Bibliography from ADS File: Stencel.Bib June 27, 2021 1
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2017 Býk Otec Fir 2016 Býk Otec Fir 2015 Býk
2017 BÝK OTEC FIR 2016 BÝK OTEC FIR 2015 BÝK OTEC FIR 2014 BÝK OTEC FIR 1 2949 LEGACY FRAZZLED 507 2 2944 NASHVILLE DYNASTY 551 BÝCI REGISTROVANÍ V ČR 3 2933 RIVETING FRAZZLED 614 Aktualizace k: 5.1.2019 1 2920 CHARL CHARLEY 551 BÝCI *2017 a starší. TPI 2400 a více 4 2919 PINNACLE 7 MTS 5 2913 AltaLAWSON AltaROBSON 11 Natural, Zooservis 6 2908 DISCJOCKEY FORTUNE 200 Ostatní 7 2908 FULLMARKS FORTUNE 200 8 2908 EISAKU SAMURI 507 9 2907 ACURA ACHIEVER 29 10 2904 BUNDLE ACHIEVER 29 11 2903 DEDICATE SUPERHERO 551 12 2902 PURSUIT IMAX 200 13 2893 EMERALD FORTUNE 200 14 2893 AltaRNR AltaROBSON 11 15 2889 ROME FRAZZLED 614 16 2883 RENEGADE JALTAOAK 550 17 2883 SOLUTION FRAZZLED 614 18 2883 BATMAN IMAX 200 19 2882 ROYAL DUKE 29 20 2882 PONCHO NOBLE 551 21 2879 CHALLENGER SUPERHERO 200 22 2878 PERK SPECTRE 29 23 2878 CRIMSON SPECTRE 29 24 2876 MAESTRO IMAX 200 25 2874 GAMECHANGER MODESTY 1 26 2873 PYRAMID GUARANTEE 200 27 2873 MENACE DELTA-WORTH 551 28 2872 APPLEBEES ACHIEVER 29 29 2872 CASCADE KING ROYAL 507 30 2870 AltaROBERT AltaROBSON 11 31 2869 ARISTOCRAT FRAZZLED 515 32 2869 RAPID RUBI-HAZE 551 33 2867 AltaROADY AltaROBSON 11 34 2866 BIG AL FRAZZLED 507 35 2866 PETRO PROPHECY 29 36 2866 VALUE DUKE 29 37 2865 NACASH SUPERHERO 180 38 2865 EMBELLISH FORTUNE 200 39 2864 BRASS FRAZZLED 507 40 2861 MESCALERO PINNACLE 250 41 2860 KORBEL ACHIEVER 1 42 2860 TIMBERLAKE IMAX 200 43 2860 AltaHOTJOB HOTLINE 11 44 2859 ENFORCE FRAZZLED 100 45 2858 HEMINGWAY FORTUNE 200 46 2857 EXODUS REASON 250 47 2857 ALERT FORTUNE 200 48 2856 DIVERSITY MEDLEY 29 49 2856 -
Accretion Flows in Nonmagnetic White Dwarf Binaries As Observed in X-Rays
Accretion Flows in Nonmagnetic White Dwarf Binaries as Observed in X-rays Şölen Balmana,< aKadir Has University, Faculty of Engineering and Natural Sciences, Cibali 34083, Istanbul, Turkey ARTICLEINFO ABSTRACT Keywords: Cataclysmic Variables (CVs) are compact binaries with white dwarf (WD) primaries. CVs and other cataclysmic variables - accretion, accre- accreting WD binaries (AWBs) are useful laboratories for studying accretion flows, gas dynamics, tion disks - thermal emission - non-thermal outflows, transient outbursts, and explosive nuclear burning under different astrophysical plasma con- emission - white dwarfs - X-rays: bina- ditions. They have been studied over decades and are important for population studies of galactic ries X-ray sources. Recent space- and ground-based high resolution spectral and timing studies, along with recent surveys indicate that we still have observational and theoretical complexities yet to an- swer. I review accretion in nonmagnetic AWBs in the light of X-ray observations. I present X-ray diagnostics of accretion in dwarf novae and the disk outbursts, the nova-like systems, and the state of the research on the disk winds and outflows in the nonmagnetic CVs together with comparisons and relations to classical and recurrent nova systems, AM CVns and Symbiotic systems. I discuss how the advective hot accretion flows (ADAF-like) in the inner regions of accretion disks (merged with boundary layer zones) in nonmagnetic CVs explain most of the discrepancies and complexities that have been encountered in the X-ray observations. I stress how flickering variability studies from optical to X-rays can be probes to determine accretion history and disk structure together with how the temporal and spectral variability of CVs are related to that of LMXBs and AGNs. -
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. -
Red Giant Mass-Loss: Studying Evolved Stellar Winds with FUSE and HST/STIS
