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Astronomie in Theorie Und Praxis 8. Auflage in Zwei Bänden Erik Wischnewski
Astronomie in Theorie und Praxis 8. Auflage in zwei Bänden Erik Wischnewski Inhaltsverzeichnis 1 Beobachtungen mit bloßem Auge 37 Motivation 37 Hilfsmittel 38 Drehbare Sternkarte Bücher und Atlanten Kataloge Planetariumssoftware Elektronischer Almanach Sternkarten 39 2 Atmosphäre der Erde 49 Aufbau 49 Atmosphärische Fenster 51 Warum der Himmel blau ist? 52 Extinktion 52 Extinktionsgleichung Photometrie Refraktion 55 Szintillationsrauschen 56 Angaben zur Beobachtung 57 Durchsicht Himmelshelligkeit Luftunruhe Beispiel einer Notiz Taupunkt 59 Solar-terrestrische Beziehungen 60 Klassifizierung der Flares Korrelation zur Fleckenrelativzahl Luftleuchten 62 Polarlichter 63 Nachtleuchtende Wolken 64 Haloerscheinungen 67 Formen Häufigkeit Beobachtung Photographie Grüner Strahl 69 Zodiakallicht 71 Dämmerung 72 Definition Purpurlicht Gegendämmerung Venusgürtel Erdschattenbogen 3 Optische Teleskope 75 Fernrohrtypen 76 Refraktoren Reflektoren Fokus Optische Fehler 82 Farbfehler Kugelgestaltsfehler Bildfeldwölbung Koma Astigmatismus Verzeichnung Bildverzerrungen Helligkeitsinhomogenität Objektive 86 Linsenobjektive Spiegelobjektive Vergütung Optische Qualitätsprüfung RC-Wert RGB-Chromasietest Okulare 97 Zusatzoptiken 100 Barlow-Linse Shapley-Linse Flattener Spezialokulare Spektroskopie Herschel-Prisma Fabry-Pérot-Interferometer Vergrößerung 103 Welche Vergrößerung ist die Beste? Blickfeld 105 Lichtstärke 106 Kontrast Dämmerungszahl Auflösungsvermögen 108 Strehl-Zahl Luftunruhe (Seeing) 112 Tubusseeing Kuppelseeing Gebäudeseeing Montierungen 113 Nachführfehler -
An Atlas of Far-Ultraviolet Spectra of the Zeta Aurigae Binary 31 Cygni with Line Identifications
The Astrophysical Journal Supplement Series, 211:27 (14pp), 2014 April doi:10.1088/0067-0049/211/2/27 C 2014. The American Astronomical Society. All rights reserved. Printed in the U.S.A. AN ATLAS OF FAR-ULTRAVIOLET SPECTRA OF THE ZETA AURIGAE BINARY 31 CYGNI WITH LINE IDENTIFICATIONS Wendy Hagen Bauer1 and Philip D. Bennett2,3 1 Whitin Observatory, Wellesley College, 106 Central Street, Wellesley, MA 02481, USA; [email protected] 2 Department of Astronomy & Physics, Saint Mary’s University, Halifax, NS B3H 3C3, Canada 3 Eureka Scientific, Inc., 2452 Delmer Street, Suite 100, Oakland, CA 94602-3017, USA Received 2013 March 29; accepted 2013 October 26; published 2014 April 2 ABSTRACT The ζ Aurigae system 31 Cygni (K4 Ib + B4 V) was observed by the FUSE satellite during total eclipse and at three phases during chromospheric eclipse. We present the coadded, calibrated spectra and atlases with line identifications. During total eclipse, emission from high ionization states (e.g., Fe iii and Cr iii) shows asymmetric profiles redshifted from the systemic velocity, while emission from lower ionization states (e.g., Fe ii and O i) appears more symmetric and is centered closer to the systemic velocity. Absorption from neutral and singly ionized elements is detected during chromospheric eclipse. Late in chromospheric eclipse, absorption from the K star wind is detected at a terminal velocity of ∼80 km s−1. These atlases will be useful for interpreting the far-UV spectra of other ζ Aur systems, as the observed FUSE spectra of 32 Cyg, KQ Pup, and VV Cep during chromospheric eclipse resemble that of 31 Cyg. -
FY08 Technical Papers by GSMTPO Staff
