Institute of Space Sciences Annual Report 2016

Total Page:16

File Type:pdf, Size:1020Kb

Institute of Space Sciences Annual Report 2016 Institute of Space Sciences Annual Report 2016 An institute of the Consejo Superior de Investigaciones Cient´ıficas(CSIC). Affiliated with the Institut d'Estudis Espacials de Catalunya (IEEC). Contents 1 About us 5 1.1 What is the Institute of Space Sciences?...................................5 1.2 New Director..................................................5 1.3 New Manager..................................................6 1.4 Internal structure and governance of the Institute..............................6 1.5 International Advisory Committee......................................7 1.6 Development of protocols for internal operations..............................7 2 Personnel 9 2.1 List of personnel................................................9 2.2 Visitors..................................................... 10 2.3 Personnel summary............................................... 12 3 Scientific Summary 13 3.1 Department of Astrophysics and Planetary Sciences............................ 13 3.2 Department of Cosmology and Fundamental Physics............................ 14 3.3 Advanced Engineering Unit.......................................... 15 4 Some research highlights of this year 17 5 Missions and experiments 21 6 Publications summary 39 7 Publications Impact 41 8 Active projects in 2016 43 9 Appendix: Publication List 45 10 Other institutional activities 69 10.1 Ongoing & Completed Masters and Doctoral thesis............................. 69 10.2 Teaching & the Masters of Astrophysics and Cosmology.......................... 71 10.3 Outreach activities............................................... 72 10.4 Sant Cugat Forum on Astrophysics..................................... 73 10.5 Seminars Summary............................................... 73 10.6 Awards to our personnel............................................ 73 11 Competitive Funding Summary 75 12 Appendix: Seminars List 77 13 Appendix New projects in 2016 79 14 Appendix Active projects in 2016 81 3 Institute of Space Sciences 4 Chapter 1 About us 1.1 What is the Institute of Space Sciences? The Institute of Space Sciences pertains to the "Consejo Superior de Investigaciones Cient´ıficas”(the Spanish National Research Council, usually called CSIC). CSIC is the largest public institution dedicated to research in Spain and the third largest in Europe, and is formally depending on the Spanish Ministry of Economy and Competitiveness through the Secretary of State for Research, De- velopment and Innovation. Its main objective is to develop and promote research that will help bring about scientific and technological progress. Its institutes drive CSIC's research (about 120 in total, in all areas of sciences), which are spread across all the autonomous regions, and its more than 15000 staff, of whom more than 3000 are staff researchers and more than 3000 are doctors. CSIC has about 6% of all the staff dedicated to Research and Development in Spain, and they generate approximately 20% of all scientific production in the country. The Institute of Space Sciences is a new breed of research centers. It was officially created on January 17, 2008 (BOE #15, 3507, Orden ECI/4063/2007, of December 27, 2007), based on a proposal made about a decade before by the Governance of CSIC (Acta#11,11/99). The Institute of Space Sciences articulates the CSIC participation in the confederation of independent institutes affiliated with the "Institut d'Estudis Espacials de Catalunya" (IEEC). This is a non-for-profit foundation, founded inFebruary 1996, whose Board of Trustees includes, in addition to the CSIC, the Generalitat de Catalunya, the Univer- sitat de Barcelona (UB), the Universitat Aut`onomade Barcelona (UAB) and the Universitat Polit`ecnicade Catalunya (UPC). Our Institute thus benefits from the interaction and collaboration with both the larger CSIC structure and the Catalan community and government. The Director of the Institute of Space Sciences is at once, co-Director of IEEC Foundation. The association of the Institute of Space Sciences with both CSIC and IEEC is reflected in our acronym (IEEC-CSIC). In 2015, the Institute of Space Sciences (IEEC-CSIC) moved to a new facility located at the campus of the Uni- versitat Aut`onomade Barcelona. This building (property of CSIC and built on purpose for our Institute) has 3500 square meters of useful space, distributed in laboratories and offices. 1.2 New Director Founding Director Prof. Jordi Isern stepped down on February 2016 after years of service. Under his directorship the Institute was founded, and grew from just a handful researchers, scattered in different locations, to a strong group of staff and dozens of engineers and postdocs, all under the same roof. The impact of Prof. Isern in the development of the Institute has been enormous, and all staff is grateful for his efforts and leadership. From March 2016, Prof. Isern has been succeeded by ICREA Prof. Diego F. Torres. Prof. Torres was born in Buenos Aires, Argentina (1973) where he obtained a doctorate in physics (Cosmology and astrophysics of extended gravitational theories) by the National University of La Plata. He is a member of the Institute since 2006, when he arrived after several years of research at Princeton University and the Lawrence Livermore Laboratory, among others institutions, and became Director after being Head of its Department of Astrophysics and Planetary Sciences. His research focuses on compact objects and galactic cosmic rays, pulsars, its nebulae, and the origin of cosmic rays. Diego Torres' research has been awarded the Shakti Duggal Prize in Physics Cosmic Rays of the International 5 Institute of Space Sciences 6 Union of Physics, the Guggenheim Fellowship, the Wilhelm Friedrich Bessel Award from the Alexander von Humboldt Foundation, and the Sr. Visiting Professorship of the Academy of Sciences of China, among other distinctions. 1.3 New Manager Former Manager Isabel Molt`ostepped down on September 2016, after years of service. She was essential for the Institute's transition from a newborn child back in 2000 to the large research infrastructure that it is today. All staff is grateful for his efforts and help and for the countless hours of work beyond the call of her duty. From November 2016, Ms. Angels Benet has succeeded Ms. Molt`o.Ms. Benet comes to our Institute after being Deputy Manager at the Institute of Materials Sciences in Barcelona, also a CSIC Institute. 1.4 Internal structure and governance of the Institute The organization chart of the Institute is shown in the Figure below. The Director's Office is chaired by the ICE Director, and composed by the Deputy Director and the Manager of the Institute. The Assistant to the Director supports the functioning of this office. The Institute Board is composed and functions following CSIC regulations. The Institute has two Departments and one Technical Unit. These 3 bodies are: • APS: Department of Astrophysics and Planetary Sciences • CFP: Department of Cosmology and Fundamental Physics • AEU: Advanced Engineering Unit Each of these bodies (simply called Departments) have a Head. Research groups are part of these departments. According to the Institute's tradition and the approved internal regulations, all members with contracts of an initial duration of 5 years or more are considered senior Institute's members. All committees in the organization chart are executive. They are there to 'act' according to their guidelines, and to implement instructions given by their immediate upper level in the organization. Heads of Department (Committee members) are expected to be in office for a period of 4 (2) years. Our White Book for the institute's operations (available to all members, and produced in 2016) detail functioning roles, working guidelines, membership, responsibilities, procedures to implement recurrent actions, typical meetings cadence for each body, typical timescales to respond to predictable requests, etc. It also details our decision-making protocol as well as others for outreach activities, workspace allocation, teaching activities, laboratories operation, etc. The executive team is currently (3/2016-3/2020) formed by • Director: Diego F. Torres • Deputy Director: Ignasi Ribas Institute of Space Sciences 7 • Head of the Astrophysics and Planetary Science Department (APS): Josep Miquel Girart • Head of the Cosmology and Fundamental Physics Department (CFP): Enrique Gazta~naga • Head of the Advanced Engineering Unit (AEU): Josep Colom´e • Administrative Manager: Angels Benet • Assistant to the Director: Noem´ıCort´es The Institute Board is composed by the Director, Deputy Director, Manager and Heads of Department plus two working-force representatives and functions following CSIC regulations. In the period in the period 4/2016-4/2018, these representatives are Cristina Manuel y Josep M. Trigo. Current members of the commissions (4/2016-4/2018) are as follows: • Computing: Pablo Fosalba (chair) + Mart´ınCrocce + Josep Sanz • Workspace: Francisco Castander (chair) + Manager • Outreach: Laura Tol´os(chair) + Emma de O~na+ Ricard Casas • ICE Life: Nanda Rea (chair) + Carlos F. Sopuerta + V´ıctorMat´ın • Teaching: Aldo Serenelli (chair) + Margarita Hernanz + Llu´ısGesa 1.5 International Advisory Committee The International Advisory Committee of the Institute of Space Sciences has been formed in 2016 , and is currently (2016-2020) composed by • Karsten Danzmann, Max Planck Institute for Gravitational Physics, Hannover, Director. Expert on Gravita- tional Waves physics, is Director of the Division of Laser
Recommended publications
  • The TESS Light Curve of AI Phoenicis
    MNRAS 000,1{14 (2020) Preprint 9 June 2020 Compiled using MNRAS LATEX style file v3.0 The TESS light curve of AI Phoenicis P. F. L. Maxted,1? Patrick Gaulme,2? D. Graczyk,3? K. G. He lminiak,3? C. Johnston,4? Jerome A. Orosz,5? Andrej Prˇsa,6? John Southworth,1? Guillermo Torres,7? Guy R Davies,8;9? Warrick Ball,8;9 and William J Chaplin8;9 1Astrophysics group, Keele University, Keele, Staordshire, ST5 5BG, UK. 2Max-Planck-Institut fur¨ Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077, G¨ottingen, Germany. 3Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, ul. Rabia´nska 8, 87-100 Toru´n, Poland. 4Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, B-3001 Leuven, Belgium. 5Astronomy Department, San Diego State University, 5500 Campanile Drive, San Diego, CA 92182-1221, USA. 6Villanova University, Dept. of Astrophysics and Planetary Science, 800 Lancaster Avenue, Villanova PA 19085, USA. 7Center for Astrophysics, Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA. 8School of Physics and Astronomy, University of Birmingham, Birmingham, B15 2TT, UK. 9Stellar Astrophysics Centre (SAC), Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. Accepted XXX. Received YYY; in original form ZZZ ABSTRACT Accurate masses and radii for normal stars derived from observations of detached eclipsing binary stars are of fundamental importance for testing stellar models and may be useful for calibrating free parameters in these model if the masses and radii are sufficiently precise and accurate. We aim to measure precise masses and radii for the stars in the bright eclipsing binary AI Phe, and to quantify the level of system- atic error in these estimates.
    [Show full text]
  • Grant Proposals, 1991-1999
    Grant Proposals, 1991-1999 Finding aid prepared by Smithsonian Institution Archives Smithsonian Institution Archives Washington, D.C. Contact us at [email protected] Table of Contents Collection Overview ........................................................................................................ 1 Administrative Information .............................................................................................. 1 Descriptive Entry.............................................................................................................. 1 Names and Subjects ...................................................................................................... 1 Container Listing ............................................................................................................. 2 Grant Proposals https://siarchives.si.edu/collections/siris_arc_251859 Collection Overview Repository: Smithsonian Institution Archives, Washington, D.C., [email protected] Title: Grant Proposals Identifier: Accession 99-171 Date: 1991-1999 Extent: 17 cu. ft. (17 record storage boxes) Creator:: Smithsonian Astrophysical Observatory. Contracts and Procurement Office Language: English Administrative Information Prefered Citation Smithsonian Institution Archives, Accession 99-171, Smithsonian Astrophysical Observatory, Contracts and Procurement Office, Grant Proposals Descriptive Entry This accession consists of records documenting Smithsonian Astrophysical Observatory projects and activities. Materials include proposals, correspondence, progress
    [Show full text]
  • 121012-AAS-221 Program-14-ALL, Page 253 @ Preflight
    221ST MEETING OF THE AMERICAN ASTRONOMICAL SOCIETY 6-10 January 2013 LONG BEACH, CALIFORNIA Scientific sessions will be held at the: Long Beach Convention Center 300 E. Ocean Blvd. COUNCIL.......................... 2 Long Beach, CA 90802 AAS Paper Sorters EXHIBITORS..................... 4 Aubra Anthony ATTENDEE Alan Boss SERVICES.......................... 9 Blaise Canzian Joanna Corby SCHEDULE.....................12 Rupert Croft Shantanu Desai SATURDAY.....................28 Rick Fienberg Bernhard Fleck SUNDAY..........................30 Erika Grundstrom Nimish P. Hathi MONDAY........................37 Ann Hornschemeier Suzanne H. Jacoby TUESDAY........................98 Bethany Johns Sebastien Lepine WEDNESDAY.............. 158 Katharina Lodders Kevin Marvel THURSDAY.................. 213 Karen Masters Bryan Miller AUTHOR INDEX ........ 245 Nancy Morrison Judit Ries Michael Rutkowski Allyn Smith Joe Tenn Session Numbering Key 100’s Monday 200’s Tuesday 300’s Wednesday 400’s Thursday Sessions are numbered in the Program Book by day and time. Changes after 27 November 2012 are included only in the online program materials. 1 AAS Officers & Councilors Officers Councilors President (2012-2014) (2009-2012) David J. Helfand Quest Univ. Canada Edward F. Guinan Villanova Univ. [email protected] [email protected] PAST President (2012-2013) Patricia Knezek NOAO/WIYN Observatory Debra Elmegreen Vassar College [email protected] [email protected] Robert Mathieu Univ. of Wisconsin Vice President (2009-2015) [email protected] Paula Szkody University of Washington [email protected] (2011-2014) Bruce Balick Univ. of Washington Vice-President (2010-2013) [email protected] Nicholas B. Suntzeff Texas A&M Univ. suntzeff@aas.org Eileen D. Friel Boston Univ. [email protected] Vice President (2011-2014) Edward B. Churchwell Univ. of Wisconsin Angela Speck Univ. of Missouri [email protected] [email protected] Treasurer (2011-2014) (2012-2015) Hervey (Peter) Stockman STScI Nancy S.
    [Show full text]
  • The Cataclysmic Variable AE Aquarii: Orbital Variability in V Band
    The cataclysmic variable AE Aquarii: orbital variability in V band R. Zamanov & G. Latev Institute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences, Tsarigradsko Shose 72, BG-1784 Sofia, Bulgaria [email protected] [email protected] (Submitted on 28.11.2016. Accepted on 31.01.2017) Abstract. We present 62.7 hours observations of the cataclysmic variable AE Aqr in Johnson V band. These are non-published archive electro-photometric data obtained during the time period 1993 to 1999. We construct the orbital variability in V band and obtain a Fourier fit to the double-wave quiescent light curve. The strongest flares in our data set are in phase interval 0.6 - 0.8. The data can be downloaded from http://www.astro.bas.bg/∼rz/DATA/AEAqr.elphot.dat. Key words: Stars: novae, cataclysmic variables – Accretion, accretion disks – white dwarfs – Stars: individual: AE Aqr 1 Introduction AE Aqr is a bright intermediate polar cataclysmic variable (V ≈ 11−12.3). In this semi-detached binary system a spotted K type dwarf (K0-K4 IV/V star) transfers material through the inner Lagrangian point L1 toward a magnetic white dwarf (Skidmore et al. 2003, Hill et al. 2016). It has a relatively long orbital period of 9.88 hours (Robinson et al. 1991; Echevarr´ıa et al. 2008) and an extremely short rotational period of the white dwarf of only 33 s (Patterson et al. 1980). To appear in such a state, AE Aqr should be a former supersoft X-ray binary, in which the mass transfer rate in the recent past (≈ 107 yr) has been much higher than its current value (Schenker et al.
    [Show full text]
  • Msc-Whipple Analysis 2010
    TWO DIMENSIONAL ANALYSIS OF INCOMPLETE PARAMETERISED ARCHIVAL DATA FROM THE WHIPPLE 10 METRE IMAGING ATMOSPHERIC CHERENKOV TELESCOPE CENTERED ON AE AQUARII by Michael Connolly H.Dip., B.D., B.Ph., B.Sc. A dissertation submitted to the Centre for Astronomy, School of Physics, National University of Ireland, Galway in fulfilment of the requirements for the degree of Master of Science Supervisor Dr Mark Lang February 2010 Galway, Ireland MSc-Whipple Analysis 2010 Dedicated to the memory of Martin Connolly (1940-1985) Hard work and belief can accomplish, With God’s help 1. Michael Connolly Page 2 MSc-Whipple Analysis 2010 1. Michael Connolly Page 3 MSc-Whipple Analysis 2010 Contents List of Figures. 8 List of Tables. 12 Acknowledgements. 12 Abstract. 14 Chapter 1: Introduction to Thesis 1.1 Introduction. 16 1.2 Thesis Overview. 17 1.3 Personal Contribution. 18 Chapter 2: Very High Energy Gamma-Ray Astronomy 2.1 Introduction. 20 2.2 Gamma ray production in the Earth’s atmosphere. 23 2.3 Extensive Air Showers. 23 2.3.1 Pair Production. 24 2.3.2 Electron-photon cascades or electromagnetic showers. 25 2.4 Extensive air showers from two different progenitors. 26 2.4.1 Properties of gamma ray induced showers. 26 2.4.2 Properties of cosmic ray induced showers. 27 2.5 What is Cherenkov light? . 28 1. Michael Connolly Page 4 MSc-Whipple Analysis 2010 2.6 Relative incidence of high energy electromagnetic photons . 31 2.7 History. 33 2.8 VHE gamma ray sources and production. 38 2.8.1 Physical processes involved in gamma ray production.
    [Show full text]
  • Search for Gamma-Ray Emission from AE Aquarii with Seven Years of FERMI-LAT Observations
    Search for gamma-ray emission from AE Aquarii with seven years of FERMI-LAT observations Jian Li1, Diego F. Torres1,2, Nanda Rea1,3, Emma de O˜na Wilhelmi1, Alessandro Papitto4, Xian Hou5, & Christopher W. Mauche6 ABSTRACT AE Aquarii (AE Aqr) is a cataclysmic binary hosting one of the fastest rotating (Pspin = 33.08 s) white dwarfs known. Based on seven years of Fermi Large Area Tele- scope (LAT) Pass 8 data, we report on a deep search for gamma-ray emission from æ. Using X-ray observations from ASCA, XMM-Newton, Chandra, Swift, Suzaku, and NuSTAR, spanning 20 years, we substantially extend and improve the spin ephemeris of æ. Using this ephemeris, we searched for gamma-ray pulsations at the spin period of the white dwarf. No gamma-ray pulsations were detected above 3 σ significance. Neither phase-averaged gamma-ray emission nor gamma-ray variability of æ is de- tected by Fermi-LAT. We impose the most restrictive upper limit to the gamma-ray flux from æ to date: 1.3 × 10−12 erg cm−2 s−1 in the 100 MeV–300 GeV energy range, providing constraints on models. Subject headings: gamma rays: stars — cataclysmic binary: individual: æ 1. Introduction Cataclysmic variables (CVs) are semi-detached binaries consisting of a white dwarf (WD) and a companion star, usually a red dwarf. æ is a bright (V≈11, Welsh et al. 1999) CV hosting one of the fastest rotating WDs known (Pspin = 33.08 s, Patterson 1979) and a K 4-5 V secondary; it is arXiv:1608.06662v1 [astro-ph.HE] 23 Aug 2016 1Institute of Space Sciences (IEEC-CSIC), Campus UAB, Carrer de Magrans s/n, 08193 Barcelona, Spain 2Instituci´oCatalana de Recerca i Estudis Avanc¸ats (ICREA), E-08010 Barcelona, Spain 3Anton Pannekoek Institute, University of Amsterdam, Postbus 94249, NL-1090-GE Amsterdam, The Netherlands 4INAF-Osservatorio Astronomico di Roma, via di Frascati 33, I-00040 Monte Porzio Catone, Roma, Italy 5Key Laboratory for the Structure and Evolution of Celestial Objects, Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, China.
    [Show full text]
  • Arxiv:2006.10868V2 [Astro-Ph.SR] 9 Apr 2021 Spain and Institut D’Estudis Espacials De Catalunya (IEEC), C/Gran Capit`A2-4, E-08034 2 Serenelli, Weiss, Aerts Et Al
    Noname manuscript No. (will be inserted by the editor) Weighing stars from birth to death: mass determination methods across the HRD Aldo Serenelli · Achim Weiss · Conny Aerts · George C. Angelou · David Baroch · Nate Bastian · Paul G. Beck · Maria Bergemann · Joachim M. Bestenlehner · Ian Czekala · Nancy Elias-Rosa · Ana Escorza · Vincent Van Eylen · Diane K. Feuillet · Davide Gandolfi · Mark Gieles · L´eoGirardi · Yveline Lebreton · Nicolas Lodieu · Marie Martig · Marcelo M. Miller Bertolami · Joey S.G. Mombarg · Juan Carlos Morales · Andr´esMoya · Benard Nsamba · KreˇsimirPavlovski · May G. Pedersen · Ignasi Ribas · Fabian R.N. Schneider · Victor Silva Aguirre · Keivan G. Stassun · Eline Tolstoy · Pier-Emmanuel Tremblay · Konstanze Zwintz Received: date / Accepted: date A. Serenelli Institute of Space Sciences (ICE, CSIC), Carrer de Can Magrans S/N, Bellaterra, E- 08193, Spain and Institut d'Estudis Espacials de Catalunya (IEEC), Carrer Gran Capita 2, Barcelona, E-08034, Spain E-mail: [email protected] A. Weiss Max Planck Institute for Astrophysics, Karl Schwarzschild Str. 1, Garching bei M¨unchen, D-85741, Germany C. Aerts Institute of Astronomy, Department of Physics & Astronomy, KU Leuven, Celestijnenlaan 200 D, 3001 Leuven, Belgium and Department of Astrophysics, IMAPP, Radboud University Nijmegen, Heyendaalseweg 135, 6525 AJ Nijmegen, the Netherlands G.C. Angelou Max Planck Institute for Astrophysics, Karl Schwarzschild Str. 1, Garching bei M¨unchen, D-85741, Germany D. Baroch J. C. Morales I. Ribas Institute of· Space Sciences· (ICE, CSIC), Carrer de Can Magrans S/N, Bellaterra, E-08193, arXiv:2006.10868v2 [astro-ph.SR] 9 Apr 2021 Spain and Institut d'Estudis Espacials de Catalunya (IEEC), C/Gran Capit`a2-4, E-08034 2 Serenelli, Weiss, Aerts et al.
    [Show full text]
  • On the Mass Transfer in AE Aquarii
    A&A 421, 1131–1142 (2004) Astronomy DOI: 10.1051/0004-6361:20040319 & c ESO 2004 Astrophysics On the mass transfer in AE Aquarii N. R. Ikhsanov1,3,4,V.V.Neustroev2,5, and N. G. Beskrovnaya3,4 1 Korea Astronomy Observatory, 61-1 Whaam-dong, Yusong-gu, Taejon 305-348, Republic of Korea 2 Computational Astrophysics Laboratory, National University of Ireland, Galway, Newcastle Rd., Galway, Ireland 3 Central Astronomical Observatory of the Russian Academy of Sciences, Pulkovo 65/1, 196140 St. Petersburg, Russia 4 Isaac Newton Institute of Chile, St. Petersburg Branch, Russia 5 Isaac Newton Institute of Chile, Kazan Branch, Russia Received 24 February 2004 / Accepted 30 March 2004 Abstract. The observed properties of the close binary AE Aqr indicate that the mass transfer in this system operates via the Roche lobe overflow mechanism, but the material transferred from the normal companion is neither accreted onto the surface of the white dwarf nor stored in a disk around its magnetosphere. As previously shown, such a situation can be realized if the white dwarf operates as a propeller. At the same time, the efficiency of the propeller action by the white dwarf is insufficient to explain the rapid braking of the white dwarf, which implies that the spin-down power is in excess of the bolometric luminosity of the system. To avoid this problem we have simulated the mass-transfer process in AE Aqr assuming that the observed braking of the white dwarf is governed by a pulsar-like spin-down mechanism. We show that the expected Hα Doppler tomogram in this case resembles the tomogram observed from the system.
    [Show full text]
  • Save Pdf (0.09
    THE SOLAR-TYPE ECLIPSING BINARY SYSTEM AI PHOENICIS E.F. Milone and B.J. Hrivnak Rothney Astrophysical Observatory, The Univ. of Calgary INTRODUCTION AI Phe was discovered to be variable and identified as an EA binary by Strohmeier (1972). Reipurth (1978) subsequently carried out uvby photometry, determined the period (24.5923 d), and noted the lengthy totality of primary minimum and the displacement of the second­ ary minimum. Imbert (1978) obtained radial velocity curves and deter­ mined spectroscopic orbital elements. Imbert also gives a spectroscopic classification of G2V for the primary (hotter) component and approxi­ mately G5 for the secondary. AI Phe thus appeared to offer a unique opportunity to study the limb darkening of a non-interacting solar-type star. As an extension of a solar UV limb darkening study (Kjeldseth Moe and Milone 1978), ten IUE spectra were obtained on Aug. 12 in 2 successive shifts (cf Milone et al 1981). In conjunct-ion with this, ground-based 5-colour photometry and spectroscopy were carried out at CTIO and at UTLCO. PRESENT WORK UBVRI photometry was carried out in September 1981 by Hrivnak at CTIO, and over the season, by I. Sheldon at Las Campanas. Figure 1 displays the differential V light curve relative to comparison star HD 6236. Standardization to the Johnson system permitted the deter­ mination of magnitude and colours of the two components, since the secondary is seen alone at primary minimum. star V U - V B - V V - R V - I S 9.326 1.35 0.85 0.70 1.15 P 9.335 0.47 0.49 0.47 0.70 Spectra taken iri eclipse beginning at phase 0P.0048 reveal a composite spectral type of about G5.
    [Show full text]
  • The Iso Handbook
    THE ISO HANDBOOK Volume I: ISO – Mission & Satellite Overview Martin F. Kessler1,2, Thomas G. M¨uller1,4, Kieron Leech 1, Christophe Arviset1, Pedro Garc´ıa-Lario1, Leo Metcalfe1, Andy M. T. Pollock1,3, Timo Prusti1,2 and Alberto Salama1 SAI-2000-035/Dc, Version 2.0 November, 2003 1 ISO Data Centre, Science Operations and Data Systems Division Research and Scientific Support Department of ESA, Villafranca del Castillo, P.O. Box 50727, E-28080 Madrid, Spain 2 ESTEC, Science Operations and Data Systems Division Research and Scientific Support Department of ESA, Keplerlaan 1, Postbus 299, 2200 AG Noordwijk, The Netherlands 3 Computer & Scientific Co. Ltd., 230 Graham Road, Sheffield S10 3GS, England 4 Max-Planck-Institut f¨ur extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany ii Document Information Document: The ISO Handbook Volume: I Title: ISO - Mission & