DOCSLIB.ORG

Csillagászati Évkönyv Az 1955

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Csillagászati Évkönyv Az 1955 302268 CSILLAGÁSZATI ÉVKÖNYV AZ 1955. ÉVRE Tartalomjegyzékből: E. Schatzman: Kritikai megjegyzések Európában és Amerikában elterjedt kozmogóniai elméletekről.7 — Dezső Lóránt: A napfogyatkozások geometriája — Izsák Imre: Hogyan mérték meg a Hold és a Nap távolságát.— Voroncov-Veljaminov: Asztrofizika. »MŰVELT NÉP« TÜDOMÁNYOS ÉS ISMERETTERJESZTŐ KIADÓ CSILLAGASZATI ÉVKÖNYV AZ 1955. ÉVRE SZERKESZTETTE: A TÁRSADALOM ÉS TERMÉSZETTUDOMÁNYI ISMERETTERJESZTŐ TÁRSULAT CSILLAGÁSZATI SZAKOSZTÁLYA »MŰ VÉLT NÉP« ' TUDOMÁNYOS é s ismeretterjesztő k i a d ó BUDAPEST, 1955 A kiadásért felel a Művelt Nép Könyvkiadó igazgatója Felelős szerkesztő: Neu Piroska Műszaki felelős: Löblin Imre t Kézirat beérkezett: 1954. XII. 2. Imprimálva: 1955. II. 15. Terjedelem: 14 (A 5) ív Példányszám: 15oo Ez a könyv a MNOSZ 5601-54 és 5602-50Á szabvány szerint készült Budapesti Szikra Nyomda, V., Honvéd-u. 10. —■ 4667 — Felelős vezető: Lengyel Lajos igazgató CSILLAGÁSZATI ADATOK AZ 1955. ÉVRE » A közép-európai zónaidőben megadott értékekhez a nyári időszámítás tartama alatt 1 órát kell hozzáadni, hogy a Magyarországon használt időadatokat nyerjük. Összeállította: Mersits József tudományos munkaerő a Magyar Tudományos Akadémia Csillagvizsgáló Intézeténél l* I. J A N U Á R Közép-európai zónaidőben Budapesten A NAP A HOLD A A HOLD hete nyug­ nyug­ napja fényváltozásai Dátum A hét napjai : Az év hányadik kel Az év Az év hányadik kel delel szik szik h m h m h m h m h m h m 1 Sz 1 i 7 32 11 47 16 03 10 42 _ _ D 21 29 2 v ■ 2 7 32 11 48 16 05 11 07 0 20 3 H 2 3 7 32 11 48 16 06 11 35 1 38 4 K 4 7 32 11 49 16 06 12 10 2 57 5 Sz 5 7 32 11 49 16 07 12 55 4 15 6 Cs 6 7 32 11 50 16 08 13 53 5 28 7 P 7 7 32 11 50 16 09 15 02 6 30 '8 Sz 8 7 31 11 51 16 10 16 19 7 19 © 13 34 9 V 9 7 31 11 51 16 12 17 38 7 57 10 H 3. 10 7 30 11 51 16 13 18 55 8 27 11 K 11 7 30 11 52 16 14 20 09 8 52 12 Sz 12 7 29 11 52 16 16 21 20 9 13 13 Cs 13 7 29 11 52 16 17 22 28 9 34 14 P 14 7 29 11 53 16 19 23 35 9 53 15 Sz 15 7 28 11 53 16 20 ------- 10 24 C 23 13 16 V 16 7 28 11 53 16 21 0 40 10 37 17 H 4 17 7 27 11 54 16 22 1 45 11 03 18 K 18 7 26 11 54 16 24 2 48 11 35 19 Sz 19 7 25 11 55 16 25 3 49 12 14 20 Cs 20 7 24 11 55 16 27 4 44 13 01 21 P 21 7 23 11 55 16 28 5 33 13 56 22 Sz 22 7 22 11 56 16 30 6 15 14 59 23 V 23 7 22 11 56 16 31 6 49 16 07 @ 2 06 24 H 5 24 7 21 11 56 16 32 7 19 17 17 25 K 25 7 20 11 56 16 34 7 44 18 29 26 Sz 26 7 19 11 56 16 35 8 06 19 42 27 Cs 27 7 17 11 57 16 37 8 27 20 55 28 R 28 7 16 11 57 16 39 8 49 22 10 29 Sz 29 7 15 11 57 16 40 9 12 