B. Szeidl, Konkoly Observatory
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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. -
Winter Constellations
Winter Constellations *Orion *Canis Major *Monoceros *Canis Minor *Gemini *Auriga *Taurus *Eradinus *Lepus *Monoceros *Cancer *Lynx *Ursa Major *Ursa Minor *Draco *Camelopardalis *Cassiopeia *Cepheus *Andromeda *Perseus *Lacerta *Pegasus *Triangulum *Aries *Pisces *Cetus *Leo (rising) *Hydra (rising) *Canes Venatici (rising) Orion--Myth: Orion, the great hunter. In one myth, Orion boasted he would kill all the wild animals on the earth. But, the earth goddess Gaia, who was the protector of all animals, produced a gigantic scorpion, whose body was so heavily encased that Orion was unable to pierce through the armour, and was himself stung to death. His companion Artemis was greatly saddened and arranged for Orion to be immortalised among the stars. Scorpius, the scorpion, was placed on the opposite side of the sky so that Orion would never be hurt by it again. To this day, Orion is never seen in the sky at the same time as Scorpius. DSO’s ● ***M42 “Orion Nebula” (Neb) with Trapezium A stellar nursery where new stars are being born, perhaps a thousand stars. These are immense clouds of interstellar gas and dust collapse inward to form stars, mainly of ionized hydrogen which gives off the red glow so dominant, and also ionized greenish oxygen gas. The youngest stars may be less than 300,000 years old, even as young as 10,000 years old (compared to the Sun, 4.6 billion years old). 1300 ly. 1 ● *M43--(Neb) “De Marin’s Nebula” The star-forming “comma-shaped” region connected to the Orion Nebula. ● *M78--(Neb) Hard to see. A star-forming region connected to the Orion Nebula. -
La Constellation Du Cocher Ou Auriga ( Latin )
DansDans lala ss éérierie lesles constellationsconstellations lala constellationconstellation dudu CocherCocher ouou AurigaAuriga (( LatinLatin )) - Repérage - Caractéristiques - Histoire Constellation d’hiver, le Cocher fait partie des 48 constellations originellement répertoriées par Ptolémée dans son Almageste*. Superficie 657 deg² à comparer aux 1 255 deg² d’Hercule par exemple… * L'Almageste (qui est l'arabisation du grec ancien megistos (byblos) signifiant grand (livre)) est une œuvre de Claude Ptolémée datant du IIe siècle étant la somme des connaissances les plus avancées de son époque Patrice D écembre 2008 en mathématiques et en astronomie. L'Almageste contient également un catalogue d'étoiles. LocalisationLocalisation RepRep ééragerage • Le Cocher est une constellation très étendue traversée par la Voie Lactée et riche en amas d'étoiles, la constellation du Cocher se signale d'abord par son étoile principale, Capella. • Si la Grande Ourse est visible, Capella se situe dans la direction pointée par le grand chariot, à une vingtaine de degrés vers l’ Est. • Capella - Presque aussi brillante que Véga de la Lyre et d'une luminosité supérieure à celle de Rigel d'Orion. FormeForme • Partiellement circumpolaire, observée depuis une latitude de 45° Nord, la constellation dessine sensiblement un pentagone formé dans le sens des aiguilles d'une montre par Capella α Aur, ς Aur, ß du Taureau située juste à la limite sud de la constellation, puis en remontant vers le nord, θ Aur et ß Aur. • L'autre élément remarquable de la constellation est formé par les trois petites "chevrettes" η, ζ et ε Aur, qui forment un triangle serré au Sud de Capella. CaractCaract ééristiquesristiques CapellaCapella Capella (α Aurigae) appartient au groupe de tête des étoiles les plus éclatantes de nos nuits. -
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. -
Milan Dimitrijevic Avgust.Qxd
