Observational Evidence for Tidal Interaction in Close Binary Systems, Including Short-Period Extrasolar Planets
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The Effect of the Apsidal Motion on the Light Curve of the Close Binary HD 93205 (O3V+O8V)?
A&A 397, 921–925 (2003) Astronomy DOI: 10.1051/0004-6361:20021438 & c ESO 2003 Astrophysics The effect of the apsidal motion on the light curve of the close binary HD 93205 (O3V+O8V)? A. M. van Genderen?? Leiden Observatory, Postbus 9513, 2300 RA Leiden, The Netherlands Received 25 June 2002/Accepted 28 August 2002 Abstract. The 1982–1985 photometry (VBLUW system) of the O3V+O8V close binary HD 93205 has been rediscussed be- cause of new insights into its true nature and orbital changes. By comparing this data set with the one obtained by Antokhina et al. (2000) in 1993, and using the same ephemeris to construct the light curve in the phase diagram, the effect of the apsidal motion became obvious: a phase shift between the two light curves and a small change of the shape. A phase-locked light variationintheL passband (containing the higher Balmer lines) is clearly present in the 1982–1985 data set and is presumably due to absorption if the O8 star is seen through cooler inter-binary gas, e.g. the bow-shock between the two colliding winds. Key words. stars: variables: general – stars: binaries: close – stars: early-type – stars: individual: HD 93205 1. Introduction Sect. 2). So far only the observations in the V band relative to the comparison star were published (Papers I, IX). The phase HD 93205 (O3V+O8V) is the earliest known system for which diagrams of the 1982–1985 and 1993 data sets, the latter from an RV is known, of which the first was presented by Conti & Antokhina et al. -
Journal Reprints-Astronomy/Download/8526
SPACE PATTERNS AND PAINTINGS (published in the "Engineer" magazine No. 8-9, 2012) Sagredo. - If the end of the pen, which was on the ship during my entire voyage from Venice to Alexandretta, were able to leave a visible trace of its entire path, then what kind of trace, what mark, what line would it leave? Simplicio. - I would leave a line stretching from Venice to the final place, not completely straight, or rather, extended in the form of an arc of a circle, but more or less wavy, depending on how much the ship swayed along the way ... Sagredo. - If, therefore, the artist, upon leaving the harbor, began to draw with this pen on a sheet of paper and continued drawing until Alexandretta, he could get from his movement a whole picture of figures ... at least a trace left ... by the end of the pen would be nothing more than a very long and simple line. G. Galileo "Dialogue on the two main systems of the world" Space has been giving astronomers surprise after surprise lately. A number of mysterious space objects were discovered that were not predicted by astrophysics and contradicted it. The more advanced observation methods become, the more such surprises. At one time, I. Shklovsky argued that the discovery of such "cosmic wonders" would confirm the reality of extraterrestrial intelligence, its enormous technical capabilities. But in reality, the "cosmic miracles" showed the backwardness of terrestrial science, which the opium of relativism smiled so much that now it cannot clearly explain ordinary cosmic phenomena caused by natural causes. -
X-Ray Study of Stellar Winds with Suzaku
X-ray Study of Stellar Winds with Suzaku Yoshiaki Hyodo Department of Physics, Graduate School of Science, Kyoto University Kitashirakawa Oiwake-cho, Sakyo-ku, Kyoto, 606-8502, Japan [email protected] This thesis was submitted to the Department of Physics, Graduate School of Science, Kyoto University on January 5 2009 in partial fulfillment of the requirements for the degree of Doctor of Philosophy in physics. Abstract Stellar winds from massive stars play an important role for dynamical and chemical evolution of galaxies. To evaluate their effects in a galaxy scale, both the total number and the properties