Sion Meeting—Table of Contents, JAAVSO Volume 35, 2006
Total Page：16
File Type：pdf, Size：1020Kb
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............................................................................................................ -
Antony Hewish
PULSARS AND HIGH DENSITY PHYSICS Nobel Lecture, December 12, 1974 by A NTONY H E W I S H University of Cambridge, Cavendish Laboratory, Cambridge, England D ISCOVERY OF P U L S A R S The trail which ultimately led to the first pulsar began in 1948 when I joined Ryle’s small research team and became interested in the general problem of the propagation of radiation through irregular transparent media. We are all familiar with the twinkling of visible stars and my task was to understand why radio stars also twinkled. I was fortunate to have been taught by Ratcliffe, who first showed me the power of Fourier techniques in dealing with such diffraction phenomena. By a modest extension of existing theory I was able to show that our radio stars twinkled because of plasma clouds in the ionosphere at heights around 300 km, and I was also able to measure the speed of ionospheric winds in this region (1) . My fascination in using extra-terrestrial radio sources for studying the intervening plasma next brought me to the solar corona. From observations of the angular scattering of radiation passing through the corona, using simple radio interferometers, I was eventually able to trace the solar atmo- sphere out to one half the radius of the Earth’s orbit (2). In my notebook for 1954 there is a comment that, if radio sources were of small enough angular size, they would illuminate the solar atmosphere with sufficient coherence to produce interference patterns at the Earth which would be detectable as a very rapid fluctuation of intensity. -
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, -
Flares on Active M-Type Stars Observed with XMM-Newton and Chandra
Flares on active M-type stars observed with XMM-Newton and Chandra Urmila Mitra Kraev Mullard Space Science Laboratory Department of Space and Climate Physics University College London A thesis submitted to the University of London for the degree of Doctor of Philosophy I, Urmila Mitra Kraev, confirm that the work presented in this thesis is my own. Where information has been derived from other sources, I confirm that this has been indicated in the thesis. Abstract M-type red dwarfs are among the most active stars. Their light curves display random variability of rapid increase and gradual decrease in emission. It is believed that these large energy events, or flares, are the manifestation of the permanently reforming magnetic field of the stellar atmosphere. Stellar coronal flares are observed in the radio, optical, ultraviolet and X-rays. With the new generation of X-ray telescopes, XMM-Newton and Chandra , it has become possible to study these flares in much greater detail than ever before. This thesis focuses on three core issues about flares: (i) how their X-ray emission is correlated with the ultraviolet, (ii) using an oscillation to determine the loop length and the magnetic field strength of a particular flare, and (iii) investigating the change of density sensitive lines during flares using high-resolution X-ray spectra. (i) It is known that flare emission in different wavebands often correlate in time. However, here is the first time where data is presented which shows a correlation between emission from two different wavebands (soft X-rays and ultraviolet) over various sized flares and from five stars, which supports that the flare process is governed by common physical parameters scaling over a large range. -
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, -
Download This Issue (Pdf)
