DOCSLIB.ORG

The Balmer Decrement in the Emission Spectra of Astronomical Objects

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
The Balmer Decrement in the Emission Spectra of Astronomical Objects The Balmer decrement in the emission spectra of astronomical objects Item Type text; Thesis-Reproduction (electronic) Authors Bloom, Gary Stuart, 1940- Publisher The University of Arizona. Rights Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author. Download date 03/10/2021 20:45:29 Link to Item http://hdl.handle.net/10150/318347 THE BALMER DECREMENT IN THE EMISSION SPECTRA OF ASTRONOMICAL OBJECTS, by Gary Stuart Bloom A Thesis Submitted to the Faculty of the DEPARTMENT OF PHYSICS In Partial Fulfillment of the Requirements For the Degree of MASTER OF SCIENCE In the Graduate College THE UNIVERSITY OF ARIZONA 1 9 6 9 STATEMENT BY AUTHOR This thesis has been submitted in partial ful­ fillment of requirements for an advanced degree at The University of Arizona and is deposited in the University Library to be made available to borrowers under rules of the Library. Brief quotations from this thesis are allowable without special permission, provided that accurate acknowl­ edgment of source is made. Requests for permission for extended quotation from or reproduction of this manuscript in whole or in part may be granted by the head of the major department or the Dean of the Graduate College when in his judgment the proposed use of the material is in the interests of scholarship. In all other instances, however, permission must be obtained from the author. SIGNED:__ APPROVAL BY THESIS DIRECTOR This thesis has been approved on the date shown below: PREFACE Due to the nature of the problem undertaken, namely, comparison of the Balmer decrements In astronomical emission spectra, the details of this thesis were becoming dated even prior to completion of the work. We have tried to gather together results of all studies pertinent to this report which have been published in English, German, or French prior to the fall of 1 9 6 5. Some studies published in Russian are included, but we do not claim to have exhausted this literature. Work published in other languages have not been included. Due to the necessity of completing this study, we have ignored the promulgation of results currently being published. Inclusion of such data should give more accurate results for some of the objects we examined, and would probably improve the averages which we have computed. At least one such study, Vorontsov-Vel' yaminov et a l , (1965), gives corrections of their former data which we have used in this study. Their recalibration gave them intensity increases upward of 20$. In our search into the literature of objects exhibit­ ing Balmer emission spectra, we inadvertantly overlooked the Wolf-Rayet class of stars which are known to exhibit these ill lines (see5 for example., Ambartsumyan 1958, pp. 490-496). A cursory search to remedy our lack of information about the decrement has not been successful, and we have found only an emission decrement from the nebulosity associated with a WC star. (Andrillat and Andrillat 1953)° TABLE OF CONTENTS PAGE LIST OF TABLES . viii LIST OF ILLUSTRATIONS xvil ABSTRACT » . » o 0 0 0 Q . XX INTRODUCTION . , 1 GENERAL REMARKS 4 The Definition ........... 4 Problems of Measurement . , 4 Corrections to the Raw Data . , 6 The Uses of the Balmer Decrement 10 Types of Intensity Data Found in the Literature . , 11 Normalizing the Data 14 GASEOUS NEBULAE. 15 Historical Remarks 15 The Published Data 17 NGC 1535 .... 20 NGC 1976 . , 22 NGC 2022 .... 22 ■ NGC 2392 .... 27 NGC 2440 . ... ... 28 NGC 6543 . ... 29 NGC 6572 .... 29 NGC 6741 .... 29 NGC 6826 .... 31 NGC 7009 .... 32 NGC 702? .... NGC 7662 .... 1 IC 351....... 36 IC 418 ..... 