AURA/NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation July 23, 2008 Revised as Complete and Submitted December 23, 2008 NGC 660, ~13 Mpc from the Earth, is a peculiar, polar ring galaxy that resulted from two galaxies colliding. It consists of a nearly edge-on disk and a strongly warped outer disk. Image Credit: T.A. Rector/University of Alaska, Anchorage NATIONAL OPTICAL ASTRONOMY OBSERVATORY NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation December 23, 2008 TABLE OF CONTENTS EXECUTIVE SUMMARY ............................................................................................................................. 1 1 SCIENTIFIC ACTIVITIES AND FINDINGS ..................................................................................... 2 1.1 Cerro Tololo Inter-American Observatory...................................................................................... 2 The Once and Future Supernova η Carinae...................................................................................................... 2 A Stellar Merger and a Missing White Dwarf.................................................................................................. 3 Imaging the COSMOS...................................................................................................................................... 3 The Hubble Constant from a Gravitational Lens.............................................................................................. 4 A New Dwarf Nova in the Period Gap............................................................................................................ -
THE 1979 ECLIPSE of ZETA AURIGAE Robert D. Chapman
THE 1979 ECLIPSE OF ZETA AURIGAE Robert D. Chapman Laboratory forAstronomy and Solar Physics Goddard Space Flight Center Greenbelt, ND 20771 ABSTRACT Observations of the system ; Aurigae made around primary eclipse are described, and their significance is discussed in a preliminary fashion. THE OBSERVATIONS High-dispersion, long- and short-wavelength spectra of the atmospheric eclipsing binary star system ; Aurigae (K2II + B8V) have been obtained during a total of ten observing sessions between September 15, 1979 and March 31, 1980. Dates of observations, corresponding to numbered positions in Figure I are: (I) Sept. 15, (2) Nov. i, (3) Nov. 13, (4) Nov. 15, (S) Nov. 18, (6) Nov. 22, (7) Dec. 16, [8) Jan. 29, (9) Feb. 29, (10) Mar. 31. The spectrum obtained on Sept. 15 resembles the spectrum of a single late B-star [e.g. the B6V star o Eri). Atmospheric effects are present and increasing in strength between Nov. i and Nov. 18. To a first approximation, the spectrum changes appear to be an increase in strength and number of absorption lines with changes in the undisturbed continuum being small. This point requires further study, however. On Nov. 22, the B star had passed second contact, and the spectrum of the system was a pure emission line spectrum. At mid-eclipse, on Dec. 16 the spectrum had changed but little from its appearance on Nov. 22. The egress spectra obtained in 1980 are not significantly different in appearance from the ingress spectra. A study of differences in detail is being undertaken now. Figure 2 shows the behavior of the Fe II resonance lines in three spectra. -
Plotting Variable Stars on the H-R Diagram Activity
Pulsating Variable Stars and the Hertzsprung-Russell Diagram The Hertzsprung-Russell (H-R) Diagram: The H-R diagram is an important astronomical tool for understanding how stars evolve over time. Stellar evolution can not be studied by observing individual stars as most changes occur over millions and billions of years. Astrophysicists observe numerous stars at various stages in their evolutionary history to determine their changing properties and probable evolutionary tracks across the H-R diagram. The H-R diagram is a scatter graph of stars. When the absolute magnitude (MV) – intrinsic brightness – of stars is plotted against their surface temperature (stellar classification) the stars are not randomly distributed on the graph but are mostly