23 26 30 V 30 7 14 11 57 16 42 9 39 ------ - 31 H 6 31 7 13 11 57 16 43 10 11 0 44 -$> 6 05 Nap: 4-én lS^-kor földközelben. Hold: 6-án 10h-kor földközelben, látszólagos sugara: 16'28", 8 18-án 4h-kor földtávolban, látszólagos sugara : 14'46", 9 4 HÓNAP 0h v i 1 á g i d ő k o r A NAP A HOLD Julián Csillagidő* dátum (Z = 0°-nál) 2435... rekta- dekliná­ látszó­ rekta- dekliná­ szcenziója ciója sugara szcenziója ciója h m s h m o / t n h m O / ...108,5 6 39 29,297 18 43 - 23 05 16 18 23 48 + 4 23 109,5 6 43 25,855 18 47 23 00 16 18 0 38 9 51 110,5 6 47 22,413 18 51 22 55 16 18 1 32 14 56 111,5 651 18,971 18 56 22 49 16 18 2 29 19 16 112,5 6 55 15,530 19 00 22 43 16 18 3 30 22 29 113,5 6 59 12,088 19 05 22 37 16 18 4 34 24 14 114,5 7 03 08,646 19 09 22 30 16 18 5 38 24 19 115,5 7 07 05,204 19 13 22 22 16 18 6 42 22 42 116,5 7 11 01,762 19 18 22 15 16 18 7 43 19 36 117,5 7 14 58,319 19 22 22 06 16 18 4 40 15 23 118,5 7 18 54,877 19 26 21 57 16 18 9 33 10 27 119,5 7 22 51,435 19 31 21 48 16 18 10 23 + 5 09 120,5 7 26 47,993 19 35 21 39 16 18 11 11 — 0 12 121,5 7 30 44,550 19 39 21 29 16 18 11 57 5 24 122,5 7 34 41,108 19 44 21 18 16 18 12 43 10 14 123,5 7 3837,665 1948 21 07 16 17 13 29 14 36 124,5 7 42 34,223 19 52 20 56 16 17 14 16 18 19 125,5 7 46 30,780 19 57 20 44 16 17 15 04 21 17 126,5 7 50 27,337 20 01 20 32 16 17 15 55 23 21 127,5 7 54 23,894 20 05 20 20 16 17 16 47 24 23 128,5 7 58 20,451 20 09 20 07 16 17 17 40 24 17 129,5 8 02 17,008 20 14 19 54 16 17 18 33 23 02 130,5 8 06 13,565 20 18 19 40 16 17 19 26 20 39 131,5 8 10 10,122 20 22 19 26 16 17 20 18 17 14 132,5 8 14 06,678 20 26 19 12 16 17 21 08 12 56 133,5 8 18 03,235 20 30 18 58 16 17 21 58 7 58 134,5 8 21 59,791 20 35 18 43 16 16 22 47 — 2 33 135,5 8 25 56,348 20 39 18 27 16 16 23 36 + 3 03 136,5 82952,904 2043 1812 16 16 0 27 8 34 137,5 8 33 49,460 20 47 17 56 16 16 1 20 13 43 138,5 8 37 46,016 20 51 — 17 39 16 16 2 15 + 18 11 *A Berliner Asironomisches Jahrbuch nyomán az a valódi csillagidő, amely a nutációnak a hosszúperiódusú tagját magában foglalja (de a rövidperiódusút nem). 5 I. FEBRUÁR Közép-európai zónaidőben Budapesten a A NAP A HOLD g A HOLD nyug­ fényváltozásai hete nyug­ napja kel A A hét napjai Az év hányadik Q Az év hányadik kel ’delel szik szik h m h m h m h m h m h m 1 K (6) 32 .7 12 11 57 16 44 10 51 2 01 2 Sz 33 7 10 11 58 16 46 11 41 3 13 3 Cs 34 7 09 11 58 16 48 12 43 4 17 4 P 35 7 07 11 58 16 50 13 55 5 10 5 Sz 36 7 06 11 58 16 51 15 12 5 52 6 V 37 7 05 11 58 16 53 16 29 6 25 7 H 7 38 7 04 11 58 16 54 17 45 6 52 ® 2 43 8 K 39 7 02 11 58 16 55 18 57 7 15 9 Sz 40 7 00 11 58 16 57 20 08 7 36 10 Cs 41 6 59 11 58 16 59 21 16 7 57 11 P 42 6 