NORTHWESTERN UNIVERSITY Single Audit Report Year Ended August 31, 2019 (With Independent Auditors' Report Thereon)
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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. -
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. -
Astronomy Magazine 2011 Index Subject Index
Astronomy Magazine 2011 Index Subject Index A AAVSO (American Association of Variable Star Observers), 6:18, 44–47, 7:58, 10:11 Abell 35 (Sharpless 2-313) (planetary nebula), 10:70 Abell 85 (supernova remnant), 8:70 Abell 1656 (Coma galaxy cluster), 11:56 Abell 1689 (galaxy cluster), 3:23 Abell 2218 (galaxy cluster), 11:68 Abell 2744 (Pandora's Cluster) (galaxy cluster), 10:20 Abell catalog planetary nebulae, 6:50–53 Acheron Fossae (feature on Mars), 11:36 Adirondack Astronomy Retreat, 5:16 Adobe Photoshop software, 6:64 AKATSUKI orbiter, 4:19 AL (Astronomical League), 7:17, 8:50–51 albedo, 8:12 Alexhelios (moon of 216 Kleopatra), 6:18 Altair (star), 9:15 amateur astronomy change in construction of portable telescopes, 1:70–73 discovery of asteroids, 12:56–60 ten tips for, 1:68–69 American Association of Variable Star Observers (AAVSO), 6:18, 44–47, 7:58, 10:11 American Astronomical Society decadal survey recommendations, 7:16 Lancelot M. Berkeley-New York Community Trust Prize for Meritorious Work in Astronomy, 3:19 Andromeda Galaxy (M31) image of, 11:26 stellar disks, 6:19 Antarctica, astronomical research in, 10:44–48 Antennae galaxies (NGC 4038 and NGC 4039), 11:32, 56 antimatter, 8:24–29 Antu Telescope, 11:37 APM 08279+5255 (quasar), 11:18 arcminutes, 10:51 arcseconds, 10:51 Arp 147 (galaxy pair), 6:19 Arp 188 (Tadpole Galaxy), 11:30 Arp 273 (galaxy pair), 11:65 Arp 299 (NGC 3690) (galaxy pair), 10:55–57 ARTEMIS spacecraft, 11:17 asteroid belt, origin of, 8:55 asteroids See also names of specific asteroids amateur discovery of, 12:62–63 -
Macrocosmo Nº33
HA MAIS DE DOIS ANOS DIFUNDINDO A ASTRONOMIA EM LÍNGUA PORTUGUESA K Y . v HE iniacroCOsmo.com SN 1808-0731 Ano III - Edição n° 33 - Agosto de 2006 * t i •■•'• bSÈlÈWW-'^Sif J fé . ’ ' w s » ws» ■ ' v> í- < • , -N V Í ’\ * ' "fc i 1 7 í l ! - 4 'T\ i V ■ }'- ■t i' ' % r ! ■ 7 ji; ■ 'Í t, ■ ,T $ -f . 3 j i A 'A ! : 1 l 4/ í o dia que o ceu explodiu! t \ Constelação de Andrômeda - Parte II Desnudando a princesa acorrentada £ Dicas Digitais: Softwares e afins, ATM, cursos online e publicações eletrônicas revista macroCOSMO .com Ano III - Edição n° 33 - Agosto de I2006 Editorial Além da órbita de Marte está o cinturão de asteróides, uma região povoada com Redação o material que restou da formação do Sistema Solar. Longe de serem chamados como simples pedras espaciais, os asteróides são objetos rochosos e/ou metálicos, [email protected] sem atmosfera, que estão em órbita do Sol, mas são pequenos demais para serem considerados como planetas. Até agora já foram descobertos mais de 70 Diretor Editor Chefe mil asteróides, a maior parte situados no cinturão de asteróides entre as órbitas Hemerson Brandão de Marte e Júpiter. [email protected] Além desse cinturão podemos encontrar pequenos grupos de asteróides isolados chamados de Troianos que compartilham a mesma órbita de Júpiter. Existem Editora Científica também aqueles que possuem órbitas livres, como é o caso de Hidalgo, Apolo e Walkiria Schulz Ícaro. [email protected] Quando um desses asteróides cruza a nossa órbita temos as crateras de impacto. A maior cratera visível de nosso planeta é a Meteor Crater, com cerca de 1 km de Diagramadores diâmetro e 600 metros de profundidade. -