Volume 46 Number 2 JAAVSO 2018 The Journal of the American Association of Variable Star Observers Unmanned Aerial Systems for Variable Star Astronomical Observations The NASA Altair UAV in flight. Also in this issue... • A Study of Pulsation and Fadings in some R CrB Stars • Photometry and Light Curve Modeling of HO Psc and V535 Peg • Singular Spectrum Analysis: S Per and RZ Cas • New Observations, Period and Classification of V552 Cas • Photometry of Fifteen New Variable Sources Discovered by IMSNG Complete table of contents inside... The American Association of Variable Star Observers 49 Bay State Road, Cambridge, MA 02138, USA The Journal of the American Association of Variable Star Observers Editor John R. Percy Laszlo L. Kiss Ulisse Munari Dunlap Institute of Astronomy Konkoly Observatory INAF/Astronomical Observatory and Astrophysics Budapest, Hungary of Padua and University of Toronto Asiago, Italy Toronto, Ontario, Canada Katrien Kolenberg Universities of Antwerp Karen Pollard Associate Editor and of Leuven, Belgium Director, Mt. John Observatory Elizabeth O. Waagen and Harvard-Smithsonian Center University of Canterbury for Astrophysics Christchurch, New Zealand Production Editor Cambridge, Massachusetts Michael Saladyga Nikolaus Vogt Kristine Larsen Universidad de Valparaiso Department of Geological Sciences, Valparaiso, Chile Editorial Board Central Connecticut State Geoffrey C. Clayton University, Louisiana State University New Britain, Connecticut Baton Rouge, Louisiana Vanessa McBride Kosmas Gazeas IAU Office of Astronomy for University of Athens Development; South African Athens, Greece Astronomical Observatory; and University of Cape Town, South Africa The Council of the American Association of Variable Star Observers 2017–2018 Director Stella Kafka President Kristine Larsen Past President Jennifer L. -
Uv Ceti Type Variable Stars Presented in the General Catalogue of Variable Stars
IX BULGARIAN-SERBIAN ASTRONOMICAL CONFERENCE: . ASTROINFORMATICS . Sofia, 2 – 4 July, 2014 UV CETI TYPE VARIABLE STARS PRESENTED IN THE GENERAL CATALOGUE OF VARIABLE STARS Katya Tsvetkova Institute of Mathematics and Informatics, Bulgarian Academy of Sciences Sofia, 2 – 4 July, 2014 IX BULGARIAN-SERBIAN ASTRONOMICAL CONFERENCE: . ASTROINFORMATICS . Abstract We present the place and the status of UV Ceti type variable stars in the General Catalogue of Variable Stars (GCVS4, edition April 2013) having in view the improved typological classification, which is accepted in the already prepared GCVS4.2 edition. The improved classification is based on understanding the major astrophysical reasons for variability. The distribution statistics is done on the basis of the data from the GCVS4 and addition of data from the 80th Name List of Variable Stars - altogether 47 967 variable stars with determined type of variability. The class of the eruptive variable stars includes variables showing irregular or semi-regular brightness variations as a consequence of violent processes and flares occurring in their chromospheres and coronae and accompanied by shell events or mass outflow as stellar winds and/or by interaction with the surrounding interstellar matter. In this class the type of the UV Ceti stars is referred together with the types of Irregular variables (Herbig Ae/Be stars; T Tau type stars (classical and weak- line ones), connected with diffuse nebulae, or RW Aurigae type stars without such connection; FU Orionis type; YY Orionis type; Yellow -
GEORGE HERBIG and Early Stellar Evolution
GEORGE HERBIG and Early Stellar Evolution Bo Reipurth Institute for Astronomy Special Publications No. 1 George Herbig in 1960 —————————————————————– GEORGE HERBIG and Early Stellar Evolution —————————————————————– Bo Reipurth Institute for Astronomy University of Hawaii at Manoa 640 North Aohoku Place Hilo, HI 96720 USA . Dedicated to Hannelore Herbig c 2016 by Bo Reipurth Version 1.0 – April 19, 2016 Cover Image: The HH 24 complex in the Lynds 1630 cloud in Orion was discov- ered by Herbig and Kuhi in 1963. This near-infrared HST image shows several collimated Herbig-Haro jets emanating from an embedded multiple system of T Tauri stars. Courtesy Space Telescope Science Institute. This book can be referenced as follows: Reipurth, B. 