57 11 58 17 01 22 23 8 17 12 Sz 43 6 56 11 58 17 02 23 29 8 40 13 V 44 6 55 11 58 17 04 —— 9 05 14 H 8 45 6 53 11 58 17 05 0 24 9 34 (g; 20 40 15 K 46 6 51 11 58 17 07 1 36 10 10 16 Sz 47 6 49 11 58 17 08 2 33 10 53 17 Cs 48 6 47 11 58 17 10 3 25 11 44 18 P 49 6 45 11 58 17 12 4 10 12 44 19 Sz 50 6 44 11 58 17 13 4 47 13 49 20 V 51 6 43 11 58 17 14 5 18 14 59 21 II 9 52 6 41 11 58 17 16 5 44 16 11 22 K 53 6 39 11 58 17 17 6 09 17 25 ® 16 54 23 Sz 54 6 37 11 58 17 19 6 32 18 39 24 Cs 55 6 35 11 57 17 21 6 54 19 56 25 P 56 6 34 11 57 17 23 7 17 21 13 26 Sz 57 £ 11 57 17 23 7 44 22 32 0 32 27 V 58 11 57 17 24 8 16 23 50 0 30 28 H 10 59 17 26 8 52 6 28 11 57 Hold: 2-án 20h-kor földközelben, látszólagos sugara: 16' 10", 4 16-án lh-kor földtávolban, látszólagos sugara : 14'48", 2 27-én 14h-kor földközelben, látszólagos sugara: 16' 11", 8 6 HÓNAP 0h v 1 á g i d ő k o r A NAP A HOLD Julián Csillagidő dátum (X = 0°-nál) 2435..
Load more

Recommended publications
  • Comparing Catelan's Equations to Distances from GAIA Using an RR
    Comparing Catelan's equations to distances from GAIA using an RR Lyrae type star, SW Andromedae by Talon Dow A senior thesis submitted to the faculty of Brigham Young University - Idaho in partial fulfillment of the requirements for the degree of Bachelor of Science Department of Physics Brigham Young University - Idaho March 2021 1 Copyright ©2021 Talon Dow All Rights Reserved 2 BRIGHAM YOUNG UNIVERSITY - IDAHO DEPARTMENT APPROVAL of a senior thesis submitted by Talon Dow This thesis has been reviewed by the research advisor, research coordinator, and department chair and has been found to be satisfactory. Date Stephen McNeil, Advisor Date Stephen Turcotte, Committee Member Date Brian Tonks, Committee Member Date R. Todd Lines, Chair 3 Abstract COMPARING CATELAN'S EQUATIONS TO DISTANCES FROM GAIA USING AN RR LYRAE TYPE STAR, SW ANDROMEDAE Talon Dow Department of Physics and Astronomy Bachelor of Science In this project, we try to establish how accurate Catelans' equations are using a RR Lyrae star, SW Andromedae. Utilizing telescopes from the Las Cumbres Observatory, we took data of the star over two weeks in the V, i, Z and B filters. Using that data and metallicity obtained from several different journal articles, we obtain an average distance to the star of 447 + = − 30 parsecs. That distance is not within the distance recorded by GAIA which is 562 + = − 52 parsecs. Our methodology is explained and can be duplicated to rerun our measurements. 4 Acknowledgements I would like to thank Michael Fitzgerald, the creator of this project and the time he spent creating the videos for us to learn of off.