Download This Issue (Pdf)
Volume 46 Number 1 JAAVSO 2018 The Journal of the American Association of Variable Star Observers Optical Flares and Quasi-Periodic Pulsations on CR Draconis during Periastron Passage Upper panel: 2017-10-10-flare photon counts, time aligned with FFT spectrogram. Lower panel: FFT spectrogram shows time in UT seconds versus QPP periods in seconds. Flares cited by Doyle et al. (2018) are shown with (*). Also in this issue... • The Dwarf Nova SY Cancri and its Environs • KIC 8462852: Maria Mitchell Observatory Photographic Photometry 1922 to 1991 • Visual Times of Maxima for Short Period Pulsating Stars III • Recent Maxima of 86 Short Period Pulsating Stars Complete table of contents inside... The American Association of Variable Star Observers 49 Bay State Road, Cambridge, MA 02138, USA The Journal of the American Association of Variable Star Observers Editor John R. Percy Kosmas Gazeas Kristine Larsen Dunlap Institute of Astronomy University of Athens Department of Geological Sciences, and Astrophysics Athens, Greece Central Connecticut State University, and University of Toronto New Britain, Connecticut Toronto, Ontario, Canada Edward F. Guinan Villanova University Vanessa McBride Associate Editor Villanova, Pennsylvania IAU Office of Astronomy for Development; Elizabeth O. Waagen South African Astronomical Observatory; John B. Hearnshaw and University of Cape Town, South Africa Production Editor University of Canterbury Michael Saladyga Christchurch, New Zealand Ulisse Munari INAF/Astronomical Observatory Laszlo L. Kiss of Padua Editorial Board Konkoly Observatory Asiago, Italy Geoffrey C. Clayton Budapest, Hungary Louisiana State University Nikolaus Vogt Baton Rouge, Louisiana Katrien Kolenberg Universidad de Valparaiso Universities of Antwerp Valparaiso, Chile Zhibin Dai and of Leuven, Belgium Yunnan Observatories and Harvard-Smithsonian Center David B. -
Hydrogen Subordinate Line Emission at the Epoch of Cosmological Recombination M
Astronomy Reports, Vol. 47, No. 9, 2003, pp. 709–716. Translated from Astronomicheski˘ı Zhurnal, Vol. 80, No. 9, 2003, pp. 771–779. Original Russian Text Copyright c 2003 by Burgin. Hydrogen Subordinate Line Emission at the Epoch of Cosmological Recombination M. S. Burgin Astro Space Center, Lebedev Physical Institute, Russian Academy of Sciences, Profsoyuznaya ul. 84/32, Moscow, 117997 Russia Received December 10, 2002; in final form, March 14, 2003 Abstract—The balance equations for the quasi-stationary recombination of hydrogen plasma in a black- body radiation field are solved. The deviations of the excited level populations from equilibrium are computed and the rates of uncompensated line transitions determined. The expressions obtained are stable for computations of arbitrarily small deviations from equilibrium. The average number of photons emitted in hydrogen lines per irreversible recombination is computed for plasma parameters corresponding to the epoch of cosmological recombination. c 2003 MAIK “Nauka/Interperiodica”. 1. INTRODUCTION of this decay is responsible for the appreciable differ- When the cosmological expansion of the Universe ence between the actual degree of ionization and the lowered the temperature sufficiently, the initially ion- value correspondingto the Saha –Boltzmann equi- ized hydrogen recombined. According to [1, 2], an librium. A detailed analysis of processes affectingthe appreciable fraction of the photons emitted at that recombination rate and computations of the temporal time in subordinate lines survive to the present, lead- behavior of the degree of ionization for various sce- ingto the appearance of spectral lines in the cosmic narios for the cosmological expansion are presented background (relict) radiation. Measurements of the in [5, 6]. -