of massive stars should be understood. Most massive stars have soft X-ray emission, while some have additional hard emission. Although it is indicated that the binarity is important, the condition for hard X-ray production has not yet been elucidated. Also, some massive star clusters exhibit diffuse (pc scale) X-ray emission, where stellar winds may be depositing energy to the interstellar space. However, previous studies were not able to clarify the origin of the diffuse emission. It is even unclear whether the emission is physically related to the star cluster or not. The X-ray Imaging Spectrometer (XIS) on board Suzaku has a good energy resolution, a low and stable background, and a large effective area, which are suited for narrow-band surveys and spectroscopy of both point-like and extended X-ray emission. Using the XIS, we performed a very deep survey in the direction of the central region of our Galaxy and pointing observations of three well-known star forming regions in our Galaxy (M 17, the Carina Nebula, and the Arches cluster). -
LIST of PUBLICATIONS Aryabhatta Research Institute of Observational Sciences ARIES (An Autonomous Scientific Research Institute
LIST OF PUBLICATIONS Aryabhatta Research Institute of Observational Sciences ARIES (An Autonomous Scientific Research Institute of Department of Science and Technology, Govt. of India) Manora Peak, Naini Tal - 263 129, India (1955−2020) ABBREVIATIONS AA: Astronomy and Astrophysics AASS: Astronomy and Astrophysics Supplement Series ACTA: Acta Astronomica AJ: Astronomical Journal ANG: Annals de Geophysique Ap. J.: Astrophysical Journal ASP: Astronomical Society of Pacific ASR: Advances in Space Research ASS: Astrophysics and Space Science AE: Atmospheric Environment ASL: Atmospheric Science Letters BA: Baltic Astronomy BAC: Bulletin Astronomical Institute of Czechoslovakia BASI: Bulletin of the Astronomical Society of India BIVS: Bulletin of the Indian Vacuum Society BNIS: Bulletin of National Institute of Sciences CJAA: Chinese Journal of Astronomy and Astrophysics CS: Current Science EPS: Earth Planets Space GRL : Geophysical Research Letters IAU: International Astronomical Union IBVS: Information Bulletin on Variable Stars IJHS: Indian Journal of History of Science IJPAP: Indian Journal of Pure and Applied Physics IJRSP: Indian Journal of Radio and Space Physics INSA: Indian National Science Academy JAA: Journal of Astrophysics and Astronomy JAMC: Journal of Applied Meterology and Climatology JATP: Journal of Atmospheric and Terrestrial Physics JBAA: Journal of British Astronomical Association JCAP: Journal of Cosmology and Astroparticle Physics JESS : Jr. of Earth System Science JGR : Journal of Geophysical Research JIGR: Journal of Indian -
Information Bulletin on Variable Stars
COMMISSIONS AND OF THE I A U INFORMATION BULLETIN ON VARIABLE STARS Nos November July EDITORS L SZABADOS K OLAH TECHNICAL EDITOR A HOLL TYPESETTING K ORI ADMINISTRATION Zs KOVARI EDITORIAL BOARD L A BALONA M BREGER E BUDDING M deGROOT E GUINAN D S HALL P HARMANEC M JERZYKIEWICZ K C LEUNG M RODONO N N SAMUS J SMAK C STERKEN Chair H BUDAPEST XI I Box HUNGARY URL httpwwwkonkolyhuIBVSIBVShtml HU ISSN COPYRIGHT NOTICE IBVS is published on b ehalf of the th and nd Commissions of the IAU by the Konkoly Observatory Budap est Hungary Individual issues could b e downloaded for scientic and educational purp oses free of charge Bibliographic information of the recent issues could b e entered to indexing sys tems No IBVS issues may b e stored in a public retrieval system in any form or by any means electronic or otherwise without the prior written p ermission of the publishers Prior written p ermission of the publishers is required for entering IBVS issues to an electronic indexing or bibliographic system to o CONTENTS C STERKEN A JONES B VOS I ZEGELAAR AM van GENDEREN M de GROOT On the Cyclicity of the S Dor Phases in AG Carinae ::::::::::::::::::::::::::::::::::::::::::::::::::: : J BOROVICKA L SAROUNOVA The Period and Lightcurve of NSV ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::::::::::: W LILLER AF JONES A New Very Long Period Variable Star in Norma ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::::::::::::: EA KARITSKAYA VP GORANSKIJ Unusual Fading of V Cygni Cyg X in Early November ::::::::::::::::::::::::::::::::::::::: -