10 2l49 o 9 a 00 . o © V e e » 38 IC 4997 o6 . a . o 0 *0. » Implications of the :Published Data. 1: Average Decrements for Each Nebula 40 Steep, Average, and Shallow Decrements 45 Summary and Conclusions . 55 v vi TABLE OP CONTENTS--Continued . PAGE STARS f 58 Observational Difficulties and Star Types . 58 Be Stars 61 Variable Stars 62 Pulsating Variablea--.3 Canis Major is Type . , 66 Eruptive Variables-=T Tauri Stars ...... 67 Eruptive Variables--Novae ......... i 67 Description ............... 67 Published Data ............. 71 Eruptive Variables “--Nova-Like Variables . 78 Recurrent Novae ............. 81 R Coronae Borealis Stars ........ 81 P Cygni Stars ...... ....... ... 84 Symbiotic Stars ............. 92 Summary and Evaluation of the Published Data . 106 Additional Data ................. 110 SOLAR PHENOMENA . \ . 112 Solar Regions and the Sites of Hydrogen Emission Spectra ... 112 The Flash Spectrum of the Chromosphere ...... 115 History and Observational Techniques .... 115 Specification of Balmer Decrements in the Chromosphere ............ 122 The Published Data . 128 Normal Regions ............... 128 Excited Regions ............... 133 Discussion of the Data and Some Comparisons ............... 134 The Average Chromospheric • Balmer Decrement ................ 163 Local Phenomena . , . 186 Definitions ..... 186 Presentation of Data and Comments . 189 ' Quiescent Prominences ....... ....... 191 Active Prominences ............. 193 Published Data ............. 193 Analysis of the Data . ........... 196 Limb Flares ................. 200 Dxsk Flares . ■. @ . 201 Summary . ... ® 207 vii TABLE OF COEFEIfPS - -Continued PAGE COMCLTOIMG REMABl^ ................... 210 Galaxies ..................... 210 Quasi-Stellar Objects ............... 212 tE> y . 212 A Suggestion ................... 213 APPMBXX A— Balmer Line Intensity Data as Originally Published for Nebulae ............... 215 APPENDIX B— Balmer Line Intensity Data as Originally Published for Stars ....... ............ 219 APPENDIX C— Balmer Line Intensity Data as Originally Published for the Solar Chromosphere ....... 233 APPENDIX D— Intermediate Steps in the Computer Calculations ................... 251 APPENDIX E— Balmer Line Intensity Data as Originally Published for Solar Flares and Prominences .... 259 BIBLIOGRAPHY ...................... 266 LIST OF TABLES TABLE PAGE 1. Nebulae Examined in Detail with References Thereto ..................... 19 2. Balmer Decrements Published for NGG 1535 ..... 21 3. Averages of Mendez1 11 Point Observations of NGG 1976 23 4. Balmer Decrements Published for NGG 1976 24 5. Balmer Decrements Published for HOC 2022 ..... 27 6. Balmer Decrements Published for NGG 2392 ..... 27 7. Balmer Decrements Published for NGG 2440 ..... 28 8. Balmer Decrements Published for NGG 6543 ..... 29 9. Balmer Decrements Published for NGG 6572*....... 30 10. Balmer Decrements Published for NGG 6741 ..... 31 11. Balmer Decrements Published for NGG 6826 ..... 32 12. Balmer Decrements Published for NGG 7009 ....... 33 i 13. Balmer Decrements Published for NGG 7027 ..... 34 14. Balmer Decrements Published for NGG 7662 ..... 35. 15. Balmer Decrements Published for IC 351 ...... 36 16. Balmer Decrements Published for 10 4l8 ...... 37 17. Balmer Decrements Published for IG 2149 ..... 38 18. Balmer Decrements Published for 10 4997 ..... 39 19. Weights Assigned to Publications in Order to Compute the Average Balmer Decrement for Each Nebula . ......... 44 viii ix LIST OF TABLES— Continued ' TABLE PAGE 20. Weighted Averages of the Balraer Intensities for Selected Nebulae {First Group) ...... 46 21. Weighted Averages of the Balraer Intensities for Selected Nebulae (Second Group) ......... 47 22. Average Balraer Line Decrements for Gaseous Nebulae ......... 50 23. The "Average11 Intensity Range in Gaseous Nebulae for Each Balmer Line and the Number of Nebulae Whose Intensities Fell Within and to Either Side of this Range ...» 