    [Show full text]
  • Dark Matter 101
    DARK MATTER 101 DARK MATTER 101 From production to detection David G. Cerdeno˜ CONTENTS 1 Motivation for dark matter 1 1.1 Motivation for Dark Matter 1 1.1.1 Galactic scale 2 1.1.2 Galaxy Clusters 3 1.1.3 Cosmological scale 4 1.2 Dark Matter properties 5 1.2.1 Neutral 5 1.2.2 Nonrelativistic 5 1.2.3 NonBaryonic 6 1.2.4 Long-lived 6 1.2.5 Collisionless 7 2 Freeze Out of Massive Species 9 2.1 Cosmological Preliminaries 9 2.2 Time evolution of the number density 12 2.2.1 Freeze out of relativistic species 15 2.2.2 Freeze out of non-relativistic species 16 2.2.3 WIMPs 17 2.3 Computing the DM annihilation cross section 17 2.3.1 Special cases 18 v vi CONTENTS 3 Direct DM detection 23 3.1 Preliminaries 23 3.1.1 DM flux 23 3.1.2 Kinematics 23 3.2 The master formula for direct DM detection 24 3.2.1 The scattering cross section 24 3.2.2 The importance of the threshold 25 3.2.3 Velocity distribution function 26 3.2.4 Energy resoultion 26 3.3 Exponential spectrum 26 3.4 Annual modulation 26 3.5 Directional detection 27 3.6 Coherent neutrino scattering 27 3.7 Inelastic 27 4 Neutrinos 29 4.1 Preliminaries - copied form internet 29 References 31 CHAPTER 1 MOTIVATION FOR DARK MATTER The existence of a vast amount of dark matter (DM) in the Universe is supported by many astrophysical and cosmological observations.
    [Show full text]
  • Dissertation
    Dissertation submitted to the Instituto de Astrofísica, Facultad de Física Pontificia Universidad Católica de Chile, Chile for the degree of Doctor in Astrophysics submitted to the Combined Faculties for the Natural Sciences and for Mathematics of the Ruperto-Carola University of Heidelberg, Germany for the degree of Doctor of Natural Sciences Put forward by M.Sc. Gergely Hajdu Born in Miskolc, Hungary Oral examination: 06 August 2019 Structure of the obscured Galactic disk with pulsating variables Gergely Hajdu Referees: Prof. Dr. Márcio Catelan Prof. Dr. Eva Grebel ABSTRACT Bright pulsating variables, such as Cepheids and RR Lyrae, are prime probes of the structure of both the young and old stellar components of the Milky Way. However, the far side of the Galactic disk has not yet been mapped using such variables as tracers, due to the severe extinction caused by foreground interstellar dust. In this thesis, the near-infrared light curves from the VISTA Variables in the Vía Láctea survey are utilized to penetrate these regions of high extinction and thus discover thou- sands of previously “hidden” Cepheid and RR Lyrae variables. The analysis of the light curves of RR Lyrae variables, was performed with a newly developed fitting algorithm, and their metallicities determined from their near-infrared light-curve shapes, using a newly developed method. These photometric metal abundances, combined with their positions within the Galactic disk, lend support to theories of an early, inside-out forma- tion of the Galactic disk. The newly discovered Cepheids were classified into the old (Type II) and young (Clas- sical) subtypes. A new near-infrared extinction law was determined using the Type II Cepheids, taking advantage of their concentration around the Galactic center.