EDEXCEL INTERNATIONAL GCSE (9 –1) Student Book 1
EDEXCEL INTERNATIONAL GCSE (9 –1) MATHEMATICS A Student Book 1 David Turner, Ian Potts eBook included 1 Online access to your ActiveBook Thank you for buying this Edexcel International GCSE (9-1) Mathematics A Student Book 1. It comes with three years’ access* to ActiveBook – an online, digital version of your textbook. You can personalise your ActiveBook with notes, highlights and links to your wider reading. It is perfect for supporting your coursework and revision activities. * For new purchases only. If this access code has already been revealed, it may no longer be valid. If you have bought this textbook second hand, the code may already have been used by the fi rst owner of the book. How to access your ActiveBook Scratch the panel off with a coin to reveal your unique access code. Do not use a knife or other sharp object 1 as it may damage the code. 2 Go to www.pearsonactivelearn.com If you already have an ActiveLearn Digital Services account (ActiveTeach or ActiveLearn), log in and click 3 ‘I have a new access code’ in the top right of the screen. • Type in the code above and select ‘Activate’. If you do not have an ActiveLearn Digital Services account, click ‘Register’. It is free to do this. 4 • Type in the code above and select ‘Activate’. • Simply follow the instructions on screen to register. Important information • The access code can only be used once. • Please activate your access code as soon as possible, as it does have a ‘use by date’. If your code has expired when you enter it, please contact our ActiveLearn support site at [email protected] • The ActiveBook will be valid for three years upon activation. -
Arxiv:1902.02360V2 [Astro-Ph.GA] 8 Feb 2019 Ers and the Accretion of Smaller Galaxies (E.G
DRAFT VERSION FEBRUARY 11, 2019 Typeset using LATEX twocolumn style in AASTeX62 The Next Generation Fornax Survey (NGFS): V. Discovery of a dwarf-dwarf galaxy pair at z = 0:30 and its characterization using deep VLT/MUSE observations ∗ y z x EVELYN J. JOHNSTON,1 , PAUL EIGENTHALER,1 , THOMAS H. PUZIA,1 YASNA ORDENES-BRICENO˜ ,1, 2 , MATTHEW A. TAYLOR,3 , ∗ KARLA ALAMO-MART´INEZ,4 , PATRICK COTˆ E´,5 GASPAR GALAZ,1 EVA K. GREBEL,2 MICHAEL HILKER,6 ARIANE LANC¸ ON,7 y STEFFEN MIESKE,8 RUBEN SANCHEZ´ -JANSSEN,9 AND YU RONG1 , 1Institute of Astrophysics, Pontificia Universidad Catolica´ de Chile, Av. Vicuna˜ Mackenna 4860, 7820436 Macul, Santiago, Chile 2Astronomisches Rechen-Institut, Zentrum fur¨ Astronomie der Universitat¨ Heidelberg, Monchhofstraße¨ 12-14, D-69120 Heidelberg, Germany 3Gemini Observatory, Northern Operations Center, 670 North A’ohoku Place, Hilo, HI 96720, USA 4Departamento de Astronomia, Instituto de F´ısica, Universidade Federal do Rio Grande do Sul, 91501-970 Porto Alegre, R.S, Brazil 5NRC Herzberg Astronomy and Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada 6European Southern Observatory, Karl-Schwarzchild-Str. 2, D-85748 Garching, Germany 7Observatoire astronomique de Strasbourg, Universite´ de Strasbourg, CNRS, UMR 7550, 11 rue de l’Universite, F-67000 Strasbourg, France 8European Southern Observatory, 3107 Alonso de Cordova,´ Vitacura, Santiago 9STFC UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, UK (Received September 13, 2018; Revised February 01, 2019; Accepted February 02, 2019) Submitted to ApJ ABSTRACT We report the detection of a pair of dwarf galaxies at z = 0:30 which may be in the early stages of an 9 interaction. -