52 24. A Comparison of Nebula Balmer-Line Intensities with the Group of "Average".Intensities .... 53 2 5 . Be Stars Examined and References Thereto ..... 61 26. Balmer Line Intensities and Decrements for y Cassiopeiae from 9/37 to 12/38 ........ 63 27. Balmer Decrements of 10 Be Stars ......... 64 28. Balmer Decrement of S Cephei ............ 67 2 9. Balmer Decrements of Two T Taurl Stars ..... .. 6 9. 30. Studies Made of Novae, Published Since. 1950 . , . 72 31. Balmer Decrements of Nova Serp 1909 and Nova ' Scu 1949 ................. 0 . .75 3 2 . Balmer Decrements of Nova Aqu 1918 » . .... 76 33. Balmer Decrements of Nova DK Lae 1950 ...... 77 34. Balmer Decrements of Nova Herculis i960 ..... 78 35. Balmer Decrements of Nova Herculis 1934 ..... 79 3 6. Balmer Decrements of Nova T Coronae Borealis . 82 37. Balmer Decrements of Nova RS Ophluchi 1958 .... 82 3 8 . Balmer Decrements of xx Ophiuchi (HD 116114) . 85 •X LIST OF TABLES--Continued TABLE PAGE 39. Balmer Decrements of P Cyg and HD 51585 ........... 89 40. Balmer Decrements of x Ophiuchl .......... 90 41. Studies Made of Symbiotic Stars Published Since 1950 ......... 93 42. Balmer Decrements of Z Andromedae ......... 97 4 3 . Balmer Decrements of BF Cygni ........... 99 44. Balmer Decrements of WC 6 0 3 ................ 100 4 5 . Balmer Decrements of 01 Cygni ................ 100 46. Balmer Decrements of x C y g n i ......... 101 4 7 . Balmer Decrements of AXPe r s e i .............. 101 48. Balmer Decrements of AG Pegasi .......... 102 4 9 . Balmer Decrements of BDtll°4673 ........... 103 50. Balmer Emission Line Intensity Value Spreads Published for Eight Star. Categories ...... 107 51. Studies of Stars Published Prior to 1950 , . Ill 52. Balmer Line Studies Resulting from Solar Eclipse Observations . ................
Load more

Recommended publications
  • 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............................................................................................................
    [Show full text]
  • A Hot Subdwarf-White Dwarf Super-Chandrasekhar Candidate
    A hot subdwarf–white dwarf super-Chandrasekhar candidate supernova Ia progenitor Ingrid Pelisoli1,2*, P. Neunteufel3, S. Geier1, T. Kupfer4,5, U. Heber6, A. Irrgang6, D. Schneider6, A. Bastian1, J. van Roestel7, V. Schaffenroth1, and B. N. Barlow8 1Institut fur¨ Physik und Astronomie, Universitat¨ Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, D-14476 Potsdam-Golm, Germany 2Department of Physics, University of Warwick, Coventry, CV4 7AL, UK 3Max Planck Institut fur¨ Astrophysik, Karl-Schwarzschild-Straße 1, 85748 Garching bei Munchen¨ 4Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106, USA 5Texas Tech University, Department of Physics & Astronomy, Box 41051, 79409, Lubbock, TX, USA 6Dr. Karl Remeis-Observatory & ECAP, Astronomical Institute, Friedrich-Alexander University Erlangen-Nuremberg (FAU), Sternwartstr. 7, 96049 Bamberg, Germany 7Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA 8Department of Physics and Astronomy, High Point University, High Point, NC 27268, USA *[email protected] ABSTRACT Supernova Ia are bright explosive events that can be used to estimate cosmological distances, allowing us to study the expansion of the Universe. They are understood to result from a thermonuclear detonation in a white dwarf that formed from the exhausted core of a star more massive than the Sun. However, the possible progenitor channels leading to an explosion are a long-standing debate, limiting the precision and accuracy of supernova Ia as distance indicators. Here we present HD 265435, a binary system with an orbital period of less than a hundred minutes, consisting of a white dwarf and a hot subdwarf — a stripped core-helium burning star.
