為及雙腔Maser的振蕩現象,李鐵城,方勵之,《物理學報》,1964, 20(8):753-760 . On the radiation of molecules in detuned cavity and the phenomena of double-cavity masers, T.C. Li and L.Z. Fang, Acta Physica Sinica (ISSN 1000-3290), 1964, 20, 753 6. 金屬表面反射光中的諧波,方勵之,《物理學報》,1964, 20(8):817-818 . Harmonic waves from the reflection at metallic surface, L.Z. Fang, Acta Physica Sinica (ISSN 1000-3290), 1964, 20, 817 7. 關於光激射器的線寬,方勵之,羅一祖,《物理學報》,1964, 20(11):1079-1089 . On the linewidth of lasers, L.Z. Fang and Y.Z. Luo, Acta Physica Sinica (ISSN 1000-3290), 1964, 20, 1079 1965 1 編校者簡介—— 楊 建：原中國科學院南京紫金山天文台專家，曾任江蘇省天文學會副理事長，現定居於澳大利亞； 王樹軍：1980年代在中國科大师从方勵之研習近代物理學史，現在美國威州Merge Healthcare從事軟件開發； 馮瓏瓏：1980年代在中國科大師從方勵之研習天體物理學，現為中國科學院南京紫金山天文台研究員。 8.
    [Show full text]
  • Evolution of Thermally Pulsing Asymptotic Giant Branch Stars
    The Astrophysical Journal, 822:73 (15pp), 2016 May 10 doi:10.3847/0004-637X/822/2/73 © 2016. The American Astronomical Society. All rights reserved. EVOLUTION OF THERMALLY PULSING ASYMPTOTIC GIANT BRANCH STARS. V. CONSTRAINING THE MASS LOSS AND LIFETIMES OF INTERMEDIATE-MASS, LOW-METALLICITY AGB STARS* Philip Rosenfield1,2,7, Paola Marigo2, Léo Girardi3, Julianne J. Dalcanton4, Alessandro Bressan5, Benjamin F. Williams4, and Andrew Dolphin6 1 Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA 2 Department of Physics and Astronomy G. Galilei, University of Padova, Vicolo dell’Osservatorio 3, I-35122 Padova, Italy 3 Osservatorio Astronomico di Padova—INAF, Vicolo dell’Osservatorio 5, I-35122 Padova, Italy 4 Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA 5 Astrophysics Sector, SISSA, Via Bonomea 265, I-34136 Trieste, Italy 6 Raytheon Company, 1151 East Hermans Road, Tucson, AZ 85756, USA Received 2016 January 1; accepted 2016 March 14; published 2016 May 6 ABSTRACT Thermally pulsing asymptotic giant branch (TP-AGB) stars are relatively short lived (less than a few Myr), yet their cool effective temperatures, high luminosities, efficient mass loss, and dust production can dramatically affect the chemical enrichment histories and the spectral energy distributions of their host galaxies. The ability to accurately model TP-AGB stars is critical to the interpretation of the integrated light of distant galaxies, especially in redder wavelengths. We continue previous efforts to constrain the evolution and lifetimes of TP-AGB stars by modeling their underlying stellar populations. Using Hubble Space Telescope (HST) optical and near-infrared photometry taken of 12 fields of 10 nearby galaxies imaged via the Advanced Camera for Surveys Nearby Galaxy Survey Treasury and the near-infrared HST/SNAP follow-up campaign, we compare the model and observed TP- AGB luminosity functions as well as the ratio of TP-AGB to red giant branch stars.
    [Show full text]
  • Absolute-Magnitude Calibration for W Uma-Type Systems. II. in Uence Of
    AbsoluteMagnitude Calibration for W UMatype Systems I I Inuence of Metallicity 1 Slavek Rucinski Longb ow Drive Scarb orough Ontario MW W Canada March ABSTRACT A mo dication to the absolute magnitude calibration for W UMatype systems taking into account dierences in metal abundances is derived on the basis of contact binary systems recently discovered in metalp o or clusters A preliminary estimate of the magnitude of the metallicitydependent term for the B V based calibration is M F eH The calibration based on the V I color is V C exp ected to b e less sensitive with the correction term F eH Need for a metallicitydependent term in the calibration Searches for gravitational microlenses are currently giving large numbers of serendipitously discovered variable stars Among these variables there are many W UMatype contact binaries On the basis of the rst part of the catalog of variable stars discovered during the OGLE pro ject Udalski et al one can estimate the total number of contact binaries which will b e discovered in the Baade Window during OGLE at well over one thousand This estimate is based on discoveries of such systems in the rst part of the catalog which covered one of the OGLE elds ie less than of the whole area searched the Central Baade Window BWC and reached I The newly discovered systems will provide excellent statistics for the p erio d color and amplitude distributions of contact binaries much b etter than those based on the skyeld sample which is heavily biased towards largeamplitude variables Kaluzny
    [Show full text]
  • Cfa in the News ~ Week Ending 3 January 2010
    Wolbach Library: CfA in the News ~ Week ending 3 January 2010 1. New social science research from G. Sonnert and co-researchers described, Science Letter, p40, Tuesday, January 5, 2010 2. 2009 in science and medicine, ROGER SCHLUETER, Belleville News Democrat (IL), Sunday, January 3, 2010 3. 'Science, celestial bodies have always inspired humankind', Staff Correspondent, Hindu (India), Tuesday, December 29, 2009 4. Why is Carpenter defending scientists?, The Morning Call, Morning Call (Allentown, PA), FIRST ed, pA25, Sunday, December 27, 2009 5. CORRECTIONS, OPINION BY RYAN FINLEY, ARIZONA DAILY STAR, Arizona Daily Star (AZ), FINAL ed, pA2, Saturday, December 19, 2009 6. We see a 'Super-Earth', TOM BEAL; TOM BEAL, ARIZONA DAILY STAR, Arizona Daily Star, (AZ), FINAL ed, pA1, Thursday, December 17, 2009 Record - 1 DIALOG(R) New social science research from G. Sonnert and co-researchers described, Science Letter, p40, Tuesday, January 5, 2010 TEXT: "In this paper we report on testing the 'rolen model' and 'opportunity-structure' hypotheses about the parents whom scientists mentioned as career influencers. According to the role-model hypothesis, the gender match between scientist and influencer is paramount (for example, women scientists would disproportionately often mention their mothers as career influencers)," scientists writing in the journal Social Studies of Science report (see also ). "According to the opportunity-structure hypothesis, the parent's educational level predicts his/her probability of being mentioned as a career influencer (that ism parents with higher educational levels would be more likely to be named). The examination of a sample of American scientists who had received prestigious postdoctoral fellowships resulted in rejecting the role-model hypothesis and corroborating the opportunity-structure hypothesis.
