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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............................................................................................................ -
Unknown Amorphous Carbon II. LRS SPECTRA the Sample Consists Of
Table I A summary of the spectral -features observed in the LRS spectra of the three groups o-f carbon stars. The de-finition o-f the groups is given in the text. wavelength Xmax identification Group I B - 12 urn E1 9.7 M™ Silicate 12 - 23 jim E IB ^m Silicate Group II < 8.5 M"i A C2H2 CS? 12 - 16 f-i/n A 13.7 - 14 Mm C2H2 HCN? 8 - 10 Mm E 8.6 M"i Unknown 10 - 13 Mm E 11.3 - 11 .7 M«> SiC Group III 10 - 13 MJn E 11.3 - 11 .7 tun SiC B - 23 Htn C Amorphous carbon 1 The letter in this column indicates the nature o-f the -feature: A = absorption; E = emission; C indicates the presence of continuum opacity. II. LRS SPECTRA The sample consists of 304 carbon stars with entries in the LRS catalog (Papers I-III). The LRS spectra have been divided into three groups. Group I consists of nine stars with 9.7 and 18 tun silicate features in their LRS spectra pointing to oxygen-rich dust in the circumstellar shell. These sources are discussed in Paper I. The remaining stars all have spectra with carbon-rich dust features. Using NIR photometry we have shown that in the group II spectra the stellar photosphere is the dominant continuum. The NIR color temperature is of the order of 25OO K. Paper II contains a discussion of sources with this class of spectra. The continuum in the group III spectra is probably due to amorphous carbon dust. -
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. -
Title of the Paper
Variable Star and Exoplanet Section of Czech Astronomical Society and Planetarium Ostrava Proceedings of the 51st Conference on Variable Stars Research Planetarium Ostrava, Ostrava, Czech Republic 1st November - 3rd November 2019 Editor-in-chief Radek Kocián Participants of the conference OPEN EUROPEAN JOURNAL ON VARIABLE STARS November 2020 http://oejv.physics.muni.cz ISSN 1801-5964 DOI: 10.5817/OEJV2020-0208 TABLE OF CONTENTS Modeling of GX Lacertae ........................................................................................................................................ 5 Cataclysmic variable CzeV404 Her ......................................................................................................................... 8 On the spin period variability in intermediate polars ............................................................................................. 11 Photometric and spectroscopic observation of symbiotic variables at private observatory Liptovská Štiavnica ... 18 Outburst activity of flare stars 2014 – 2019 ........................................................................................................... 29 2 OPEN EUROPEAN JOURNAL ON VARIABLE STARS November 2020 http://oejv.physics.muni.cz ISSN 1801-5964 DOI: 10.5817/OEJV2020-0208 INTRODUCTION The Variable Star and Exoplanet Section of the Czech Astronomical Society organized traditional autumn conference on research and news in the field of variable stars. The conference was held in a comfortable space of Ostrava Planetarium. In addition -
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. -
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, -
Contents Sisukord
Contents Sisukord Eessõna ................................... 8 Foreword.................................. 9 1 Ülevaade 10 1.1 Uurimisteemad ja grandid ..................... 10 1.1.1 Sihtfinantseeritavad teadusteemad ............ 10 1.1.2 Eesti Teadusagentuuri grandid .............. 10 1.1.3 Euroopa Liidu 7. raamprogrammi projektid ...... 11 1.1.4 Euroopa kosmoseagentuuri Euroopa koostööriikide programmi projektid .................... 11 1.1.5 Euroopa Liidu struktuuritoetused ............ 11 1.1.6 COST projektid ....................... 13 1.1.7 Muud projektid ja lepingud ................ 13 1.2 Töötajad ............................... 14 1.3 Tunnustused ............................. 15 1.4 Eelarve ................................ 17 1.5 Aparatuur ja seadmed ....................... 18 1.6 Teadusnõukogu töö ......................... 19 1.7 Suhted avalikkusega ........................ 20 1.8 Tänuavaldused ........................... 23 2 Summary 24 2.1 Researchprojectsandgrants. 24 2.1.1 Targetfinancedprojects . 24 2.1.2 EstonianResearchCouncilgrants . 24 2.1.3 The European Commission 7th Framework Program- meprojects ......................... 25 2.1.4 European Space Agency Programme for European CooperatingStates . 25 2.1.5 FinancingfromtheEUStructuralFunds. 25 2.1.6 COSTprojects........................ 27 2.1.7 Someotherprojectsandcontracts . 27 2.2 Staff.................................. 28 2.3 Awards................................ 29 2.4 Budget ................................ 31 2.5 Instrumentsandfacilities . 32 3 2.6 ScientificCouncil -
The Planets for 1955 24 Eclipses, 1955 ------29 the Sky and Astronomical Phenomena Month by Month - - 30 Phenomena of Jupiter’S S a Te Llite S
THE OBSERVER’S HANDBOOK FOR 1955 PUBLISHED BY The Royal Astronomical Society of Canada C. A. C H A N T, E d ito r RUTH J. NORTHCOTT, A s s is t a n t E d ito r DAVID DUNLAP OBSERVATORY FORTY-SEVENTH YEAR OF PUBLICATION P r i c e 50 C e n t s TORONTO 13 Ross S t r e e t Printed for th e Society By the University of Toronto Press THE ROYAL ASTRONOMICAL SOCIETY OF CANADA The Society was incorporated in 1890 as The Astronomical and Physical Society of Toronto, assuming its present name in 1903. For many years the Toronto organization existed alone, but now the Society is national in extent, having active Centres in Montreal and Quebec, P.Q.; Ottawa, Toronto, Hamilton, London, and Windsor, Ontario; Winnipeg, Man.; Saskatoon, Sask.; Edmonton, Alta.; Vancouver and Victoria, B.C. As well as nearly 1000 members of these Canadian Centres, there are nearly 400 members not attached to any Centre, mostly resident in other nations, while some 200 additional institutions or persons are on the regular mailing list of our publications. The Society publishes a bi-monthly J o u r n a l and a yearly O b s e r v e r ’s H a n d b o o k . Single copies of the J o u r n a l are 50 cents, and of the H a n d b o o k , 50 cents. Membership is open to anyone interested in astronomy. Annual dues, $3.00; life membership, $40.00. -