FY13 High-Level Deliverables
National Optical Astronomy Observatory Fiscal Year Annual Report for FY 2013 (1 October 2012 – 30 September 2013) Submitted to the National Science Foundation Pursuant to Cooperative Support Agreement No. AST-0950945 13 December 2013 Revised 18 September 2014 Contents NOAO MISSION PROFILE .................................................................................................... 1 1 EXECUTIVE SUMMARY ................................................................................................ 2 2 NOAO ACCOMPLISHMENTS ....................................................................................... 4 2.1 Achievements ..................................................................................................... 4 2.2 Status of Vision and Goals ................................................................................. 5 2.2.1 Status of FY13 High-Level Deliverables ............................................ 5 2.2.2 FY13 Planned vs. Actual Spending and Revenues .............................. 8 2.3 Challenges and Their Impacts ............................................................................ 9 3 SCIENTIFIC ACTIVITIES AND FINDINGS .............................................................. 11 3.1 Cerro Tololo Inter-American Observatory ....................................................... 11 3.2 Kitt Peak National Observatory ....................................................................... 14 3.3 Gemini Observatory ........................................................................................ -
IAU Symp 269, POST MEETING REPORTS
IAU Symp 269, POST MEETING REPORTS C.Barbieri, University of Padua, Italy Content (i) a copy of the final scientific program, listing invited review speakers and session chairs; (ii) a list of participants, including their distribution on gender (iii) a list of recipients of IAU grants, stating amount, country, and gender; (iv) receipts signed by the recipients of IAU Grants (done); (v) a report to the IAU EC summarizing the scientific highlights of the meeting (1-2 pages). (vi) a form for "Women in Astronomy" statistics. (i) Final program Conference: Galileo's Medicean Moons: their Impact on 400 years of Discovery (IAU Symposium 269) Padova, Jan 6-9, 201 Program Wednesday 6, location: Centro San Gaetano, via Altinate 16.0 0 – 18.00 meeting of Scientific Committee (last details on the Symp 269; information on the IYA closing ceremony program) 18.00 – 20.00 welcome reception Thursday 7, morning: Aula Magna University 8:30 – late registrations 09.00 – 09.30 Welcome Addresses (Rector of University, President of COSPAR, Representative of ESA, President of IAU, Mayor of Padova, Barbieri) Session 1, The discovery of the Medicean Moons, the history, the influence on human sciences Chair: R. Williams Speaker Title 09.30 – 09.55 (1) G. Coyne Galileo's telescopic observations: the marvel and meaning of discovery 09.55 – 10.20 (2) D. Sobel Popular Perceptions of Galileo 10.20 – 10.45 (3) T. Owen The slow growth of human humility (read by Scott Bolton) 10.45 – 11.10 (4) G. Peruzzi A new Physics to support the Copernican system. Gleanings from Galileo's works 11.10 – 11.35 Coffee break Session 1b Chair: T. -
Orion® Intelliscope® Computerized Object Locator
INSTRUCTION MANUAL Orion® IntelliScope® Computerized Object Locator #7880 Providing Exceptional Consumer Optical Products Since 1975 Customer Support (800) 676-1343 E-mail: [email protected] Corporate Offices (831) 763-7000 89 Hangar Way, Watsonville, CA 95076 IN 229 Rev. G 01/09 Congratulations on your purchase of the Orion IntelliScope™ Com pu ter ized Object Locator. When used with any of the SkyQuest IntelliScope XT Dobsonians, the object locator (controller) will provide quick, easy access to thousands of celestial objects for viewing with your telescope. Coil cable jack The controller’s user-friendly keypad combined with its database of more than 14,000 RS-232 jack celestial objects put the night sky literally at your fingertips. You just select an object to view, press Enter, then move the telescope manually following the guide arrows on the liquid crystal display (LCD) screen. In seconds, the IntelliScope’s high-resolution, 9,216- step digital encoders pinpoint the object, placing it smack-dab in the telescope’s field of Backlit liquid-crystal display view! Easy! Compared to motor-dependent computerized telescopes systems, IntelliScope is faster, quieter, easier, and more power efficient. And IntelliScope Dobs eschew the complex initialization, data entry, or “drive training” procedures required by most other computer- ized telescopes. Instead, the IntelliScope setup involves simply pointing the scope to two bright stars and pressing the Enter key. That’s it — then you’re ready for action! These instructions will help you set up and properly operate your Intelli Scope Com pu ter- ized Object Locator. Please read them thoroughly. Table of Contents 1. -
Arxiv:1008.3235V2 [Astro-Ph.HE] 30 Aug 2010 .Roth M
F ermi Large Area Telescope Observation of a Gamma-ray Source at the Position of Eta Carinae A. A. Abdo1,2, M. Ackermann3, M. Ajello3, A. Allafort3, L. Baldini4, J. Ballet5, G. Barbiellini6,7, D. Bastieri8,9, K. Bechtol3, R. Bellazzini4, B. Berenji3, R. D. Blandford3, E. Bonamente10,11, A. W. Borgland3, A. Bouvier3, T. J. Brandt12,13, J. Bregeon4, A. Brez4, M. Brigida14,15, P. Bruel16, R. Buehler3, T. H. Burnett17, G. A. Caliandro18, R. A. Cameron3, P. A. Caraveo19, S. Carrigan9, J. M. Casandjian5, C. Cecchi10,11, O.¨ C¸elik20,21,22, S. Chaty5, A. Chekhtman1,23, C. C. Cheung1,2, J. Chiang3, S. Ciprini11, R. Claus3, J. Cohen-Tanugi24, L. R. Cominsky25, J. Conrad26,27,28, C. D. Dermer1, F. de Palma14,15, S. W. Digel3, E. do Couto e Silva3, P. S. Drell3, R. Dubois3, D. Dumora29,30, C. Favuzzi14,15, S. J. Fegan16, E. C. Ferrara20, M. Frailis31,32, Y. Fukazawa33, P. Fusco14,15, F. Gargano15, N. Gehrels20, S. Germani10,11, N. Giglietto14,15, F. Giordano14,15, G. Godfrey3, I. A. Grenier5, M.-H. Grondin29,30, J. E. Grove1, L. Guillemot34,29,30, S. Guiriec35, D. Hadasch36, Y. Hanabata33, A. K. Harding20, M. Hayashida3, E. Hays20, A. B. Hill37,38, D. Horan16, R. E. Hughes13, R. Itoh33, M. S. Jackson39,27, G. J´ohannesson3, A. S. Johnson3, W. N. Johnson1, T. Kamae3, H. Katagiri33, J. Kataoka40, M. Kerr17, J. Kn¨odlseder12, M. Kuss4, J. Lande3, L. Latronico4, S.-H. Lee3, M. Lemoine-Goumard29,30, M. Livingstone41, M. Llena Garde26,27, F. Longo6,7, F. Loparco14,15, M. -
2005 Astronomy Magazine Index
2005 Astronomy Magazine Index Subject index flyby of Titan, 2:72–77 Einstein, Albert, 2:30–53 Cassiopeia (constellation), 11:20 See also relativity, theory of Numbers Cassiopeia A (supernova), stellar handwritten manuscript found, 3C 58 (star remnant), pulsar in, 3:24 remains inside, 9:22 12:26 3-inch telescopes, 12:84–89 Cat's Eye Nebula, dying star in, 1:24 Einstein rings, 11:27 87 Sylvia (asteroid), two moons of, Celestron's ExploraScope telescope, Elysium Planitia (on Mars), 5:30 12:33 2:92–94 Enceladus (Saturn's moon), 11:32 2003 UB313, 10:27, 11:68–69 Cepheid luminosities, 1:72 atmosphere of water vapor, 6:22 2004, review of, 1:31–40 Chasma Boreale (on Mars), 7:28 Cassini flyby, 7:62–65, 10:32 25143 (asteroid), 11:27 chonrites, and gamma-ray bursts, 5:30 Eros (asteroid), 11:28 coins, celestial images on, 3:72–73 Eso Chasma (on Mars), 7:28 color filters, 6:67 Espenak, Fred, 2:86–89 A Comet Hale-Bopp, 7:76–79 extrasolar comets, 9:30 Aeolis (on Mars), 3:28 comets extrasolar planets Alba Patera (Martian volcano), 2:28 from beyond solar system, 12:82 first image of, 4:20, 8:26 Aldrin, Buzz, 5:40–45 dust trails of, 12:72–73 first light from, who captured, 7:30 Altair (star), 9:20 evolution of, 9:46–51 newly discovered low-mass planets, Amalthea (Jupiter's moon), 9:28 extrasolar, 9:30 1:68–71 amateur telescopes. See telescopes, Conselice, Christopher, 1:20 smallest, 9:26 amateur constellations whether have diamond layers, 5:26 Andromeda Galaxy (M31), 10:84–89 See also names of specific extraterrestrial life, 4:28–34 disk of stars surrounding, 7:28 constellations eyepieces, telescope. -