1. M. Platiša, M. Popović, M. Dimitrijević, N. Konjević: 1975, Z. Fur Natur- forsch. 30a, 212 [A 1].* 1. Griem, H. R.: 1975, Stark Broadening, Adv. Atom. Molec. Phys. 11, 331. 2. Platiša, M., Popović, M. V., Konjević, N.: 1975, Stark broadening of O II and O III lines, Astron. Astrophys. 45, 325. 3. Konjević, N., Wiese, W. L.: 1976, Experimental Stark widths and shifts for non-hydrogenic spectral lines of ionized atoms, J. Phys. Chem. Ref. Data 5, 259. 4. Hey, J. D.: 1977, On the Stark broadening of isolated lines of F (II) and Cl (III) by plasmas, JQSRT 18, 649. 5. Hey, J. D.: 1977, Estimates of Stark broadening of some Ar III and Ar IV lines, JQSRT 17, 729. 6. Hey, J. D.: Breger, P.: 1980, Stark broadening of isolated lines emitted by singly - ionized tin, JQSRT 23, 311. 7. Hey, J. D.: Breger, P.: 1981, Stark broadening of isolated ion lines by plas- mas: Application of theory, in Spectral Line Shapes I, ed. B. Wende, W. de Gruyter, 201. 8. Сыркин, М. И.: 1981, Расчеты электронного уширения спектральных линий в теории оптических свойств плазмы, Опт. Спектроск. 51, 778. 9. Wiese, W. L., Konjević, N.: 1982, Regularities and similarities in plasma broadened spectral line widths (Stark widths), JQSRT 28, 185. 10. Konjević, N., Pittman, T. P.: 1986, Stark broadening of spectral lines of ho- mologous, doubly ionized inert gases, JQSRT 35, 473. 11. Konjević, N., Pittman, T. P.: 1987, Stark broadening of spectral lines of ho- mologous, doubly - ionized inert gases, JQSRT 37, 311. 12. Бабин, С. -
Astronomy 111 Recitation #1
Astronomy 142 Recitation #10 5 April 2013 Formulas to remember Leavitt's Law (classical Cepheid variables): MV =−2.77 log Π− 1.69 d mMVV−=5log 10 pc Hubble’s Law (galaxies in the uniform Universal expansion): vr = Hd0 -1 -1 -1 -1 H0 = 74.2 km sec Mpc= 22.8 km sec Mly Redshift z =(λλ − 00) λ SN Ia magnitude(dereddened) 00 d mMVV=++5log 25 Mpc 0 MV = −19.14 dE dm Black hole accretion Lc= = εε2 , ≈ 0.1. dt dt Eddington luminosity 25 4 3GMmpe m c 2eL LL<= ; M> E 4 25 23e Gmpe m c Workshop problems Warning! The workshop problems you will do in groups in Recitation are a crucial part of the process of building up your command of the concepts important in AST 142 and subsequent courses. Do not, therefore, do your work on scratch paper and discard it. Better for each of you to keep your own account of each problem, in some sort of bound notebook. 1. (Team discussion) A type Ia supernova happens when a the mass of a white dwarf, accreting material from a close-by normal or giant stellar companions, approaches the Stoner-Anderson- Chandrasekhar mass, MM= 1.4 . Review your previous experience with degenerate stars and answer the following questions, in order. a. If mass is added to a white dwarf, does its radius get larger, smaller, or stay the same? Is this different from what happens when mass is added to an ordinary, nondegenerate star? 2013 University of Rochester 1 All rights reserved Astronomy 142, Spring 2013 b. -
The Radio Astronomy of Bruce Slee
CSIRO PUBLISHING Review www.publish.csiro.au/journals/pasa Publications of the Astronomical Society of Australia, 2004, 21, 23–71 From the Solar Corona to Clusters of Galaxies: The Radio Astronomy of Bruce Slee Wayne Orchiston Australia Telescope National Facility, PO Box 76, Epping NSW 2121, Australia (e-mail: [email protected]) Received 2003 May 8, accepted 2003 September 27 Abstract: Owen Bruce Slee is one of the pioneers of Australian radio astronomy. During World War II he independently discovered solar radio emission, and, after joining the CSIRO Division of Radiophysics, used a succession of increasingly more sophisticated radio telescopes to examine an amazing variety of celestial objects and phenomena. These ranged from the solar corona and other targets in our solar system, to different types of stars and the ISM in our Galaxy, and beyond to distant galaxies and clusters of galaxies. Although long retired, Slee continues to carry out research, with emphasis on active stars and clusters of