Spectral Observations of AG Draconis During Quiescence and Outburst (1993–1995)
Astron. Astrophys. 347, 151–163 (1999) ASTRONOMY AND ASTROPHYSICS Spectral observations of AG Draconis during quiescence and outburst (1993–1995) M.T. Tomova and N.A. Tomov National Astronomical Observatory Rozhen, P.O. Box 136, BG-4700 Smolyan, Bulgaria ([email protected]) Received 30 July 1998 / Accepted 1 February 1999 Abstract. High and intermediate resolution observations of the depends on the nebula’s velocity field, which on its side is deter- blue and the Hα spectral regions of the symbiotic star AG Dra mined by the components’ interaction. That is why investigation at quiescence and during an active phase in 1994 and 1995 of the interaction in the symbiotic stars is of prime importance were performed. Variationsof profiles, fluxes and radial velocity for understanding their nature. data of a number of emission lines are investigated. The width The star AG Dra (BD +67◦922) is a known symbiotic (FWHM) of all of these lines was very large at times close to the system with high galactic latitude, large barycentric velocity 1 1994 light maximum. The emission measure of the surrounding γ = 148 km s− and a relatively early spectral type (K). Its nebula was also calculated using Balmer continuum emission photometric− period is about 550d (Meinunger 1979; Skopal on the basis of U photometric observations from the literature. 1994). The consistency of this period with the orbital period It turned out that at the times of the 1994 and 1995 visual light of the binary is confirmed by radial velocity variations of the maxima the emission measure has increased by a factor of 15 cool primary component, measured by Garcia & Kenyon (1988), and 8 respectively, compared with its quiescent maximal value. -
A Review of the Disc Instability Model for Dwarf Novae, Soft X-Ray Transients and Related Objects a J.M
A review of the disc instability model for dwarf novae, soft X-ray transients and related objects a J.M. Hameury aObservatoire Astronomique de Strasbourg ARTICLEINFO ABSTRACT Keywords: I review the basics of the disc instability model (DIM) for dwarf novae and soft-X-ray transients Cataclysmic variable and its most recent developments, as well as the current limitations of the model, focusing on the Accretion discs dwarf nova case. Although the DIM uses the Shakura-Sunyaev prescription for angular momentum X-ray binaries transport, which we know now to be at best inaccurate, it is surprisingly efficient in reproducing the outbursts of dwarf novae and soft X-ray transients, provided that some ingredients, such as irradiation of the accretion disc and of the donor star, mass transfer variations, truncation of the inner disc, etc., are added to the basic model. As recently realized, taking into account the existence of winds and outflows and of the torque they exert on the accretion disc may significantly impact the model. I also discuss the origin of the superoutbursts that are probably due to a combination of variations of the mass transfer rate and of a tidal instability. I finally mention a number of unsolved problems and caveats, among which the most embarrassing one is the modelling of the low state. Despite significant progresses in the past few years both on our understanding of angular momentum transport, the DIM is still needed for understanding transient systems. 1. Introduction tems using Doppler tomography techniques (Steeghs et al. 1997; Marsh and Horne 1988; see also Marsh and Schwope Dwarf novae (DNe) are cataclysmic variables (CV) that 2016 for a recent review). -
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, -
Present Status and Future Directions of the EVN
http://www.evlbi.org/ Present status and future directions of the EVN Michael Lindqvist, Onsala Space Observatory Zsolt Paragi, JIVE Onsala Space Observatory http://www.evlbi.org/ Thanks Tasso! Onsala Space Observatory http://www.evlbi.org/ VLBI science • Radio jet & black hole physics • Radio source evolution • Astrometry • Galactic and extra-galactic masers • Gravitational lenses • Supernovae and gamma-ray-burst studies • Nearby and distant starburst galaxies • Nature of faint radio source population • HI absorption studies in AGN • Space science VLBI • Transients • SETI Onsala Space Observatory http://www.evlbi.org/ Description of the EVN • The European VLBI Network (EVN) was formed in 1980. Today it includes 15 major institutes, including the Joint Institute for VLBI ERIC, JIVE • JIVE operates EVN correlator. JIVE is also involved in supporting EVN users and operations of EVN as a facility. JIVE has officially been established as an European Research Infrastructure Consortium (ERIC). • The EVN operates an “open sky” policy • No standing centralised budget for the EVN - distributed European facility Onsala Space Observatory http://www.evlbi.org/ The network Onsala Space Observatory http://www.evlbi.org/ EVN and e-VLBI From tape reel to intercontinental light paths • Pieces falling into place around 2003: – Introduction of Mark5 recording system (game changer) by Haystack Observatory – Emergence of high bandwidth optical fibre networks e-VLBI JIVE Hot scienceJIVE • The development of e-VLBI has been spearheaded by the JIVE/EVN (EXPReS, Garrett) • In this way, the EVN/JIVE is a recognized SKA pathfinder Onsala Space Observatory http://www.evlbi.org/ e-VLBI - rapid turn-around • e-VLBI has made rapid turn-around possible – X-ray, γ-ray binaries in flaring states (including novae) – AGN γ-ray outbursts — locus of VHE emission – Other high-energy flaring (e.g., Crab) – Outbursts in Mira variables (spectral-line) – Just-exploded GRBs, SNe – Binaries (incl.