Candidate Milky Way Satellites in the Galactic Halo
A&A 477, 139–145 (2008) Astronomy DOI: 10.1051/0004-6361:20078392 & c ESO 2007 Astrophysics Candidate Milky Way satellites in the Galactic halo C. Liu1,2,J.Hu1,H.Newberg3,andY.Zhao1 1 National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, PR China e-mail: [email protected] 2 Graduate University of Chinese Academy of Sciences, Beijing 100049, PR China 3 Department of Physics, Applied Physics, and Astronomy, Rensselaer Polytechnic Institute, Troy, NY 12180, USA Received 1 August 2007 / Accepted 28 September 2007 ABSTRACT Aims. Sloan Digital Sky Survey (SDSS) DR5 photometric data with 120◦ <α<270◦,25◦ <δ<70◦ were searched for new Milky Way companions or substructures in the Galactic halo. Methods. Five candidates are identified as overdense faint stellar sources that have color-magnitude diagrams similar to those of known globular clusters, or dwarf spheroidal galaxies. The distance to each candidate is estimated by fitting suitable stellar isochrones to the color-magnitude diagrams. Geometric properties and absolute magnitudes are roughly measured and used to determine whether the candidates are likely dwarf spheroidal galaxies, stellar clusters, or tidal debris. Results. SDSSJ1000+5730 and SDSSJ1329+2841 are probably faint dwarf galaxy candidates while SDSSJ0814+5105, SDSSJ0821+5608, and SDSSJ1058+2843 are very likely extremely faint globular clusters. Conclusions. Follow-up study is needed to confirm these candidates. Key words. Galaxy: structure – Galaxy: halo – galaxies: dwarf – Local Group 1. Introduction globular clusters: Willman 1 (Willman et al. 2005b) and Segue 1 (Belokurov et al. 2007). The discovery of tidal streams in the Milky Way from the accre- It is impossible to see these objects in SDSS images since tion of smaller galaxies supports hierarchical merging cosmogo- they are resolved into field stars. -
Cycle 25 Approved Programs
Cycle 25 Approved Programs Phase II First Name Last Name Institution Country Type Resources Title 15328 Jessica Agarwal Max Planck Institute for Solar DEU GO 5 Orbital period and formation process of the exceptional binary asteroid System Research system 288P 15090 Marcel Agueros Columbia University in the City of USA GO 35 A UV spectroscopic survey of periodic M dwarfs in the Hyades New York 15091 Marcel Agueros Columbia University in the City of USA SNAP 86 A UV spectroscopic snapshot survey of low-mass stars in the Hyades New York 15092 Monique Aller Georgia Southern University Res. USA GO 6 Testing Dust Models at Moderate Redshift: Is the z=0.437 DLA toward 3C & Svc. Foundation, Inc 196 Rich in Carbonaceous Dust? 15193 Alessandra Aloisi Space Telescope Science Institute USA GO 22 Addressing Ionization and Depletion in the ISM of Nearby Star-Forming Galaxies 15194 Alessandra Aloisi Space Telescope Science Institute USA GO 18 The Epoch of the First Star Formation in the Closest Metal-Poor Blue Compact Dwarf Galaxy UGC 4483 15299 Julian Alvarado GomeZ Smithsonian Institution USA GO 13 Weaving the history of the solar wind with magnetic field lines Astrophysical Observatory 15093 Jennifer Andrews University of Arizona USA GO 18 Dwarfs and Giants: Massive Stars in Little Dwarf Galaxies 15222 Iair Arcavi University of California - Santa USA GO 1 What Type of Star Made the One-of-a-kind Supernova iPTF14hls? Barbara 15223 Matthew Auger University of Cambridge GBR GO 1 The Brightest Galaxy-Scale Lens 15300 Thomas Ayres University of Colorado -