restricted to a few well-defined regions. The stars within the same regions share a common set of characteristics. As the physical characteristics of a star change over its evolutionary history, its position on the H-R diagram The H-R Diagram changes also – so the H-R diagram can also be thought of as a graphical plot of stellar evolution. From the location of a star on the diagram, its luminosity, spectral type, color, temperature, mass, age, chemical composition and evolutionary history are known. Most stars are classified by surface temperature (spectral type) from hottest to coolest as follows: O B A F G K M. These categories are further subdivided into subclasses from hottest (0) to coolest (9). The hottest B stars are B0 and the coolest are B9, followed by spectral type A0. Each major spectral classification is characterized by its own unique spectra. -
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. -
Prof. Mustafa Türker ÖZKAN
Prof. Mustafa Türker ÖZKAN OPfefricseo Pnhaol nIen:f +or9m0 2a1t2io 4n40 0369 Extension: 10294 EFmaxa iPl:h oznkea:n +t@9i0s t2a1n2b u4l4.e0d u0.3tr70 AWdedbr:e hstst:p :A/s/tarvoenso.imstia vneb uUlz.eadyu B.tirli/molzekrai nBtö/lümü, İstanbul Üniversitesi Beyazıt Yerleşkesi, 34119, Fatih-İstanbul EDodcutocraatteio, İnst aInnbfuol rÜmniavetriosintesi, Faculty of Science, Astronomi Ve Uzay Bilimleri, Turkey 1981 - 1987 UPonsdtegrrgardaudautaet, eİs, tİastnabnublu Ül nÜinveivresritseitsei,s Fi, aFcauclutylt oy fo Sfc Siecniecnec, eA, sAtrsotrnoonmomi Vi eV Ue zUazya By iBlimilimlerlei,r Ti, uTrukrekye 1y 917987 3- 1- 9189077 FEnogrliesihg, nB2 L Uapnpgeru Iangteersmediate Dissertations ADsotcrtoonroamtey, G aünnde Sşp Laeckee Slecrieinndceks,i 1D9o8ğ7u-Batı Asimetrisinin Nedenleri Üzerine, Istanbul University, Faculty of Science, APostsrtognraodmuya taen, dP lSapnaect ev eS cÇieifnt-cYeısld, 1ız9 Y8ö0rüngelerinde Büyük Eksen Dönmesi, Istanbul University, Faculty of Science, Research Areas aPnhdy sOicbss, eArsvtartoionnosm, yS taanrsd, ANsattruorpahl ySsciicesn, cSeusn and Solar Systems, Astronomy and Astrophysics: Instrumentation Techniques Academic Titles / Tasks APrsosofecsiastoer ,P Irsotafensbsuolr U, Insitvaenrbsuitly U, Fnaivceurltsyit yo,f FSaccieunltcye o, Af sStcrioencoem, Ay satnrodn Sopmacye a Sncdie Snpcaecse, 1S9c9ie5n c- eCso, n1t9in9u0e -s 1995 RAessiesatarcnht PArsosfisetsasnotr, ,İ Issttaannbbuul lÜ Unniviveerrssititeys,i ,F Faaccuultlyty o of fS Sccieiennccee, ,A Asstrtroonnoommyy a anndd S Sppaaccee S Sccieienncceess, -
Magnetic Field, Chemical Composition and Line Profile Variability of The
Mon. Not. R. Astron. Soc. 000, 1–11 (2010) Printed 20 November 2018 (MN LATEX style file v2.2) Magnetic field, chemical composition and line profile variability of the peculiar eclipsing binary star AR Aur⋆ C.P. Folsom1†, O. Kochukhov2, G.A. Wade3, J. Silvester3,4, S. Bagnulo1 1Armagh Observatory, College Hill, Armagh Northern Ireland BT61 9DG 2Department of Astronomy and Space Physics, Uppsala University, 751 20 Uppsala, Sweden 3Department of Physics, Royal Military College of Canada, P.O. Box 17000, Station ‘Forces’, Kingston, Ontario, Canada, K7K 7B4 4Department of Physics, Engineering Physics & Astronomy, Queen’s University, Kingston, Ontario, Canada, K7L 3N6 Received: 2010; Accepted: 2010 ABSTRACT AR Aur is the only eclipsing binary known to contain a HgMn star, making it an ideal case for a detailed study of the HgMn phenomenon. HgMn stars are a poorly understood class of chemically peculiar stars, which have traditionally been thought not to possess significant magnetic fields. However, the recent discovery of line profile variability in some HgMn stars, apparently attributable to surface abundance patches, has brought this belief into question. In this paper we investigate the chemical abun- dances, line profile variability, and magnetic field of the primary and secondary of the AR Aur system, using a series of high resolution spectropolarimetric observations. We find the primary is indeed a HgMn star, and present the most precise abundances yet determined for this star. We find the secondary is a weak Am star, and is possibly still on the pre-main sequence. Line profile variability was observed in a range of lines in the primary, and is attributed to inhomogeneous surface distributions of some el- ements. -