    [Show full text]
  • NL 2011-2 Backup
    Newsletter 2011-3 August 2011 www.variablestarssouth.org Hawkes Bay Astronomical Society members at the site of their partially completed Pukerangi roll-off observatory. Photo by Graham Palmer and provided by Col Bembrick. Col’s recollections of the 2011 RASNZ conference hosted by the Hawkes Bay Astronomical Society appear on page 11. Contents From the director - Tom Richards ........................................................................................................................... 2 Variables from Linden – Towards the Hub - Alan Plummer ................................................................. 4 BL Telescopii - Observations of the 2011 eclipse - Peter F Williams ............................................ 7 A DSLR bright Cepheid project - Can you help? - Stan Walker ........................................................ 9 RASNZ Conference Napier, 2011 - Col Bembrick ................................................................................... 11 Recurrent Novae - Stan Walker .............................................................................................................................. 13 Southern Binaries DSLR Project - Mark Blackford .................................................................................. 17 Equatorial Eclipsing Binaries Project - Tom Richards ............................................................................ 19 SPADES Report - Tom Richards ...........................................................................................................................
    [Show full text]
  • Naming the Extrasolar Planets
    Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named.
    [Show full text]
  • Správa O Činnosti Organizácie SAV Za Rok 2017
    Astronomický ústav SAV Správa o činnosti organizácie SAV za rok 2017 Tatranská Lomnica január 2018 Obsah osnovy Správy o činnosti organizácie SAV za rok 2017 1. Základné údaje o organizácii 2. Vedecká činnosť 3. Doktorandské štúdium, iná pedagogická činnosť a budovanie ľudských zdrojov pre vedu a techniku 4. Medzinárodná vedecká spolupráca 5. Vedná politika 6. Spolupráca s VŠ a inými subjektmi v oblasti vedy a techniky 7. Spolupráca s aplikačnou a hospodárskou sférou 8. Aktivity pre Národnú radu SR, vládu SR, ústredné orgány štátnej správy SR a iné organizácie 9. Vedecko-organizačné a popularizačné aktivity 10. Činnosť knižnično-informačného pracoviska 11. Aktivity v orgánoch SAV 12. Hospodárenie organizácie 13. Nadácie a fondy pri organizácii SAV 14. Iné významné činnosti organizácie SAV 15. Vyznamenania, ocenenia a ceny udelené organizácii a pracovníkom organizácie SAV 16. Poskytovanie informácií v súlade so zákonom o slobodnom prístupe k informáciám 17. Problémy a podnety pre činnosť SAV PRÍLOHY A Zoznam zamestnancov a doktorandov organizácie k 31.12.2017 B Projekty riešené v organizácii C Publikačná činnosť organizácie D Údaje o pedagogickej činnosti organizácie E Medzinárodná mobilita organizácie F Vedecko-popularizačná činnosť pracovníkov organizácie SAV Správa o činnosti organizácie SAV 1. Základné údaje o organizácii 1.1. Kontaktné údaje Názov: Astronomický ústav SAV Riaditeľ: Mgr. Martin Vaňko, PhD. Zástupca riaditeľa: Mgr. Peter Gömöry, PhD. Vedecký tajomník: Mgr. Marián Jakubík, PhD. Predseda vedeckej rady: RNDr. Luboš Neslušan, CSc. Člen snemu SAV: Mgr. Marián Jakubík, PhD. Adresa: Astronomický ústav SAV, 059 60 Tatranská Lomnica http://www.ta3.sk Tel.: 052/7879111 Fax: 052/4467656 E-mail: [email protected] Názvy a adresy detašovaných pracovísk: Astronomický ústav - Oddelenie medziplanetárnej hmoty Dúbravská cesta 9, 845 04 Bratislava Vedúci detašovaných pracovísk: Astronomický ústav - Oddelenie medziplanetárnej hmoty prof.