2016, http://ifa.hawaii.edu/SP1 i FOREWORD I first learned about George Herbig’s work when I was a teenager. I grew up in Denmark in the 1950s, a time when Europe was healing the wounds after the ravages of the Second World War. Already at the age of 7 I had fallen in love with astronomy, but information was very hard to come by in those days, so I scraped together what I could, mainly relying on the local library. At some point I was introduced to the magazine Sky and Telescope, and soon invested my pocket money in a subscription. Every month I would sit at our dining room table with a dictionary and work my way through the latest issue. In one issue I read about Herbig-Haro objects, and I was completely mesmerized that these objects could be signposts of the formation of stars, and I dreamt about some day being able to contribute to this field of study. -
University of Hawai'i, Institute for Astronomy Publications in Calendar
University of Hawai‘i, Institute for Astronomy Publications in Calendar Year 2004 The names of authors listed as affiliated with IfA in each ar- &Wainscoat, R. J. Twenty-Three High-Redshift Super- ticle are in boldface. novae from the Institute for Astronomy Deep Survey: Doubling the Supernova Sample at z > 0.7. ApJ, 602, Abazajian, K., et al., including Siegmund, W. A., & Sza- 571–594 (2004) pudi, I. The Second Data Release of the Sloan Digital Sky Survey. AJ, 128, 502–512 (2004) Bendo, G. J., & Joseph, R. D. Nuclear Stellar Populations in the Infrared Space Observatory Atlas of Bright Spiral Abbas, M. M., LeClair, A., Owen, T., et al. The Nitrogen Galaxies. AJ, 127, 3338–3360 (2004) Isotopic Ratio in Jupiter’s Atmosphere from Observations by the Composite Infrared Spectrometer on the Cassini Bettoni, D., Mazzei, P., Della Valle, A., Franceschini, G. D. Spacecraft. ApJ, 602, 1063–1074 (2004) A., & Aussel, H. Optical and Spectroscopic Follow-Up of the Deeper FIR Selected Sample. Mem. Soc. Astron. Abel, N. P., Brogan, C. L., Ferland, G. J., O’Dell, C. R., Italiana Suppl., 5, 267–271 (2004) Shaw, G., & Troland, T. H. Physical Conditions in Orion’s Veil. ApJ, 609, 247–260 (2004) Beuzit, J.-L., et al., including Roddier, C., Roddier, F., & Mart´ın, E. L. New Neighbours. III. 21 New Compan- Allen, S. W., Schmidt, R. W., Ebeling, H., Fabian, A. C., ions to Nearby Dwarfs, Discovered with Adaptive Optics. &van Speybroeck, L. Constraints on Dark Energy from A&A, 425, 997–1008 (2004) Chandra Observations of the Largest Relaxed Galaxy Clusters. -
Index to JRASC Volumes 61-90 (PDF)
THE ROYAL ASTRONOMICAL SOCIETY OF CANADA GENERAL INDEX to the JOURNAL 1967–1996 Volumes 61 to 90 inclusive (including the NATIONAL NEWSLETTER, NATIONAL NEWSLETTER/BULLETIN, and BULLETIN) Compiled by Beverly Miskolczi and David Turner* * Editor of the Journal 1994–2000 Layout and Production by David Lane Published by and Copyright 2002 by The Royal Astronomical Society of Canada 136 Dupont Street Toronto, Ontario, M5R 1V2 Canada www.rasc.ca — [email protected] Table of Contents Preface ....................................................................................2 Volume Number Reference ...................................................3 Subject Index Reference ........................................................4 Subject Index ..........................................................................7 Author Index ..................................................................... 121 Abstracts of Papers Presented at Annual Meetings of the National Committee for Canada of the I.A.U. (1967–1970) and Canadian Astronomical Society (1971–1996) .......................................................................168 Abstracts of Papers Presented at the Annual General Assembly of the Royal Astronomical Society of Canada (1969–1996) ...........................................................207 JRASC Index (1967-1996) Page 1 PREFACE The last cumulative Index to the Journal, published in 1971, was compiled by Ruth J. Northcott and assembled for publication by Helen Sawyer Hogg. It included all articles published in the Journal during the interval 1932–1966, Volumes 26–60. In the intervening years the Journal has undergone a variety of changes. In 1970 the National Newsletter was published along with the Journal, being bound with the regular pages of the Journal. In 1978 the National Newsletter was physically separated but still included with the Journal, and in 1989 it became simply the Newsletter/Bulletin and in 1991 the Bulletin. That continued until the eventual merger of the two publications into the new Journal in 1997. -