Biological Damage of Uv Radiation in Environments Of
BIOLOGICAL DAMAGE OF UV RADIATION IN ENVIRONMENTS OF F-TYPE STARS by SATOKO SATO Presented to the Faculty of the Graduate School of The University of Texas at Arlington in Partial Fulfillment of the Requirements for the Degree of DOCTOR OF PHILOSOPHY THE UNIVERSITY OF TEXAS AT ARLINGTON May 2014 Copyright c by Satoko Sato 2014 All Rights Reserved I dedicate this to my daughter Akari Y. Sato. Acknowledgements First of all, I would like to thank my supervising professor Dr. Manfred Cuntz. His advice on my research and academic life has always been invaluable. I would have given up the Ph.D. bound program without his encouragement and generous support as the supervising professor during a few difficult times in my life. I would like to thank Dr. Wei Chen, Dr. Yue Deng, Dr. Zdzislaw E. Musielak, and Dr. Sangwook Park for their interest in my research and for their time to serve in my committee. Next, I would like to acknowledge my research collaborators at University of Guanajuato, Cecilia M. Guerra Olvera, Dr. Dennis Jack, and Dr. Klaus-Peter Schr¨oder,for providing me the data of F-type evolutionary tracks and UV spectra. I would also like to express my deep gratitude to my parents, Hideki and Kumiko Yakushigawa, for their enormous support in many ways in my entire life, and to my sister, Tomoko Yakushigawa, for her constant encouragement to me. I am grateful to my husband, Makito Sato, and my daughter, Akari Y. Sato. Their presence always gives me strength. I am thankful to my parents-in-law, Hisao and Tsuguho Sato, and my grand-parents-in-law, Kanji and Ayako Momoi, for their financial support and prayers. -
Tez.Pdf (5.401Mb)
ANKARA ÜNİVERSİTESİ FEN BİLİMLERİ ENSTİTÜSÜ YÜKSEK LİSANS TEZİ ÖRTEN DEĞİŞEN YILDIZLARDA DÖNEM DEĞİŞİMİNİN YILDIZLARIN FİZİKSEL PARAMETRELERİNE BAĞIMLILIĞININ ARAŞTIRILMASI Uğurcan SAĞIR ASTRONOMİ VE UZAY BİLİMLERİ ANABİLİM DALI ANKARA 2006 Her hakkı saklıdır TEŞEKKÜR Tez çalışmam esnasında bana araştırma olanağı sağlayan ve çalışmamın her safhasında yakın ilgi ve önerileri ile beni yönlendiren danışman hocam Sayın Yrd.Doç.Dr. Birol GÜROL’a ve maddi manevi her türlü desteği benden esirgemeyen aileme teşekkürlerimi sunarım. Uğurcan SAĞIR Ankara, Şubat 2006 iii İÇİNDEKİLER ÖZET………………………………………………………………….......................... i ABSTRACT……………………………………………………………....................... ii TEŞEKKÜR……………………………………………………………...................... iii SİMGELER DİZİNİ…………………………………………………….................... vii ŞEKİLLER DİZİNİ...................................................................................................... x ÇİZELGELER DİZİNİ.............................................................................................. xiv 1. GİRİŞ........................................................................................................................ 1 1.1 Çalışmanın Kapsamı................................................................................................ 1 1.2 Örten Çift Sistemlerin Türleri ve Özellikleri........................................................ 1 2. KURAMSAL TEMELLER................................................................................... 3 2.1 Örten Değişen Yıldızlarda Dönem Değişim Nedenleri..................................