galaxies. A quiet and unassuming man, Slee has spent more than half a century making an important, wide-ranging contribution to astronomy, and his work deserves to be more widely known. Keywords: biographies — Bruce Slee — radio continuum: galaxies — radio continuum: ISM — radio continuum: stars — stars: flare — Sun: corona 1 Introduction Radio astronomy is so new a discipline that it has yet to acquire an extensive historical bibliography. With founda- tions dating from 1931 this is perhaps not surprising, and it is only since the publication of Sullivan’s classic work, The Early Years of Radio Astronomy, in 1984 that schol- ars have begun to take a serious interest in the history of this discipline and its ‘key players’. -
The Washburn Observer
The Washburn Observer Volume 3, No. 2 • Fall 2013 • www.astro.wisc.edu New Faces in the Department This Fall Inside This Issue he Astronomy Department welcomes the Charee Peters has an MA degree incoming 2013–14 class of graduate students, in physics from the Fisk-Vanderbilt Letter from the Chair 2 T visiting faculty and postdocs. Masters-to-PhD Bridge Program and a John Chisholm Bitten by BS degree in physics from the University Astronomy and Travel Bugs 3 Elijah Bernstein-Cooper has a BS degree in phys- of Denver (Colorado). She is working with Professor Eric Wilcots on observing SKA Pathfinders: A Bright ics, with an astronomy emphasis, from Macalester Radio Future 4 College in St. Paul, Minnesota. He is working with HI regions (interstellar clouds of neutral Professor Snezana Stanimirovic to answer what hydrogen) in intermediate galaxies to Department Welcomes better understand star formation, galaxy Second Grainger Fellow 5 role atomic hydrogen plays in the formation of molecular hydrogen in giant molecular clouds. formation and evolution, and/or cosmic Solar System’s in Good magnetic fields. Hands with Anne Kinney 6 Yi-Hao Chen has an MS degree in astrophysics For Garret Frankson, from Ludwig-Maximillian University in Munich, Brianna Smart has a BS degree in astron- Astronomy Is a Passion 6 Germany and a BS degree in physics from National omy and physics from the University of Arizona in Tucson. She is working with News Notes 7 Taiwan University in Taipei. He is working with Professor Sebastian Heinz on studying the effect senior scientist Matt Haffner on studying of magnetic fields on propagation of jets from the ISM using the Wisconsin H-Alpha compact objects. -
On the Application of Stark Broadening Data Determined with a Semiclassical Perturbation Approach
Atoms 2014, 2, 357-377; doi:10.3390/atoms2030357 OPEN ACCESS atoms ISSN 2218-2004 www.mdpi.com/journal/atoms Article On the Application of Stark Broadening Data Determined with a Semiclassical Perturbation Approach Milan S. Dimitrijević 1,2,* and Sylvie Sahal-Bréchot 2 1 Astronomical Observatory, Volgina 7, 11060 Belgrade, Serbia 2 Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique, Observatoire de Paris, UMR CNRS 8112, UPMC, 5 Place Jules Janssen, 92195 Meudon Cedex, France; E-Mail: [email protected] (S.S.-B.) * Author to whom correspondence should be addressed; E-Mail: [email protected]; Tel.: +381-64-297-8021; Fax: +381-11-2419-553. Received: 5 May 2014; in revised form: 20 June 2014 / Accepted: 16 July 2014 / Published: 7 August 2014 Abstract: The significance of Stark broadening data for problems in astrophysics, physics, as well as for technological plasmas is discussed and applications of Stark broadening parameters calculated using a semiclassical perturbation method are analyzed. Keywords: Stark broadening; isolated lines; impact approximation 1. Introduction Stark broadening parameters of neutral atom and ion lines are of interest for a number of problems in astrophysical, laboratory, laser produced, fusion or technological plasma investigations. Especially the development of space astronomy has enabled the collection of a huge amount of spectroscopic data of all kinds of celestial objects within various spectral ranges. Consequently, the atomic data for trace elements, which had not been -