Red Giant Mass-Loss: Studying Evolved Stellar Winds with FUSE and HST/STIS A dissertation submitted to the University of Dublin for the degree of Doctor of Philosophy Cian Crowley Supervisor: Dr. Brian R. Espey Trinity College Dublin, July 2006 School of Physics University of Dublin Trinity College Dublin ii For Mam and Dad Declaration I hereby declare that this thesis has not been submitted as an exercise for a degree at this or any other University and that it is entirely my own work. I agree that the Library may lend or copy this thesis upon request. Signed, Cian Crowley July 25, 2006. Publications Crowley, C., Espey, B. R.,. & McCandliss, S. R., 2006, In prep., ‘FUSE and HST/STIS Observations of the Eclipsing Symbiotic Binary EG Andromedae’ Acknowledgments I wish to acknowledge and thank Brian Espey, Stephan McCandliss and Peter Hauschildt for their contributions to this work. Most especially I would like to express my gratitude to my supervisor Brian Espey for his enthusiastic supervision, patience and encourage- ment. His help, support and advice is very much appreciated. In addition, the helpful and insightful comments and advice from numerous people, inlcuding, Graham Harper, Philip Bennett, Alex Brown, Gary Ferland, Tom Ake, B-G Anderson and Dugan With- erick, were invaluable and again, very much appreciated. Also, a special word of thanks for their viva comments and feedback for Alex Brown and Peter Gallagher. This work was supported by Enterprise Ireland Basic Research grant SC/2002/370 from EU funded NDP. The FUSE data were obtained under the Guest Investigator Pro- gram and supported by NASA grants NAG5-8994 and NAG5-10403 to the Johns Hopkins University (JHU). -
Solar Writer Report for Abraham Lincoln
FIXED STARS A Solar Writer Report for Abraham Lincoln Written by Diana K Rosenberg Compliments of:- Stephanie Johnson Seeing With Stars Astrology PO Box 159 Stepney SA 5069 Australia Tel/Fax: +61 (08) 8331 3057 Email: [email protected] Web: www.esotech.com.au Page 2 Abraham Lincoln Natal Chart 12 Feb 1809 12:40:56 PM UT +0:00 near Hodgenville 37°N35' 085°W45' Tropical Placidus 22' 13° 08°ˆ ‡ 17' ¾ 06' À ¿É ‰ 03° ¼ 09° 00° 06° 09°06° ˆ ˆ ‡ † ‡ 25° 16' 41'08' 40' † 01' 09' Œ 29' ‰ 9 10 23° ¶ 8 27°‰ 11 Ï 27° 01' ‘ ‰02' á 7 12 ‘ áá 23° á 23° ¸ 23°Š27' á Š à „ 28' 28' 6 18' 1 10°‹ º ‹37' 13° 05' ‹ 5 Á 22° ½ 27' 2 4 01' Ü 3 07° Œ ƒ » 09' 23° 09° Ý Ü 06° 16' 06' Ê 00°ƒ 13° 22' Ý 17' 08°‚ Page 23 Astrological Summary Chart Point Positions: Abraham Lincoln Planet Sign Position House Comment The Moon Capricorn 27°Cp01' 12th The Sun Aquarius 23°Aq27' 12th read into 1st House Mercury Pisces 10°Pi18' 1st Venus Aries 7°Ar27' 1st read into 2nd House Mars Libra 25°Li29' 8th Jupiter Pisces 22°Pi05' 1st Saturn Sagittarius 3°Sg08' 9th read into 10th House Uranus Scorpio 9°Sc40' 8th Neptune Sagittarius 6°Sg41' 9th read into 10th House Pluto Pisces 13°Pi37' 1st The North Node Scorpio 6°Sc09' 8th The South Node Taurus 6°Ta09' 2nd The Ascendant Aquarius 23°Aq28' 1st The Midheaven Sagittarius 8°Sg22' 10th The Part of Fortune Capricorn 27°Cp02' 12th Chart Point Aspects Planet Aspect Planet Orb App/Sep The Moon Square Mars 1°32' Separating The Moon Conjunction The Part of Fortune 0°00' Applying The Sun Trine Mars 2°02' Applying The Sun Conjunction The Ascendant -
Appendix: Spectroscopy of Variable Stars
