Guide to the W. W. Morgan Papers Circa 1905-1990
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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. -
Lick Observatory Records: Photographs UA.036.Ser.07
http://oac.cdlib.org/findaid/ark:/13030/c81z4932 Online items available Lick Observatory Records: Photographs UA.036.Ser.07 Kate Dundon, Alix Norton, Maureen Carey, Christine Turk, Alex Moore University of California, Santa Cruz 2016 1156 High Street Santa Cruz 95064 [email protected] URL: http://guides.library.ucsc.edu/speccoll Lick Observatory Records: UA.036.Ser.07 1 Photographs UA.036.Ser.07 Contributing Institution: University of California, Santa Cruz Title: Lick Observatory Records: Photographs Creator: Lick Observatory Identifier/Call Number: UA.036.Ser.07 Physical Description: 101.62 Linear Feet127 boxes Date (inclusive): circa 1870-2002 Language of Material: English . https://n2t.net/ark:/38305/f19c6wg4 Conditions Governing Access Collection is open for research. Conditions Governing Use Property rights for this collection reside with the University of California. Literary rights, including copyright, are retained by the creators and their heirs. The publication or use of any work protected by copyright beyond that allowed by fair use for research or educational purposes requires written permission from the copyright owner. Responsibility for obtaining permissions, and for any use rests exclusively with the user. Preferred Citation Lick Observatory Records: Photographs. UA36 Ser.7. Special Collections and Archives, University Library, University of California, Santa Cruz. Alternative Format Available Images from this collection are available through UCSC Library Digital Collections. Historical note These photographs were produced or collected by Lick observatory staff and faculty, as well as UCSC Library personnel. Many of the early photographs of the major instruments and Observatory buildings were taken by Henry E. Matthews, who served as secretary to the Lick Trust during the planning and construction of the Observatory. -
Arxiv:2006.10868V2 [Astro-Ph.SR] 9 Apr 2021 Spain and Institut D’Estudis Espacials De Catalunya (IEEC), C/Gran Capit`A2-4, E-08034 2 Serenelli, Weiss, Aerts Et Al
Noname manuscript No. (will be inserted by the editor) Weighing stars from birth to death: mass determination methods across the HRD Aldo Serenelli · Achim Weiss · Conny Aerts · George C. Angelou · David Baroch · Nate Bastian · Paul G. Beck · Maria Bergemann · Joachim M. Bestenlehner · Ian Czekala · Nancy Elias-Rosa · Ana Escorza · Vincent Van Eylen · Diane K. Feuillet · Davide Gandolfi · Mark Gieles · L´eoGirardi · Yveline Lebreton · Nicolas Lodieu · Marie Martig · Marcelo M. Miller Bertolami · Joey S.G. Mombarg · Juan Carlos Morales · Andr´esMoya · Benard Nsamba · KreˇsimirPavlovski · May G. Pedersen · Ignasi Ribas · Fabian R.N. Schneider · Victor Silva Aguirre · Keivan G. Stassun · Eline Tolstoy · Pier-Emmanuel Tremblay · Konstanze Zwintz Received: date / Accepted: date A. Serenelli Institute of Space Sciences (ICE, CSIC), Carrer de Can Magrans S/N, Bellaterra, E- 08193, Spain and Institut d'Estudis Espacials de Catalunya (IEEC), Carrer Gran Capita 2, Barcelona, E-08034, Spain E-mail: [email protected] A. Weiss Max Planck Institute for Astrophysics, Karl Schwarzschild Str. 1, Garching bei M¨unchen, D-85741, Germany C. Aerts Institute of Astronomy, Department of Physics & Astronomy, KU Leuven, Celestijnenlaan 200 D, 3001 Leuven, Belgium and Department of Astrophysics, IMAPP, Radboud University Nijmegen, Heyendaalseweg 135, 6525 AJ Nijmegen, the Netherlands G.C. Angelou Max Planck Institute for Astrophysics, Karl Schwarzschild Str. 1, Garching bei M¨unchen, D-85741, Germany D. Baroch J. C. Morales I. Ribas Institute of· Space Sciences· (ICE, CSIC), Carrer de Can Magrans S/N, Bellaterra, E-08193, arXiv:2006.10868v2 [astro-ph.SR] 9 Apr 2021 Spain and Institut d'Estudis Espacials de Catalunya (IEEC), C/Gran Capit`a2-4, E-08034 2 Serenelli, Weiss, Aerts et al. -
Cygnus a Monthly Sky Guide for the Beginning to Intermediate Amateur Astronomer Tom Trusock 10-Aug-2005
Small Wonders: Cygnus A monthly sky guide for the beginning to intermediate amateur astronomer Tom Trusock 10-Aug-2005 Figure 1: Widefield Map 2/16 Small Wonders: Cygnus Target List Object Type Size Mag RA Dec α (alpha) Cygni (Deneb) Star 1.3 20h 41m 38.7s 45 17' 59" β (beta) Cygni (Albireo) Star 3 19h 30m 57.9s 27 58' 18" NGC 7000 Bright Nebula 120.0'x100.0' 4 20h 59m 03.2s 44 32' 16" IC 5070 Bright Nebula 60.0'x50.0' 8 20h 51m 01.1s 44 12' 13" NGC 6960 Supernova Remnant 70.0'x6.0' 7 20h 45m 57.0s 30 44' 12" NGC 6979 Bright Nebula 7.0'x3.0' 20h 51m 14.9s 32 10' 14" NGC 6992 Bright Nebula 60.0'x8.0' 7 20h 56m 39.0s 31 44' 16" M 29 Open Cluster 10.0' 6.6 20h 24m 11.6s 38 30' 58" M 39 Open Cluster 31.0' 4.6 21h 32m 10.4s 48 26' 40" NGC 6826 Planetary Nebula 36" 8.8 19h 44m 58.8s 50 32' 21" NGC 7026 Planetary Nebula 45" 10.9 21h 06m 31.4s 47 52' 28" NGC 6888 Bright Nebula 18.0'x13.0' 10 20h 12m 20.0s 38 22' 18" NGC 6946 Galaxy 11.5'x9.8' 9 20h 35m 01.0s 60 10' 19" Challenge Objects Object Type Size Mag RA Dec PK 64+ 5.1 Planetary Nebula 5" 9.6 19h 35m 02.3s 30 31' 45" Sh2-112 9.0'x7.0' Cygnus ygnus is a spectacular summer constellation. -
Observer's Handbook 1989
OBSERVER’S HANDBOOK 1 9 8 9 EDITOR: ROY L. BISHOP THE ROYAL ASTRONOMICAL SOCIETY OF CANADA CONTRIBUTORS AND ADVISORS Alan H. B atten, Dominion Astrophysical Observatory, 5071 W . Saanich Road, Victoria, BC, Canada V8X 4M6 (The Nearest Stars). L a r r y D. B o g a n , Department of Physics, Acadia University, Wolfville, NS, Canada B0P 1X0 (Configurations of Saturn’s Satellites). Terence Dickinson, Yarker, ON, Canada K0K 3N0 (The Planets). D a v id W. D u n h a m , International Occultation Timing Association, 7006 Megan Lane, Greenbelt, MD 20770, U.S.A. (Lunar and Planetary Occultations). A lan Dyer, A lister Ling, Edmonton Space Sciences Centre, 11211-142 St., Edmonton, AB, Canada T5M 4A1 (Messier Catalogue, Deep-Sky Objects). Fred Espenak, Planetary Systems Branch, NASA-Goddard Space Flight Centre, Greenbelt, MD, U.S.A. 20771 (Eclipses and Transits). M a r ie F i d l e r , 23 Lyndale Dr., Willowdale, ON, Canada M2N 2X9 (Observatories and Planetaria). Victor Gaizauskas, J. W. D e a n , Herzberg Institute of Astrophysics, National Research Council, Ottawa, ON, Canada K1A 0R6 (Solar Activity). R o b e r t F. G a r r i s o n , David Dunlap Observatory, University of Toronto, Box 360, Richmond Hill, ON, Canada L4C 4Y6 (The Brightest Stars). Ian H alliday, Herzberg Institute of Astrophysics, National Research Council, Ottawa, ON, Canada K1A 0R6 (Miscellaneous Astronomical Data). W illiam H erbst, Van Vleck Observatory, Wesleyan University, Middletown, CT, U.S.A. 06457 (Galactic Nebulae). Ja m e s T. H im e r, 339 Woodside Bay S.W., Calgary, AB, Canada, T2W 3K9 (Galaxies). -
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 -
PROJECT ORI'on a Design Study of a System for Detecting Extrasolar Planets
PROJECT ORI'ON A Design Study of a System for Detecting Extrasolar Planets . NASA NASA SP-436 PROJECT ORION A Design Stud? of a System for Detecting Extrasolar Planets David C.Black, Editor Arnes Research Center Nat~cnalAeroriautics and Space Adminislrat~on Scientific and Technical Information Branch 1986) Cover: Orion Nebula XI1 Photograph courtesy of Lick Observatory. Ode to Apodization Twinkle, twinkle, little star Thirty parsecs from where we are. Does your wobble through the sky Mean a planet is nearby? Or has the result come into being Because of one arcsecond seeing? -Raymond P. Vito Library of Congress Cataloging in Publication Data Main entry under title: Project Orion. (NASA SP ; 436) Bibliography: p. 1. Project Orion. I. Black, David C. 11. Series: United States. National Aeronautics and Space Administration. NASA SP ;436. QB602.9.P76 523.1'13 80-11728 For sale by the Sul~erintenclentof Documents. U.S. Gorevnmc~ntPrinting Olficc \X7a\hinrrton n C 70402 TABLE OF CONTENTS Page PREFACE ......................................... ix 1 . INTRODUCTION ................................. 1 Discovery of Our Planetary System .................. 1 Efforts .to Detect Other Planetary Systems ............. 4 Project Orion ................................... 6 2 . TOWARD DESIGN CONCEPTS ..................... 11 Remarks Concerning the Term "Planet" .............. II Detection Problem .Astrophysical Aspects ........... 12 Detectioil Problem .Terrestrial Aspects .............. 24 Detection Problem .Hardware Aspects ............... 30 Summary ..................................... -
The Sky This Month Joel Swallow the Sky This Month
The Sky This Month Joel Swallow The Sky this Month • The Moon this month • The planets this month • The Big Dipper: signpost to the sky • Double Stars [20] [1] The Moon This Month Full Moon: November 14th New Moon: November 29th Full Moon: December 14th [3] [2] Supermoons : November 14th and December 14th [21] • On December 14th The Moon is 6.5% closer than it is on average • The Supermoon last month was even closer! – the closest it has been at the time of a full moon since 1948. • http://time.unitarium.com/moon/where.html : shows you where the moon is tonight (or any night) in relation to the Earth! [19] [18] Copernicous The Moon Aristachus • The dark regions of the Moon are called Mare (seas). • The lighter regions are known as the lunar highlands – oldest rock and mountain ranges. • Lots of craters: always best to Kepler view when these lie on the terminator. Tycho [8] The Moon [9] • The only astronomical object (apart from the ISS) you can observe that has had a visit from humans! [7] [6] Apollo Landing sites • 11: Sea of tranquillity • 12: Ocean of Storms • 13: “Houston, we've had a problem here” • 14: Fra Maro Highlands • 15: Hadley Rill • 16: Descartes Mountains • 17: Taurus-Littrow valley [10] Apollo Landing sites • 11: Sea of tranquillity • 12: Ocean of Storms • 13: “Houston, we've had a problem here” • 14: Fra Maro Highlands • 15: Hadley Rill • 16: Descartes Mountains • 17: Taurus-Littrow valley [22] [10] The Planets This Month [4] Mercury at Greatest Eastern Elongation • This is when the planet is furthest from the sun in the sky • Still only 20.8 degrees away! • Look in the W / SW sky just after sunset , forming a nice line with Mars and Venus! 11/12/16 4:25 pm Venus and Mars • Low on the southern Horizon in the evening sky 23/11/16 5:00 pm Venus and Mars • Low on the southern Horizon in the evening sky. -
Extrasolar Planets and Their Host Stars
Kaspar von Braun & Tabetha S. Boyajian Extrasolar Planets and Their Host Stars July 25, 2017 arXiv:1707.07405v1 [astro-ph.EP] 24 Jul 2017 Springer Preface In astronomy or indeed any collaborative environment, it pays to figure out with whom one can work well. From existing projects or simply conversations, research ideas appear, are developed, take shape, sometimes take a detour into some un- expected directions, often need to be refocused, are sometimes divided up and/or distributed among collaborators, and are (hopefully) published. After a number of these cycles repeat, something bigger may be born, all of which one then tries to simultaneously fit into one’s head for what feels like a challenging amount of time. That was certainly the case a long time ago when writing a PhD dissertation. Since then, there have been postdoctoral fellowships and appointments, permanent and adjunct positions, and former, current, and future collaborators. And yet, con- versations spawn research ideas, which take many different turns and may divide up into a multitude of approaches or related or perhaps unrelated subjects. Again, one had better figure out with whom one likes to work. And again, in the process of writing this Brief, one needs create something bigger by focusing the relevant pieces of work into one (hopefully) coherent manuscript. It is an honor, a privi- lege, an amazing experience, and simply a lot of fun to be and have been working with all the people who have had an influence on our work and thereby on this book. To quote the late and great Jim Croce: ”If you dig it, do it. -
Discovery, Characterization, and Dynamics of Transiting Exoplanets
D ISCOVERY ,C HARACTERIZATION , AND DISCOVERY,CHARACTERIZATION, D AND YNAMICS YNAMICS OF D OF TRANSITING EXOPLANETS T RANSITING INCENT AN YLEN E V V E XOPLANETS –V INCENT V AN E YLEN Discovery,Characterization, and Dynamics of Transiting Exoplanets Vincent Van Eylen PhDThesis,November 2015 Advisor:Prof.Simon Albrecht Co-advisors:Prof.Hans Kjeldsen,Prof.Josh Winn Stellar Astrophysics Centre (SAC) Department of Physics and Astronomy Faculty of Science and Technology Aarhus University,Denmark Vincent Van Eylen Discovery, Characterization, and Dynamics of Transiting Exoplanets November 2015 phd thesis advisors: Prof. Simon Albrecht Prof. Hans Kjeldsen Prof. Josh Winn Aarhus University – Faculty of Science and Technology Department of Physics and Astronomy – Stellar Astrophysics Centre (SAC) Ny Munkegade 120, Building 1520, Aarhus, Denmark front image: All known transiting exoplanets to date. The size of the circles is proportional to the size of the planets, while the colors range from orange for planets larger than Jupiter, to blue for planets smaller than Earth. The eight planets in the solar system are shown in white. PREFACE When doing astronomy for a few years, at some point you inevitably find yourself dragged down to tiny details - stuck at a computer, writing, calcu- lating, computing. It can be easy to forget about cool science. But there is a cure! Fly to Gran Canaria. Ignore all the tour operators and the families on their way to an all-inclusive hotel, instead, take the next plane to La Palma. Say hello to the beach. Drive up the Roque de los Muchachos: enjoy an hour cruising up on the windy road from sea level up to 2000 meter. -
Ankara Üniversitesi Akademik Arşiv Sistemi