Fy10 Budget by Program
AURA/NOAO FISCAL YEAR ANNUAL REPORT FY 2010 Revised Submitted to the National Science Foundation March 16, 2011 This image, aimed toward the southern celestial pole atop the CTIO Blanco 4-m telescope, shows the Large and Small Magellanic Clouds, the Milky Way (Carinae Region) and the Coal Sack (dark area, close to the Southern Crux). The 33 “written” on the Schmidt Telescope dome using a green laser pointer during the two-minute exposure commemorates the rescue effort of 33 miners trapped for 69 days almost 700 m underground in the San Jose mine in northern Chile. The image was taken while the rescue was in progress on 13 October 2010, at 3:30 am Chilean Daylight Saving time. Image Credit: Arturo Gomez/CTIO/NOAO/AURA/NSF National Optical Astronomy Observatory Fiscal Year Annual Report for FY 2010 Revised (October 1, 2009 – September 30, 2010) Submitted to the National Science Foundation Pursuant to Cooperative Support Agreement No. AST-0950945 March 16, 2011 Table of Contents MISSION SYNOPSIS ............................................................................................................ IV 1 EXECUTIVE SUMMARY ................................................................................................ 1 2 NOAO ACCOMPLISHMENTS ....................................................................................... 2 2.1 Achievements ..................................................................................................... 2 2.2 Status of Vision and Goals ................................................................................ -
Variable Star Section Circular
British Astronomical Association Variable Star Section Circular No 82, December 1994 CONTENTS A New Director 1 Credit for Observations 1 Submission of 1994 Observations 1 Chart Problems 1 Recent Novae Named 1 Z Ursae Minoris - A New R CrB Star? 2 The February 1995 Eclipse of 0¼ Geminorum 2 Computerisation News - Dave McAdam 3 'Stella Haitland, or Love and the Stars' - Philip Hurst 4 The 1994 Outburst of UZ Bootis - Gary Poyner 5 Observations of Betelgeuse by the SPA-VSS - Tony Markham 6 The AAVSO and the Contribution of Amateurs to VS Research Suspected Variables - Colin Henshaw 8 From the Literature 9 Eclipsing Binary Predictions 11 Summaries of IBVS's Nos 4040 to 4092 14 The BAA Instruments and Imaging Section Newsletter 16 Light-curves (TZ Per, R CrB, SV Sge, SU Tau, AC Her) - Dave McAdam 17 ISSN 0267-9272 Office: Burlington House, Piccadilly, London, W1V 9AG Section Officers Director Tristram Brelstaff, 3 Malvern Court, Addington Road, READING, Berks, RG1 5PL Tel: 0734-268981 Section Melvyn D Taylor, 17 Cross Lane, WAKEFIELD, Secretary West Yorks, WF2 8DA Tel: 0924-374651 Chart John Toone, Hillside View, 17 Ashdale Road, Cressage, Secretary SHREWSBURY, SY5 6DT Tel: 0952-510794 Computer Dave McAdam, 33 Wrekin View, Madeley, TELFORD, Secretary Shropshire, TF7 5HZ Tel: 0952-432048 E-mail: COMPUSERV 73671,3205 Nova/Supernova Guy M Hurst, 16 Westminster Close, Kempshott Rise, Secretary BASINGSTOKE, Hants, RG22 4PP Tel & Fax: 0256-471074 E-mail: [email protected] [email protected] Pro-Am Liaison Roger D Pickard, 28 Appletons, HADLOW, Kent TN11 0DT Committee Tel: 0732-850663 Secretary E-mail: [email protected] KENVAD::RDP Eclipsing Binary See Director Secretary Circulars Editor See Director Telephone Alert Numbers Nova and First phone Nova/Supernova Secretary. -