Prof.Dr. Mustafa Türker ÖZKAN
Prof.Dr. Mustafa Türker ÖZKAN İKşi Tşiesleflo Bniul:g +il9e0r 212 440 0369 Dahili: 10294 EF-apxo Tsetale: fooznkuan: t+@9is0t a2n1b2u 4l.4ed0u 0.t3r70 PWoesbta: hAtdtpr:e//sai:v Aess.tirsotannobmuil .evde uU.tzra/yo Bzkilaimntl/eri Bölümü, İstanbul Üniversitesi Beyazıt Yerleşkesi, 34119, Fatih-İstanbul EDoğkitoimra, Bİsitalgnibluelr Üiniversitesi, Fen Fakültesi, Astronomi Ve Uzay Bilimleri, Türkiye 1981 - 1987 LYiüskasnesk, İLsitsaannbsu, lİ sÜtnanivbeurls iÜtensivi, eFresnit eFsai,k Füeltne sFi,a Aküstlrteosni,o Amsit rVoen Uozmaiy V Bei lUimzaleyr Bi, iTliümrlkeiryie, T1ü9r7k3iy -e 1 1997778 - 1980 Yİnagbiliazcnec, Bı 2D Oilrltea rÜstü Yaptığı Tezler vDeo Uktzoarya B, Gilüimnleeşr iL Beköelülemriün, d1e9k8i 7Doğu-Batı Asimetrisinin Nedenleri Üzerine, İstanbul Üniversitesi, Fen Fakültesi, Astronomi vYeü kUszeaky LBisilaimnsle, rPil aBnöelüt mveü Ç, 1if9t-8Y0ıldız Yörüngelerinde Büyük Eksen Dönmesi, İstanbul Üniversitesi, Fen Fakültesi, Astronomi Araştırma Alanları AFisztirko, nAosmtroikn goömzil evme lAers,t rYoılfdizızikla, rG, üTneemş evle B Gilüimnleeşr Sistemleri, Temel Astronomi ve Astrofizik: Enstrümantasyon, Teknikler ve Akademik Unvanlar / Görevler DProoçf.D.Drr.,. , İİssttaannbbuull ÜÜnniivveerrssiitteessii, , FFeenn FFaakküülltteessii, , AAssttrroonnoommii vvee UUzzaayy BBiilliimmlleerrii BBööllüümmüü, , 11999905 -- 1D9e9v5am Ediyor AYrdaş.Dtıormç.Da rG., öİsrteavnlibsui, lİ sÜtnainvbeursl iÜtensiiv, eFresnit eFsaik, Füeltne sFi,a Aksütlrteosnio, Amsit rvoen Uozmayi vBei lUimzaleyr iB Bilöimlülemrüi ,B 1ö9lü8m7 ü- ,1 1999805 -
The Kepler Catalog of Stellar Flares James R
Western Washington University Masthead Logo Western CEDAR Physics & Astronomy College of Science and Engineering 9-20-2016 The Kepler Catalog of Stellar Flares James R. A. Davenport Western Washington University, [email protected] Follow this and additional works at: https://cedar.wwu.edu/physicsastronomy_facpubs Part of the Stars, Interstellar Medium and the Galaxy Commons Recommended Citation Davenport, James R. A., "The Kepler Catalog of Stellar Flares" (2016). Physics & Astronomy. 15. https://cedar.wwu.edu/physicsastronomy_facpubs/15 This Article is brought to you for free and open access by the College of Science and Engineering at Western CEDAR. It has been accepted for inclusion in Physics & Astronomy by an authorized administrator of Western CEDAR. For more information, please contact [email protected]. The Astrophysical Journal, 829:23 (12pp), 2016 September 20 doi:10.3847/0004-637X/829/1/23 © 2016. The American Astronomical Society. All rights reserved. THE KEPLER CATALOG OF STELLAR FLARES James R. A. Davenport1 Department of Physics & Astronomy, Western Washington University, Bellingham, WA 98225, USA Received 2016 June 20; revised 2016 July 7; accepted 2016 July 12; published 2016 September 16 ABSTRACT A homogeneous search for stellar flares has been performed using every available Kepler light curve. An iterative light curve de-trending approach was used to filter out both astrophysical and systematic variability to detect flares. The flare recovery completeness has also been computed throughout each light curve using artificial flare injection tests, and the tools for this work have been made publicly available. The final sample contains 851,168 candidate flare events recovered above the 68% completeness threshold, which were detected from 4041 stars, or 1.9% of the stars in the Kepler database.