ANKARA ÜNİVERSİTESİ FEN BİLİMLERİ ENSTİTÜSÜ YÜKSEK LİSANS TEZİ DÜŞÜK GENLİKLİ δ SCUTI YILDIZI 20 CVn’NİN ELEMENT BOLLUK ÇALIŞMASI Tolgahan KILIÇOĞLU ASTRONOMİ VE UZAY BİLİMLERİ ANABİLİM DALI ANKARA 2008 Her hakkı saklıdır ÖZET Yüksek Lisans Tezi DÜŞÜK GENLİKLİ δ SCUTI YILDIZI 20 CVn’NİN ELEMENT BOLLUK ÇALIŞMASI Tolgahan KILIÇOĞLU Ankara Üniversitesi Fen Bilimleri Enstitüsü Astronomi ve Uzay Bilimleri Anabilim Dalı Danışman : Yrd. Doç. Dr. Kutluay YÜCE Eş Danışman: Prof. Dr. Saul J. ADELMAN Bu tez çalışmasında, 20 CVn (F3 III) yıldızının, Dominion Astrofizik Gözlemevi’ndeki (Victoria, Kanada) 1.2 m’lik teleskoba bağlı Coude tayfçekerindeki Reticon ve CCD algılayıcılarla elde edilen yüksek kaliteli tayflar kullanılarak atmosfer parametreleri ve element bollukları tespit edilmiştir. Optik bölgenin λλ3820-4940 Å dalgaboyu aralığını içeren tayflar, Dr. Graham Hill ve arkadaşları (Hill et al. 1982a,b) tarafından yazılan REDUCE ve VLINE programları kullanılarak ölçülmüştür. Her tayf çizgisine ait merkezi dalgaboyu, eşdeğer genişlik, derinlik ve yarı maksimumdaki tam genişlik değerleri bulundu. Atmosfer analizi, Dr. Robert L. Kurucz (Kurucz 1993)’un yerel termodinamik denge varsayımlı, paralel düzlem geometrili ATLAS9 ve O’nun ilgili programları kullanılarak gerçekleştirildi. 20 CVn’nin çizgi tanısı yapıldıktan sonra, atmosferindeki atom ve iyonlar tespit edilmiş oldu. Çizgi tanısı, benzer tür yıldızlar için yapılacak tayfsal çalışmalar için yararlı olacaktır. Etkin sıcaklık ve yüzey çekim ivmesi, gözlemsel ve kuramsal Hγ profillerinin karşılaştırılmasından, spektrofotometrik akıların, teorik profil ve akılarla karşılaştırılmasından ve nötr ve bir kez iyonlaşmış demir çizgileri kullanılarak demir elementinin iyonizasyon dengesinden elde edilmiştir. 20 CVn için elde -1 edilen değerler: Te = 6950 K and log g = 2.80 dir. Mikrotürbülans hızı 2.6 km sn olarak hesaplandı. -
Extreme Physical Phenomena Associated with Close-In Solid Exoplanets: Models and Consequences
EXTREME PHYSICAL PHENOMENA ASSOCIATED WITH CLOSE-IN SOLID EXOPLANETS: MODELS AND CONSEQUENCES by Prabal Saxena A Dissertation Submitted to the Graduate Faculty of George Mason University In Partial fulfillment of The Requirements for the Degree of Doctor of Philosophy Computational Sciences and Informatics Committee: Dr. Michael Summers, Dissertation Director Dr. Jie Zhang, Committee Member Dr. Robert Weigel, Committee Member Dr. Paul Cooper, Committee Member Dr. Kevin Curtin, Department Chair, Department of Computational and Data Sciences Dr. Donna M. Fox, Associate Dean, Office of Student Affairs Special Programs, College of Science Peggy Agouris, Dean, College of Science Date: Summer Semester 2015 George Mason University Fairfax, VA Extreme Physical Phenomena Associated with Close-In Solid Exoplanets: Models and Consequences A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy at George Mason University By Prabal Saxena Bachelor of Science Columbia University, 2007 Director: Dr. Michael Summers, Professor (School of Physics, Astronomy and Computational Sciences) Summer Semester 2015 George Mason University Fairfax, VA Copyright © 2015 by Prabal Saxena All Rights Reserved ii Dedication I dedicate this dissertation to anyone who is willing to read it! Also to a mischievous pug named Buddy and to a rambunctious cat named Scully. iii Acknowledgments None of the research produced as part of this dissertation could have been done without the support of my family, friends, and instructors. I am especially indebted to my wonderful parents, Praveen and Punam, my wife, Angela, and my brother, Pulkit. Additionally, the work produced by this thesis is underpinned by a large body of scien- tific and computational literature as well as software - I am grateful to the many hard working individuals who produced these products.