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. -
ROSAT Observations of Superflares on RS Cvn Systems
ROSAT Observations of Superflares on RS CVn Systems Vito Giuseppe GrafFagnino Thesis submitted for the degree of Doctor of Philosophy, in the Faculty of Science of the University of London. UCL Mullard Space Science Laboratory Department of Space & Climate Physics U n i v e r s i t y • C o l l e g e • L o n d o n 2000 ProQuest Number: U642316 All rights reserved INFORMATION TO ALL USERS The quality of this reproduction is dependent upon the quality of the copy submitted. In the unlikely event that the author did not send a complete manuscript and there are missing pages, these will be noted. Also, if material had to be removed, a note will indicate the deletion. uest. ProQuest U642316 Published by ProQuest LLC(2015). Copyright of the Dissertation is held by the Author. All rights reserved. This work is protected against unauthorized copying under Title 17, United States Code. Microform Edition © ProQuest LLC. ProQuest LLC 789 East Eisenhower Parkway P.O. Box 1346 Ann Arbor, Ml 48106-1346 ,,. A Mia Moglie E Miei Genitori A bstract The following thesis involves the analysis of a number of X-ray observations of two RS CVn systems, made using the ROSAT satellite. These observa tions have revealed a number of long-duration flares lasting several days (much longer than previously observed in the X-ray energy band) and emitting ener gies which total a few percent of the available magnetic energy of the stellar system and thus far greater than previously encountered. Calculations based on the spectrally fitted parameters show that simple flare mechanisms and standard two-ribbon flare models cannot explain the observations satisfacto rily and continued heating was observed during the outbursts. -
Extrasolar Planet Detection and Characterization with the KELT-North Transit Survey
Extrasolar Planet Detection and Characterization With the KELT-North Transit Survey DISSERTATION Presented in Partial Fulfillment of the Requirements for the Degree Doctor of Philosophy in the Graduate School of The Ohio State University By Thomas G. Beatty Graduate Program in Astronomy The Ohio State University 2014 Dissertation Committee: Professor B. Scott Gaudi, Advisor Professor Andrew P. Gould Professor Marc H. Pinsonneault Copyright by Thomas G. Beatty 2014 Abstract My dissertation focuses on the detection and characterization of new transiting extrasolar planets from the KELT-North survey, along with a examination of the processes underlying the astrophysical errors in the type of radial velocity measurements necessary to measure exoplanetary masses. Since 2006, the KELT- North transit survey has been collecting wide-angle precision photometry for 20% of the sky using a set of target selection, lightcurve processing, and candidate identification protocols I developed over the winter of 2010-2011. Since our initial set of planet candidates were generated in April 2011, KELT-North has discovered seven new transiting planets, two of which are among the five brightest transiting hot Jupiter systems discovered via a ground-based photometric survey. This highlights one of the main goals of the KELT-North survey: to discover new transiting systems orbiting bright, V< 10, host stars. These systems offer us the best targets for the precision ground- and space-based follow-up observations necessary to measure exoplanetary atmospheres. In September 2012 I demonstrated the atmospheric science enabled by the new KELT planets by observing the secondary eclipses of the brown dwarf KELT-1b with the Spitzer Space Telescope.