    [Show full text]
  • PHAS 1102 Physics of the Universe 3 – Magnitudes and Distances
    PHAS 1102 Physics of the Universe 3 – Magnitudes and distances Brightness of Stars • Luminosity – amount of energy emitted per second – not the same as how much we observe! • We observe a star’s apparent brightness – Depends on: • luminosity • distance – Brightness decreases as 1/r2 (as distance r increases) • other dimming effects – dust between us & star Defining magnitudes (1) Thus Pogson formalised the magnitude scale for brightness. This is the brightness that a star appears to have on the sky, thus it is referred to as apparent magnitude. Also – this is the brightness as it appears in our eyes. Our eyes have their own response to light, i.e. they act as a kind of filter, sensitive over a certain wavelength range. This filter is called the visual band and is centred on ~5500 Angstroms. Thus these are apparent visual magnitudes, mv Related to flux, i.e. energy received per unit area per unit time Defining magnitudes (2) For example, if star A has mv=1 and star B has mv=6, then 5 mV(B)-mV(A)=5 and their flux ratio fA/fB = 100 = 2.512 100 = 2.512mv(B)-mv(A) where !mV=1 corresponds to a flux ratio of 1001/5 = 2.512 1 flux(arbitrary units) 1 6 apparent visual magnitude, mv From flux to magnitude So if you know the magnitudes of two stars, you can calculate mv(B)-mv(A) the ratio of their fluxes using fA/fB = 2.512 Conversely, if you know their flux ratio, you can calculate the difference in magnitudes since: 2.512 = 1001/5 log (f /f ) = [m (B)-m (A)] log 2.512 10 A B V V 10 = 102/5 = 101/2.5 mV(B)-mV(A) = !mV = 2.5 log10(fA/fB) To calculate a star’s apparent visual magnitude itself, you need to know the flux for an object at mV=0, then: mS - 0 = mS = 2.5 log10(f0) - 2.5 log10(fS) => mS = - 2.5 log10(fS) + C where C is a constant (‘zero-point’), i.e.
    [Show full text]
  • Variable Star Section Circular
    ΒΑΛ The British Astronomical Association VARIABLE STAR SECTION CIRCULAR 64 "LIGHT-CURVE” AUGUST 1986 ISSN 0267-9272 Office: Burlington House, Piccadilly, London, W1V 9AG SECTION OFFICERS: Director D.R.B. Saw, 'Upanova1, 18 Dolllcott, Haddenham, Aylesbury, Bucks. HP17 8JG Tel: Haddenham (0844) 292065 Assistant Director S.R. Dunlop, 140 Stocks Lane, East Wittering, nr Chichester, West Sussex P020 8NT Tel: Bracklesham Bay (0243) 670354 Secretary M.D. Taylor, 17 Cross Lane, Wakefield, West Yorkshire WF2 8DA Tel: Wakefield (0924) 374651 Programme Secretaries: Assistant Secretary (Post temporarily vacant) Telescopic Assistant Secretary J. Toone, 2 Hilton Crescent, Boothstown, Binocular Worsley, Manchester M28 4FY Tel: 061 702 8619 Eclipsing Binary J.E. Isles, Rose Cottage, 22 High Street, Secretary Wescott, Bucks. HP18 OPU Tel: Aylesbury (0296) 651779 Nova/Supernova G.M Hurst, 16 Westminster Close, Search Secretary Kempshott Rise, Basingstoke, Hants. RG22 4PP Tel: Basingstoke (0256) 471074 Chart Secretary J. Parkinson, 229 Scar Lane, Golcar, (except Eclipsing) Huddersfield, West Yorkshire HD7 4AU Tel: Huddersfield (0484) 642947 For subcription rates and charges for charts and other publications see inside back cover. Editorial It has been suggested that these C irc u la rs are often a little 'dry' and technical for some members. We are always happy to receive more 'personal' items and hope to include more in future issues. We are also including an occasional short note on some of the terms encountered, and which may not be fully explained in some of the specific articles. The first such item appears on p.13. If you have any queries, however elementary, please send them in, and we shall do our best to provide the answers.
    [Show full text]