    [Show full text]
  • ´Etoiles Variables
    Diplˆome d’E´tudes Approfondies en Astrophysique et G´eophysique ETOILES´ VARIABLES R. Scuflaire Institut d’Astrophysique et de G´eophysique Universit´e de Li`ege 1999–2000 i Avertissement Les pr´esentes notes ne pr´etendent pas couvrir de fa¸con exhaustive et de fa¸con d´etaill´ee tous les types d’´etoiles variables. Elles d´ecrivent seulement quelques types ´evoqu´esdans le cours de Stabilit´eStellaire organis´e`al’Institut d’Astrophysique et de G´eophysique de l’Universit´ede Li`ege dans le cadre du D.E.A. en Astrophysique et G´eophysique. La plupart des types d´ecrits ici appartiennent `ala classe des variables intrins`eques. Les choix effectu´esse justifient par la signification particuli`ere de ces variables vis-`a-vis de la th´eorie de l’´evolution stellaire, par la compr´ehension que nous avons des m´ecanismes de variabilit´e et par les liens entretenus avec la th´eorie de la stabilit´estellaire. Nous avons utilis´enombre de figures tir´ees de la litt´erature pour illustrer le cours. Les r´ef´erences de ces emprunts figurent `ala fin de chaque chapitre. ii iii Table des mati`eres 1 Introduction 1 1.1 Nomenclature des ´etoiles variables . 2 1.2 Classification spectrale des ´etoiles . 2 1.3 Populations stellaires . 2 1.4 Evolution stellaire . 3 2 Classification des ´etoiles variables 5 2.1 Variables pulsantes . 6 2.2 Variables en rotation . 7 2.3 Variables´eruptives ............................... 8 2.4 Variables cataclysmiques . 8 2.5 Diagrammes HR des ´etoiles variables . 8 3 Variables de type RR Lyr (RR) 13 4 Variables de type δ Cep (DCEP) 19 5 Variables de type W Vir (CW) 25 6 Variables de type RV Tau (RV) 29 7 Variables de type Mira (M) 31 8 Variables semi-r´eguli`eres (SR) et irr´eguli`eres (L) 37 9 Variables des types δ Sct (DSCT) et SX Phe (SXPHE) 39 10 Variables de type β Cep (BCEP) 45 11 Etoiles B `araies variables 49 iv 12 Variables compactes 55 13 Oscillations solaires 59 13.1 L’oscillation `a5 minutes .
    [Show full text]
  • Ian J. M. Crossfield Appointments & Experience Education
    Ian J. M. Crossfield http://www.mit.edu/∼iancross/ Massachusetts Institute of Technology, Physics Department [email protected] MIT Kavli Institute +1 949 923-0578 (USA) 77 Massachusetts Avenue, Cambridge, MA 02139 Appointments & Experience MIT Department of Physics Assistant Professor 07/2017- present • Discovery of new planets using TESS, studying planets' atmospheres using HST and ground-based tele- scopes, new isotopic measurements of cool dwarfs. University of California, Santa Cruz Adjunct Professor 12/2017- present Associate Researcher 06/2017- 07/2017 Sagan Fellow 08/2016- 05/2016 • Continued the discovery of new planets using K2 and characterizing their atmospheres with ground- and space-based telescopes. U. Arizona, Lunar and Planetary Lab Sagan Fellow 07/2014 - 08/2016 • Work to understand hazy atmospheres of extrasolar objects: cloud properties and molecular abundances in known `super-Earth' planets; discovering new transiting planets with the K2 mission. Max Planck Institut f¨urAstronomie Postdoctoral Fellow 07/2012 - 06/2014 • Extrasolar planet atmosphere characterization via transits and secondary eclipses from ground- and space-based observatories. High-resolution spectroscopy of nearby brown dwarfs. University of California, Los Angeles Graduate Studies 09/2007 - 06/2012 • Characterization of exoplanet atmospheres via phase curves, secondary eclipses, and transits. Refined parameters of known transiting planets via optical transit photometry. NASA/Jet Propulsion Laboratory Systems Engineer 07/2004 - 06/2007 • High-contrast instrument performance simulations for the Gemini Planet Imager and TMT Planet For- mation Instrument. Optical testbed work for the Space Interferometry Mission. Exoplanet science. Education University of California, Los Angeles, Los Angeles, California USA • Ph.D., Astrophysics (Dissertation Year Fellow), 06/2012 Advisor: Prof.