    [Show full text]
  • National Radio Astronomy Observatory Quarterly
    Qs V'O6?-AzIJJ NATIONAL RADIO ASTRONOMY OBSERVATORY QUARTERLY REPORT January 1 - March 31, 1990 APr TABLE OF CONTENTS A. TELESCOPE USAGE .1.. .. ... ............................... 1 B. 140-FOOT TELESCOPE1 ... ........ ............................. 1 C. 12-METER TELESCOPE6 ......... ............................. 6 D. VERY LARGE ARRAY9 .. ........ .............................. 9 E. SCIENTIFIC HIGHLIGHTS .. ........ ............................ 20 F. PUBLICATIONS ... ........ ................................ 21 G. CENTRAL DEVELOPMENT LABORATORY . ....... ....................... 21 H. GREEN BANK ELECTRONICS . ........ ........................... 23 I. 12-METER ELECTRONICS . ........ .............................. 25 J. VLA ELECTRONICS .. ........ ............................... 25 K. AIPS .. ........ .................................... 28 L. VLA COMPUTER .. ....... ................................ 28 M. VERY LONG BASELINE ARRAY . ........ .......................... 29 N. PERSONNEL ... .......... .................................. 32 APPENDIX A: LIST OF NRAO PREPRINTS A. TELESCOPE USAGE The NRAO telescopes have been scheduled for research and maintenance in the following manner during the first quarter of 1990. 140-ft 12-meter VIA Scheduled observing (hours) 1935.00 1772.25 1624.6 Scheduled maintenance and equipment changes 193.5 116.25 264.6 Scheduled tests and calibrations 127.25 261.50 261.6 Time lost 103.75 366.25 78.0 Actual observing 1831.25 1496.00 1546.7 B. 140-FOOT TELESCOPE The following line programs were conducted during the quarter. No. Observer(s) Program B-492 Bell, M. (Herzberg) Spectral survey of IRC+10216 over the Feldman, P (Herzberg) range 22.0-24.5 GHz. Matthews, H. (Herzberg) B-524 Bell, M. (Herzberg) . Studies at 17.5-24.5 GHz of heavy Avery, L. (Herzberg) molecule chemistry in shocked and Feldman, P. (Herzberg) unshocked gas in Orion. Matthews, H. (Herzberg) B-492 Bell, M. (Herzberg) Spectral survey of IRC+10216 over the Feldman, P. (Herzberg) range 22.0-24.5 GHz. Matthews, H. (Herzberg) B-525 Bell, M.
    [Show full text]
  • Dramatic Change in the Boundary Layer in the Symbiotic Recurrent
    Astronomy & Astrophysics manuscript no. tcrb˙submitted˙to˙arxiv © ESO 2018 July 4, 2018 Dramatic change in the boundary layer in the symbiotic recurrent nova T Coronae Borealis. G. J. M. Luna,1,2,3, K. Mukai,4,5 J. L. Sokoloski,6 T. Nelson,7 P. Kuin,8 A. Segreto,9 G. Cusumano,9 M. Jaque Arancibia,10,11 and N. E. Nu˜nez,11 1 CONICET-Universidad de Buenos Aires, Instituto de Astronom´ıa y F´ısica del Espacio, (IAFE), Av. Inte. G¨uiraldes 2620, C1428ZAA, Buenos Aires, Argentina e-mail: [email protected] 2 Universidad de Buenos Aires, Facultad de Ciencias Exactas y Naturales, Buenos Aires, Argentina 3 Universidad Nacional Arturo Jauretche, Av. Calchaqu´ı6200, F. Varela, Buenos Aires, Argentina 4 CRESST and X-ray Astrophysics Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA 5 Department of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, MD 21250, USA 6 Columbia Astrophysics Lab 550 W120th St., 1027 Pupin Hall, MC 5247 Columbia University, New York, New York 10027, USA 7 Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260 8 University College London, Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, RH5 6NT, U.K. 9 INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica, Via U. La Malfa 153, I-90146 Palermo, Italy 10 Departamento de F´ısica y Astronom´ıa, Universidad de La Serena, Av. Cisternas 1200, La Serena, Chile. 11 Instituto de Ciencias Astron´omicas, de la Tierra y del Espacio (ICATE-CONICET), Av. Espa˜na Sur 1512, J5402DSP, San Juan, Argentina ABSTRACT A sudden increase in the rate at which material reaches the most internal part of an accretion disk, i.e.