Appendix: Spectroscopy of Variable Stars As amateur astronomers gain ever-increasing access to professional tools, the science of spectroscopy of variable stars is now within reach of the experienced variable star observer. In this section we shall examine the basic tools used to perform spectroscopy and how to use the data collected in ways that augment our understanding of variable stars. Naturally, this section cannot cover every aspect of this vast subject, and we will concentrate just on the basics of this field so that the observer can come to grips with it. It will be noticed by experienced observers that variable stars often alter their spectral characteristics as they vary in light output. Cepheid variable stars can change from G types to F types during their periods of oscillation, and young variables can change from A to B types or vice versa. Spec troscopy enables observers to monitor these changes if their instrumentation is sensitive enough. However, this is not an easy field of study. It requires patience and dedication and access to resources that most amateurs do not possess. Nevertheless, it is an emerging field, and should the reader wish to get involved with this type of observation know that there are some excellent guides to variable star spectroscopy via the BAA and the AAVSO. Some of the workshops run by Robin Leadbeater of the BAA Variable Star section and others such as Christian Buil are a very good introduction to the field. © Springer Nature Switzerland AG 2018 M. Griffiths, Observer’s Guide to Variable Stars, The Patrick Moore 291 Practical Astronomy Series, https://doi.org/10.1007/978-3-030-00904-5 292 Appendix: Spectroscopy of Variable Stars Spectra, Spectroscopes and Image Acquisition What are spectra, and how are they observed? The spectra we see from stars is the result of the complete output in visible light of the star (in simple terms). -
GTO Keypad Manual, V5.001
ASTRO-PHYSICS GTO KEYPAD Version v5.xxx Please read the manual even if you are familiar with previous keypad versions Flash RAM Updates Keypad Java updates can be accomplished through the Internet. Check our web site www.astro-physics.com/software-updates/ November 11, 2020 ASTRO-PHYSICS KEYPAD MANUAL FOR MACH2GTO Version 5.xxx November 11, 2020 ABOUT THIS MANUAL 4 REQUIREMENTS 5 What Mount Control Box Do I Need? 5 Can I Upgrade My Present Keypad? 5 GTO KEYPAD 6 Layout and Buttons of the Keypad 6 Vacuum Fluorescent Display 6 N-S-E-W Directional Buttons 6 STOP Button 6 <PREV and NEXT> Buttons 7 Number Buttons 7 GOTO Button 7 ± Button 7 MENU / ESC Button 7 RECAL and NEXT> Buttons Pressed Simultaneously 7 ENT Button 7 Retractable Hanger 7 Keypad Protector 8 Keypad Care and Warranty 8 Warranty 8 Keypad Battery for 512K Memory Boards 8 Cleaning Red Keypad Display 8 Temperature Ratings 8 Environmental Recommendation 8 GETTING STARTED – DO THIS AT HOME, IF POSSIBLE 9 Set Up your Mount and Cable Connections 9 Gather Basic Information 9 Enter Your Location, Time and Date 9 Set Up Your Mount in the Field 10 Polar Alignment 10 Mach2GTO Daytime Alignment Routine 10 KEYPAD START UP SEQUENCE FOR NEW SETUPS OR SETUP IN NEW LOCATION 11 Assemble Your Mount 11 Startup Sequence 11 Location 11 Select Existing Location 11 Set Up New Location 11 Date and Time 12 Additional Information 12 KEYPAD START UP SEQUENCE FOR MOUNTS USED AT THE SAME LOCATION WITHOUT A COMPUTER 13 KEYPAD START UP SEQUENCE FOR COMPUTER CONTROLLED MOUNTS 14 1 OBJECTS MENU – HAVE SOME FUN! -
Curriculum Vitae Stephan Robert Mccandliss
August 2015 Curriculum Vitae Stephan Robert McCandliss Research Professor - JHU [email protected] Johns Hopkins University tel: 410-516-5272 Department of Physics & Astronomy fax: 410-516-8260 Baltimore, Maryland 21218 http://www.pha.jhu.edu/~stephan Familial History 1955/09/07 Born Salinas California 1989/01/01 Married Ann Marie McCandliss (nee Selander) 1989/11/10 Daughter Rachel Pearl McCandliss 1992/05/26 Son Ian Frederick McCandliss Education 1988 Ph.D. Astrophysics University of Colorado, Boulder 1981 B.S. Physics University of Washington, Seattle 1981 B.S. Astronomy University of Washington, Seattle Work History 2015 – present Director, Center for Astrophysical Sciences