    [Show full text]
  • Variable Star Section Circular
    British Astronomical Association VARIABLE STAR SECTION CIRCULAR No 152, June 2012 Contents Variable Star Section Display, Winchester 2012 - R. Pickard....inside front cover From the Director - R. Pickard ........................................................................... 1 The Astronomer/BAAVSS Meeting, 13 Oct 2012 - G. Hurst ............................ 3 John Bortle joins the 200K club - J. Toone ...................................................... 3 One Quarter Million and Counting - G. Poyner ............................................... 5 Eclipsing Binary News - D. Loughney .............................................................. 9 Observer Profile - J. Bortle ............................................................................. 11 An Encounter with RR Lyrae Stars. No.3 - G. Salmon .................................. 13 Light Curve of Eclipsing Contact Binary, SW Lacertae - L. Corp ................... 18 UK Night Time Cloud Cover - J. Toone .......................................................... 19 Binocular Priority List - M. Taylor ................................................................. 20 Eclipsing Binary Predictions - D. Loughney .................................................... 21 Charges for Section Publications .............................................. inside back cover Guidelines for Contributing to the Circular .............................. inside back cover ISSN 0267-9272 Office: Burlington House, Piccadilly, London, W1J 0DU VARIABLE STAR SECTION DISPLAY, WINCHESTER 2012 ROGER
    [Show full text]
  • Arthur Louis Day 27 by Philip H
    http://www.nap.edu/catalog/570.html We ship printed books within 1 business day; personal PDFs are available immediately. Biographical Memoirs V.47 Office of the Home Secretary, National Academy of Sciences ISBN: 0-309-59892-3, 560 pages, 6 x 9, (1975) This PDF is available from the National Academies Press at: http://www.nap.edu/catalog/570.html Visit the National Academies Press online, the authoritative source for all books from the National Academy of Sciences, the National Academy of Engineering, the Institute of Medicine, and the National Research Council: • Download hundreds of free books in PDF • Read thousands of books online for free • Explore our innovative research tools – try the “Research Dashboard” now! • Sign up to be notified when new books are published • Purchase printed books and selected PDF files Thank you for downloading this PDF. If you have comments, questions or just want more information about the books published by the National Academies Press, you may contact our customer service department toll- free at 888-624-8373, visit us online, or send an email to [email protected]. This book plus thousands more are available at http://www.nap.edu. Copyright © National Academy of Sciences. All rights reserved. Unless otherwise indicated, all materials in this PDF File are copyrighted by the National Academy of Sciences. Distribution, posting, or copying is strictly prohibited without written permission of the National Academies Press. Request reprint permission for this book. i e h t be ion. om r ibut f r t cannot r at not o f however, version ng, i t paper book, at ive at rm o Biographical Memoirs riginal horit ic f o e h NATIONAL ACADEMY OF SCIENCES t he aut t om r as ing-specif t ion ed f peset y http://www.nap.edu/catalog/570.html Biographical MemoirsV.47 publicat her t iles creat is h t L f M of and ot X om yles, r f st version print posed e h heading Copyright © National Academy ofSciences.
    [Show full text]
  • Vereinigung Der Sternfreunde E. V
    Diese Seite enthält im Original Werbung EDITORIAL 1 Liebe Mitglieder, liebe Sternfreunde, mit einem neuen Titellayout präsentiert Auf diesen Seiten – komplett in Farbe – 4. August in Hobbach bei Aschaffenburg sich unsere Mitgliederzeitschrift „Journal schreiben Sternfreunde für ihre Kollegen/ stattfinden, welches von der VdS veran- für Astronomie“. Auf Ihre Reaktionen innen und informieren so unsere große staltet wird. Besten Dank schon heute zum Titel und Inhalt sind wir sehr Zahl von Vereinsmitgliedern über die an die Verantwortlichen und Aktiven gespannt! Ergebnisse ihrer Beobachtungen. Bei dieses Lagers! Und bis zum Jahresende Wir bedanken uns bei all unseren diesem enormen Umfang unserer Zeit- soll die erste, komplette VdS-Einsteiger- Autoren, Mitgliedern, Fachgruppen und schrift macht es Sinn über eine dritte schrift vorliegen! den Sponsoren, die wieder mit dazu bei- Ausgabe im Jahr nachzudenken... getragen haben, daß die vorliegende Um noch effektiver auf die Wünsche und Ausgabe unserer Zeitschrift einen neuen Der Themenschwerpunkt dieses Journals Erwartungen unserer Mitglieder einge- Rekord aufstellt. Vor Ihnen liegen 160 gilt den Planeten und ihren Beob- hen zu können, legen wir dieser Seiten(!) geballter Amateur-Astronomie, achtern, um die es in den letzten Jahren Ausgabe nochmals den Fragebogen bei, die aus über 100 Beiträgen zusammen- etwas ruhiger geworden war. Nach der der im Dezemberheft aus technischen gestellt wurden. großartigen Jupiter- und Saturnopposition Gründen eingebunden war. befindet sich unser roter Nachbarplanet Wenn Sie ihn bereits an die Geschäfts- Mars derzeit in Opposition. Leider bietet stelle gesandt hatten, so danken wir die südliche Stellung in der Milchstrasse Ihnen herzlich dafür. Alle anderen nicht eben ideale Beobachtungsbeding- Mitglieder bitten wir erneut, die wenigen ungen.
    [Show full text]
  • Csillagászati Évkönyv Az 1954
    CSILLAGÁSZATI ÉVKÖNYV AZ 1954. ÉVRE % • Tartalomjegyzékből: Róka Gedeon: Csillagászat és dialektika. — Herczeg Tibor: Az égitestek rádiófrekvenciás sugár­ zása. — Guman István: Távolságmérés a változó csillagok segítségével. — Dezső Lóránt—Gerlei Ottó: A naptevékenység és a bolygók. — Csada Imre: A csillagok mágnessége. — Zerinváry Szilárd: A szov­ jet csillagászat új eredményei. MŰVELT NÉP KÖNYVKIADÓ CSILLAGÁSZATI ÉVKÖNYV AZ 1954. ÉVRE ( SZERKESZTETTE A TÁRSADALOM ÉS TERMÉSZETTUDOMÁNYI ISMERETTERJESZTŐ TÁRSULAT CSILLAGÁSZATI SZAKOSZTÁLYA MŰVELT NÉP KÖNYVKIADÓ BUDAPEST, 1954 A kiadásért felel a Művelt Nép Könyvkiadó Igazgatója Felelős szerkesztő: Neu Piroska Műszaki vezető: Löblln Imre Kézirat beérkezett: 1953. X I. 27. Példányszám: 1500. — Imprlmálva: 1954. II. 5. Terjedelem: 17.5 (A/5) Ív Ez a könyv a MNOSZ 5601—50Á és 5602—50Á szabványok szerint készült. Budapesti Szikra Nyomda, V., Honvéd-u. 10. — 16078 Felelős vezető: Lengyel Lajos Igazgató CSILLAGÁSZATI ADATOK AZ 1954. ÉVRE Összeállították: Csada Imre és Guman István tudomá­ nyos kutatók, Mersits József tudományos munkaerő a Magyar Tudományos Akadémia Csillagvizsgáló Intézeténél I. JANUÁR Középeurópai zónaidőber Budapesti :n £ A NAP A HOLD hete nyug­ nyug­ napja féhyváltozásai A A hét napjai Az Az év hányadik A A HOLD Az év Az év hányadik kel delel kel Q szik szik h m h m h m h m h m h m 1 p 1 i 7 32 11 47 16 03 4 12 12 41 2 Sz 2 7 32 11 48 16 05 5 18 13 22 3 V 3 7 32 11 48 16 06 6 17 14 16 4 H ' 2 4 7 32 11 49 16 06 7 10 15 20 5 K 5 7 32 11 49 16 07 7 52 16 34 % 2 21 6 Sz 6 7 32
    [Show full text]
  • A Summary of the Different Classes of Stellar Pulsators
    A Summary of the Different Classes of Stellar Pulsators A summary of all the classes of pulsating stars and their main properties as described in Chapter 2 is given in the tables below. This list originated from a combination of observational discoveries, measured stellar properties, and theoretical developments. Observers who found a new type of pulsator either named it after the prototype or gave the class a name according to the ob- served characteristics of the oscillations. Several pulsators, or even groups of pulsators, were afterwards found to originate from the same physical mech- anism and were thus merged into one and the same class. We sort this out here in Tables A.1 and A.2 in order to avoid further confusion on pulsating star nomenclature. The effective temperature and luminosity indicated in Tables A.1 and A.2 should be taken as rough indications only of the borders of instability strips. Often the theory is not sufficiently refined to consider these boundaries as final. Moreover, there is overlap between various classes where so-called hy- brid pulsators, whose oscillations are excited in two different layers and/or by two different mechanisms, occur. Finally, new discoveries are being made frequently, which then drive new theoretical developments possibly leading to new instability regions. The results from the future observing facilities as described in Chapter 8 will surely lead to new classes and/or subclasses with lower amplitudes compared to what is presently achievable. In the tables below, F stands for fundamental radial mode, FO for first radial overtone and S for strange mode oscillations.
    [Show full text]
  • 219Th Meeting of the American Astronomical Society
    219TH MEETING OF THE AMERICAN ASTRONOMICAL SOCIETY 8-12 JANUARY 2012 AUSTIN, TX All scientific sessions will be held at the: Austin Convention Center COUNCIL .......................... 2 500 East Cesar Chavez Street Austin, TX 78701-4121 EXHIBITORS ..................... 4 AAS Paper Sorters ATTENDEE SERVICES .......................... 9 Tom Armstrong, Blaise Canzian, Thayne Curry, Shantanu Desai, Aaron Evans, Nimish P. Hathi, SCHEDULE .....................15 Jason Jackiewicz, Sebastien Lepine, Kevin Marvel, Karen Masters, J. Allyn Smith, Joseph Tenn, SATURDAY .....................25 Stephen C. Unwin, Gerritt Vershuur, Joseph C. Weingartner, Lee Anne Willson SUNDAY..........................28 Session Numbering Key MONDAY ........................36 90s Sunday TUESDAY ........................91 100s Monday WEDNESDAY .............. 146 200s Tuesday 300s Wednesday THURSDAY .................. 199 400s Thursday AUTHOR INDEX ........ 251 Sessions are numbered in the Program Book by day and time. Please note, posters are only up for the day listed. Changes after 7 December 2011 are only included in the online program materials. 1 AAS Officers & Councilors President (6/2010-6/2013) Debra Elmegreen Vassar College Vice President (6/2009-6/2012) Lee Anne Willson Iowa State Univ. Vice President (6/2010-6/2013) Nicholas B. Suntzeff Texas A&M Univ. Vice President (6/2011-6/2014) Edward B. Churchwell Univ. of Wisconsin Secretary (6/2010-6/2013) G. Fritz Benedict Univ. of Texas, Austin Treasurer (6/2008-6/2014) Hervey (Peter) Stockman STScI Education Officer (6/2006-6/2012) Timothy F. Slater Univ. of Wyoming Publications Board Chair (6/2011-6/2015) Anne P. Cowley Arizona State Univ. Executive Officer (6/2006-Present) Kevin Marvel AAS Councilors Richard G. French Wellesley College (6/2009-6/2012) James D.
    [Show full text]
  • Lyman Continuum Leaking Galaxies. Search Strategies and Local Candidates?
    A&A 554, A38 (2013) Astronomy DOI: 10.1051/0004-6361/201118433 & c ESO 2013 Astrophysics Lyman continuum leaking galaxies. Search strategies and local candidates? N. Bergvall1, E. Leitet1, E. Zackrisson2, and T. Marquart1 1 Department of Physics and Astronomy, Uppsala University, Box 515, 751 20 Uppsala, Sweden e-mail: [nils.bergvall;elisabet.leitet;thomas.marquart]@physics.uu.se 2 Department of Astronomy, Stockholm University, Oscar Klein Center, AlbaNova, 106 91 Stockholm, Sweden e-mail: [email protected] Received 10 November 2011 / Accepted 26 February 2013 ABSTRACT Context. Star-forming dwarf galaxies may have played an important role in the reionization of the Universe, provided that some fraction of their ionizing radiation were able to escape into the intergalactic medium. Local galaxies exhibiting such Lyman-continuum (LyC) leakage could potentially shed light on the escape mechanisms involved, but only two low-redshift cases of LyC leakage have been identified so far. Here, we argue that this meager harvest may be caused by unsuitable selection criteria. Candidates for LyC leakage are normally selected by indicators of starburst activity, one of which is a high equivalent width in Hα. Such a criterion will guarantee a high production of LyC photons but will also bias the selection in favour of a high column density in the neutral gas, effectively ruling out LyC escape. Aims. In this work we want to investigate whether the lack of local LyC emitters can be caused in part by biased selection criteria, and we present a novel method of selecting targets with high escape fractions. By applying these criteria, we assemble a sample of observation targets to study their basic properties.
    [Show full text]