Accretion-Ejection Morphology of the Microquasar SS 433 Resolved at Sub-Au Scale with VLTI/GRAVITY
Accretion-ejection morphology of the microquasar SS 433 resolved at sub-au scale with VLTI/GRAVITY P.-O. Petrucci1, I. Waisberg2, J.-B Lebouquin1, J. Dexter2, G. Dubus1, K. Perraut1, F. Eisenhauer2 and the GRAVITY collaboration 1 Institute of Planetology and Astrophysics of Grenoble, France 2 Max Planck Institute fur Extraterrestrische Physik, Garching, Germany 1 What is SS 433? •SS 433 discovered in the 70’s. In the galactic plane. K=8.1! •At a distance of 5.5 kpc, embedded in the radio nebula W50 •Eclipsing binary with Period of ~13.1 days, the secondary a A-type supergiant star and the primary may be a ~10 Msun BH. 70 arcmin SS 433 130 arcmin W50 supernova remnant in radio (green) against the infrared background of stars and dust (red). 2 Moving Lines: Jet Signatures Medvedev et al. (2010) • Optical/IR spectrum: Hβ ‣ Broad emission lines (stationary lines) Hδ+ H!+ Hβ- Hβ+ ‣ Doppler (blue and red) shifted lines (moving lines) HeII CIII/NIII HeI 3 Moving Lines: Jet Signatures Medvedev et al. (2010) • Optical/IR spectrum: Hβ ‣ Broad emission lines (stationary lines) Hδ+ H!+ Hβ- Hβ+ ‣ Doppler (blue and red) shifted lines (moving lines) HeII CIII/NIII HeI •Variable, periodic, Doppler shifts reaching ~50000 km/s in redshift and ~30000 km/s in blueshift •Rapidly interpreted as signature of collimated, oppositely ejected jet periodicity of ~162 days (v~0.26c) precessing (162 days) and nutating (6.5 days) Figure 3: Precessional curves of the radial velocities of theshiftedlinesfromtheapproaching3 (lower curve) and receding (upper curve) jets, derived from spectroscopic data obtained during the first two years in which SS433 was studied (Ciatti et al. -
CANDIDATE X-RAY-EMITTING OB STARS in the CARINA NEBULA IDENTIFIED VIA INFRARED SPECTRAL ENERGY DISTRIBUTIONS Matthew S
For Publication in the Chandra Carina Complex Project Special Issue of the Astrophysical Journal Supplement Series Preprint typeset using LATEX style emulateapj v. 8/13/10 CANDIDATE X-RAY-EMITTING OB STARS IN THE CARINA NEBULA IDENTIFIED VIA INFRARED SPECTRAL ENERGY DISTRIBUTIONS Matthew S. Povich,1,2 Leisa K. Townsley,1 Patrick S. Broos,1 Marc Gagne,´ 3 Brian L. Babler,4 Remy´ Indebetouw,5 Steven R. Majewski,5 Marilyn R. Meade,4 Konstantin V. Getman,1 Thomas P. Robitaille,6,7 & Richard H. D. Townsend4 For Publication in the Chandra Carina Complex Project Special Issue of the Astrophysical Journal Supplement Series ABSTRACT We report the results of a new survey of massive, OB stars throughout the Carina Nebula using the X-ray point source catalog provided by the Chandra Carina Complex Project (CCCP) in conjunction with infrared (IR) photometry from the Two Micron All-Sky Survey and the Spitzer Space Telescope Vela–Carina survey. Mid-IR photometry is relatively unaffected by extinction, hence it provides strong constraints on the luminosities of OB stars, assuming that their association with the Carina Nebula, and hence their distance, is confirmed. We fit model stellar atmospheres to the optical (UBV)and IR spectral energy distributions (SEDs) of 182 OB stars with known spectral types and measure the bolometric luminosity and extinction for each star. We find that the extinction law measured toward the OB stars has two components: AV = 1–1.5 mag produced by foreground dust with a ratio of total-to-selective absorption RV =3.1 plus a contribution from local dust with RV > 4.0inthe Carina molecular clouds that increases as AV increases.