Johns Hopkins University 2010 – present Research Professor Johns Hopkins University 2002 – 2010 Principal Research Scientist Johns Hopkins University 1994 – 2002 Research Scientist Johns Hopkins University 1988 – 1994 Associate Research Scientist Johns Hopkins University 1981 – 1988 Ph.D. Candidate University of Colorado, Boulder 1977 – 1981 Reader and Lab Assistant University of Washington, Seattle Primary Research Interests The ionization history of the universe. Spectral signatures of dust, molecules and atoms in astrophysical environments. Rapid-response space science missions and enabling low-cost access to space. Space-based astronomical instrumentation. Service 2013 HST Cycle 21 Proposal Review Panel 2011 NASA APRA/SAT UV/Vis Review Panel Chair 2011 NSF Astronomy Advanced Technology and Instrumentation Opt/IR Panel 2008 – present Astrophysics Sounding Rocket -
Wind Mass Transfer in S-Type Symbiotic Binaries III. Confirmation of a Wind
Astronomy & Astrophysics manuscript no. 39103 ©ESO 2020 December 16, 2020 Wind mass transfer in S-type symbiotic binaries⋆ III. Confirmation of a wind focusing in EG Andromedae from the nebular [O iii] λ5007 line N. Shagatova1, A. Skopal1, S. Yu. Shugarov1, 2, R. Komžík1, E. Kundra1, and F. Teyssier3 1 Astronomical Institute, Slovak Academy of Sciences, 059 60 Tatranská Lomnica, Slovakia e-mail: [email protected] 2 P.K. Sternberg Astronomical Institute, M.V. Lomonosov Moscow State University, Russia 3 Observatoire Rouen Sud (FR) - ARAS group, 76100 Rouen, France Received / Accepted ABSTRACT Context. The structure of the wind from the cool giants in symbiotic binaries carries important information for understanding the wind mass transfer to their white dwarf companions, its fuelling, and thus the path towards different phases of symbiotic-star evolution. Aims. In this paper, we indicate a non-spherical distribution of the neutral wind zone around the red giant (RG) in the symbiotic binary star, EG And. We concentrate in particular on the wind focusing towards the orbital plane and its asymmetry alongside the orbital motion of the RG. Methods. We achieved this aim by analysing the periodic orbital variations of fluxes and radial velocities of individual components of the Hα and [O iii] λ5007 lines observed on our high-cadence medium (R 11 000) and high-resolution (R 38 000) spectra. Results. The asymmetric shaping of the neutral wind zone at the near-orbital-plane∼ region is indicated by: (i)∼ the asymmetric course of the Hα core emission fluxes along the orbit; (ii) the presence of their secondary maximum around the orbital phase ϕ = 0.1, which is possibly caused by the refraction effect; and (iii) the properties of the Hα broad wing emission originating by Raman scattering on H0 atoms. -
The Search for the Elusive Companion of EG Andromedae
The Search for the Elusive Companion of EG Andromedae Joseph E. Pesce and Robert E. Stencel Center for Astrophysics and Space Astronomy University of Colorado Boulder, CO 80309-0391 USA and Nancy A. Oliversen Computer Sciences Corporation Greenbelt, Maryland USA Abstract: We report observations at opposite quadratures of the interacting symbiotic binary EG Andromedae (HD 4174, Period = 470d). Correcting for absolute motion at the system, it appears that many of the nebular lines arise from material that moves with the red giant star. The He II feature appears to track the hot component. It may be possible to use this feature in other, similar systems in order to "pin-down" the mass ratio. The optical spectrum of EG Andromedae was first noted by Wilson (1950) to consist _1 of a high velocity (vr= -96 km s : Oliversen et al, 1985) M2 giant upon which were superposed the optical emission lines of 0 III] and the Balmer series. The