    [Show full text]
  • The Messenger
    THE MESSENGER No. 33 - September 1983 Whoever witnessed the period of intellectual suppression in Otto Heckmann the late thirties in Germany, can imagine the hazardous 1901-1983 enterprise of such a publication at that time. In 1941 Otto Heckmann received his appointment as the Director of the Hamburg Observatory. First engaged in the Otto Heckmann, past Di­ accomplishment of the great astronomical catalogues AGK 2 rector General of the and AGK 3, he soon went into the foot prints of Walter Baade European Southern Ob­ who once had built a large Schmidt telescope. The inaugura­ servatory (1962-1969), tion of the "Hamburg Big Schmidt" was the initiative step President of the Interna­ towards a greater task. tional Astronomical Union (1967-1970), and the As­ Otto Heckmann always kept close contact with Walter tronomische Gesellschaft Baade. The latter, giving lectures at the Leiden Observatory, in (1952-1957), Professor 1953 emphasized to the Eurapean astronomers the great of Astronomy and Director importance of a common European observatory "established of the Hamburg Observa­ in the southern hemisphere, equipped with powerful instru­ tory (1941-1962), died on ments, with the aim of furthering and organizing collaboration in May 13, 1983. astranomy". The European South­ In a fundamental conference with W. Baade in the spring of ern Observatory has par­ that year, a number of outstanding European astronomers, ticular reason to be grate­ Prof. Otto Heckmann among whom A. Danjon from France, P. Bourgeois from ful to Otto Heckmann Belgium, J. H. Oort from the Netherlands, Sir Harald Spencer­ Photograph: Dr. Patar Lamarsdorf whose creative impulse Jones from Great Britain, B.
    [Show full text]
  • RESEARCH PROGRAMS 140-Foot Telescope
    VS/G LI NATIONAL RADIO ASTRONOMY OBSERVATORY Charlottesville, Virginia r Quarterly Report October 1, 1981 - December 31, 1981 RESEARCH PROGRAMS 140-foot Telescope Hours Scheduled observing 1955.75 Scheduled maintenance and equipment changes 179.25 Scheduled tests and calibration 1.00 Time lost due to: equipment failure 34.75 power 9.50 weather 133.25 interference 0.00 The following line programs were conducted during this quarter. No. Observer (s) Program T-156 I. Kazes (Meudon, France) Observations to study giant molecular B. Turner clouds at the main 18 cm OH line frequencies. T-145 B. Turner Search within the 13-16 GHz range for new molecular species. S-233 L. Buxton (Illinois) Observations at 20.9 and 24.4 GHz to E. Campbell (Illinois) search for the HCN dimer (HCN) 2 . W. Flygare (Illinois) P. Jewell (Illinois) M. Schenewerk (Illinois) L. Snyder (Illinois) B-381 R. Brown Observations at 5-cm to confirm and extend the detection of recombination line emission from 3C 245 and a search for this type of emission from other QSOs. S-246 M. Bell (NRC, Canada) Search at 5 cm for recombination lines E. Seaquist (Toronto) in compact extragalactic sources. No. Observer(s) Program M-176 L. Avery (NRC, Canada) Observations at 18.2 GHz of the J=241 N. Broten (NRC, Canada) transition of HC3N, generally toward J. MacLeod (NRC, Canada) dark clouds. H. Matthews (NRC, Canada T. Oka (Chicago) The following continuum programs were conducted during this quarter. No. Observer (s) Program C-194 M. Condon (unaffiliated) Survey at 14.5 cm of extragalactic J.
    [Show full text]
  • 16Th HEAD Meeting Session Table of Contents
    16th HEAD Meeting Sun Valley, Idaho – August, 2017 Meeting Abstracts Session Table of Contents 99 – Public Talk - Revealing the Hidden, High Energy Sun, 204 – Mid-Career Prize Talk - X-ray Winds from Black Rachel Osten Holes, Jon Miller 100 – Solar/Stellar Compact I 205 – ISM & Galaxies 101 – AGN in Dwarf Galaxies 206 – First Results from NICER: X-ray Astrophysics from 102 – High-Energy and Multiwavelength Polarimetry: the International Space Station Current Status and New Frontiers 300 – Black Holes Across the Mass Spectrum 103 – Missions & Instruments Poster Session 301 – The Future of Spectral-Timing of Compact Objects 104 – First Results from NICER: X-ray Astrophysics from 302 – Synergies with the Millihertz Gravitational Wave the International Space Station Poster Session Universe 105 – Galaxy Clusters and Cosmology Poster Session 303 – Dissertation Prize Talk - Stellar Death by Black 106 – AGN Poster Session Hole: How Tidal Disruption Events Unveil the High 107 – ISM & Galaxies Poster Session Energy Universe, Eric Coughlin 108 – Stellar Compact Poster Session 304 – Missions & Instruments 109 – Black Holes, Neutron Stars and ULX Sources Poster 305 – SNR/GRB/Gravitational Waves Session 306 – Cosmic Ray Feedback: From Supernova Remnants 110 – Supernovae and Particle Acceleration Poster Session to Galaxy Clusters 111 – Electromagnetic & Gravitational Transients Poster 307 – Diagnosing Astrophysics of Collisional Plasmas - A Session Joint HEAD/LAD Session 112 – Physics of Hot Plasmas Poster Session 400 – Solar/Stellar Compact II 113
    [Show full text]
  • 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.
    [Show full text]
  • Stars and Their Spectra: an Introduction to the Spectral Sequence Second Edition James B
    Cambridge University Press 978-0-521-89954-3 - Stars and Their Spectra: An Introduction to the Spectral Sequence Second Edition James B. Kaler Index More information Star index Stars are arranged by the Latin genitive of their constellation of residence, with other star names interspersed alphabetically. Within a constellation, Bayer Greek letters are given first, followed by Roman letters, Flamsteed numbers, variable stars arranged in traditional order (see Section 1.11), and then other names that take on genitive form. Stellar spectra are indicated by an asterisk. The best-known proper names have priority over their Greek-letter names. Spectra of the Sun and of nebulae are included as well. Abell 21 nucleus, see a Aurigae, see Capella Abell 78 nucleus, 327* ε Aurigae, 178, 186 Achernar, 9, 243, 264, 274 z Aurigae, 177, 186 Acrux, see Alpha Crucis Z Aurigae, 186, 269* Adhara, see Epsilon Canis Majoris AB Aurigae, 255 Albireo, 26 Alcor, 26, 177, 241, 243, 272* Barnard’s Star, 129–130, 131 Aldebaran, 9, 27, 80*, 163, 165 Betelgeuse, 2, 9, 16, 18, 20, 73, 74*, 79, Algol, 20, 26, 176–177, 271*, 333, 366 80*, 88, 104–105, 106*, 110*, 113, Altair, 9, 236, 241, 250 115, 118, 122, 187, 216, 264 a Andromedae, 273, 273* image of, 114 b Andromedae, 164 BDþ284211, 285* g Andromedae, 26 Bl 253* u Andromedae A, 218* a Boo¨tis, see Arcturus u Andromedae B, 109* g Boo¨tis, 243 Z Andromedae, 337 Z Boo¨tis, 185 Antares, 10, 73, 104–105, 113, 115, 118, l Boo¨tis, 254, 280, 314 122, 174* s Boo¨tis, 218* 53 Aquarii A, 195 53 Aquarii B, 195 T Camelopardalis,
    [Show full text]