Výročná Správa Za Rok 2005
2005 3.1. Research output – publications 3. Monographs published in Slovakia 1. PITTICH, E.M. Astronomická ročenka 2006. Hurbanovo: Slovenská ústredná hvezdáreň, 2005. ISBN 80-85221-50-0. p. 1-272. (in Slovak) 7. Chapters in monographs published in Slovakia 2. HRIC, L. Premenné hviezdy. In PITTICH, E.M. Astronomická ročenka 2006. Hurbanovo: Slovenská ústredná hvezdáreň, 2005. ISBN 80-85221-50-0. p. 186-202. (in Slovak) 3. PITTICH, E. Čas, obloha od januára do decembra. In PITTICH, E.M. Astronomická ročenka 2006. Hurbanovo: Slovenská ústredná hvezdáreň, 2005. ISBN 80-85221-50-0. p. 3-89. (in Slovak) 4. PITTICH, E. Pohyb planét po oblohe, elongácie a jasnosti, Mesiac krátko po nove. In PITTICH, E.M. Astronomická ročenka 2006. Hurbanovo: Slovenská ústredná hvezdáreň, 2005. ISBN 80-85221-50-0. p. 90-103. (in Slovak) 5. PITTICH, E. Kométy. In PITTICH, E.M. Astronomická ročenka 2006. Hurbanovo: Slovenská ústredná hvezdáreň, 2005. ISBN 80-85221-50-0. p. 106-143. (in Slovak) 6. PITTICH, E. Galileiho mesiace. In PITTICH, E.M. Astronomická ročenka 2006. Hurbanovo: Slovenská ústredná hvezdáreň, 2005. ISBN 80-85221-50-0. p. 159-172. (in Slovak) 7. PITICHOVÁ, J. Kométy roka 2004. In PITTICH, E.M. Astronomická ročenka 2006. Hurbanovo: Slovenská ústredná hvezdáreň, 2005. ISBN 80-85221-50-0. p. 241-268. (in Slovak) 8. PORUBČAN, V. Meteorické roje. In PITTICH, E.M. Astronomická 2006. Hurbanovo: Slovenská ústredná hvezdáreň, 2005. ISBN 80-85221-50-0. p. 104-105. (in Slovak) 9. SVOREŇ, J. Teórie vzniku a vývoja asteroidov. In PITTICH, E.M. Astronomická ročenka 2006. Hurbanovo: Slovenská ústredná hvezdáreň, 2005. -
Variable Star Classification and Light Curves Manual
Variable Star Classification and Light Curves An AAVSO course for the Carolyn Hurless Online Institute for Continuing Education in Astronomy (CHOICE) This is copyrighted material meant only for official enrollees in this online course. Do not share this document with others. Please do not quote from it without prior permission from the AAVSO. Table of Contents Course Description and Requirements for Completion Chapter One- 1. Introduction . What are variable stars? . The first known variable stars 2. Variable Star Names . Constellation names . Greek letters (Bayer letters) . GCVS naming scheme . Other naming conventions . Naming variable star types 3. The Main Types of variability Extrinsic . Eclipsing . Rotating . Microlensing Intrinsic . Pulsating . Eruptive . Cataclysmic . X-Ray 4. The Variability Tree Chapter Two- 1. Rotating Variables . The Sun . BY Dra stars . RS CVn stars . Rotating ellipsoidal variables 2. Eclipsing Variables . EA . EB . EW . EP . Roche Lobes 1 Chapter Three- 1. Pulsating Variables . Classical Cepheids . Type II Cepheids . RV Tau stars . Delta Sct stars . RR Lyr stars . Miras . Semi-regular stars 2. Eruptive Variables . Young Stellar Objects . T Tau stars . FUOrs . EXOrs . UXOrs . UV Cet stars . Gamma Cas stars . S Dor stars . R CrB stars Chapter Four- 1. Cataclysmic Variables . Dwarf Novae . Novae . Recurrent Novae . Magnetic CVs . Symbiotic Variables . Supernovae 2. Other Variables . Gamma-Ray Bursters . Active Galactic Nuclei 2 Course Description and Requirements for Completion This course is an overview of the types of variable stars most commonly observed by AAVSO observers. We discuss the physical processes behind what makes each type variable and how this is demonstrated in their light curves. Variable star names and nomenclature are placed in a historical context to aid in understanding today’s classification scheme.