ultraviolet spectrum exhibits a far UV continuum and emission lines of C IV, He II, 0 III] and other species. The companion star is thought to be similar to the central star of a planetary nebula (Kenyon 1983). Oliversen et al (1985) have used the spectroscopic motion of the red giant features and an estimate of the mass of the hot object (0.7 M©) to approximate the mass ratio of about 3.5. Oliversen et al report that the red giant optical absorption features undergo an esti mated 15 km s_1 total velocity excursion between orbital quadratures. With a mass ratio of 3.5, we predict that the hot object should exhibit 53 km s_1 in spectral line displace ment. -
Milestone Goto-Bino Series .Cdr
Kson MilestoneK Standard Alt/Az GOTO Mount INSTRUCTIONS CONTENT FOR KSON STANDARD ALT/AZ GOTO USER INTRODUCTION.................................................................................1 ACCESSORIES..................................................................................2 ASSEMBLY INSTRUCTIONS.............................................................3 FEATURES.........................................................................5 OPERATION MANUAL FOR SKYTOUCH CONTROLLER............... 6 KEY DESCRIPTION.................................................................................6 STATUS DESCRIPTION...........................................................................6 OPERATION PROCESS...........................................................................7 POWER ON......................................................................................7 WARNING........................................................................................7 ALIGNMENT STATUS........................................................................7 CHANGE THE DATE..................................................................7 CHANGE THE TIME...................................................................8 CHANGE THE SITE...................................................................8 ALIGNMENT.............................................................................9 NAVIGATION STATUS.....................................................................11 MENU STATUS................................................................................11 -
COMMISSION 27 of the I.A.U. INFORMATION BULLETIN on VARIABLE STARS Nos. 3001
COMMISSION 27 OF THE I.A.U. INFORMATION BULLETIN ON VARIABLE STARS Nos. 3001 - 3100 1987 March - 1987 October EDITORS: L. SZABADOS and B. SZEIDL KONKOLY OBSERVATORY H-1525 BUDAPEST P.O. Box 67, HUNGARY HU ISSN 0374 - 0676 CONTENTS 3001 PHOTOELECTRIC ELEMENTS AND REVISED SPECTRAL TYPES OF XX Cas R.K. Srivastava 18 March 1987 3002 HR 2554 - A POSSIBLE NEW Zeta Aur SYSTEM Thomas B. Ake, S.B. Parsons 19 March 1987 3003 53 PISCIUM - LARGER AMPLITUDE Marek Wolf 23 March 1987 3004 OBSERVATIONS AND A TIME OF MINIMUM OF TV Cet Daniel B. Caton, R. Lee Hawkins 25 March 1987 3005 ON THE PRIMARY MINIMUM OF ECLIPSING BINARY AY Cam J.B. Srivastava, C.D. Kandpal 30 March 1987 3006 AN UNEXPECTEDLY EARLY FADING OF V644 Cen (CPD -60d3278) J.K. Davies, A. Evans, M.F. Bode, D.C.B Whittet 3 April 1987 3007 PHOTOELECTRIC OBSERVATIONS OF TT ARIETIS ON 1/2 OCTOBER 1986 S. Rossiger 6 April 1987 3008 DELTA Cap: A POSSIBLE RS CVn BINARY R.K. Srivastava 9 April 1987 3009 ON THE CONSTANCY OF SOME STARS IN NGC 2287 = MESSIER 41 Brian A. Skiff 13 April 1987 3010 AN IMPROVEMENT OF THE ROTATIONAL PERIOD OF CQ UMa Zdenek Mikulasek 16 April 1987 3011 CORRECT PERIOD OF THE ECLIPSING STAR MN AURIGAE H. Gessner 16 April 1987 3012 JHK LIGHT CURVES OF CG CYGNI J.K. Davies, D.K. Bedford, J.J. Fuensalida, M.J. Arevalo 17 April 1987 3013 OPTICAL BEHAVIOUR OF THE X-RAY BINARY V1727 CYGNI = 4U 2129+47 IN 1986 W.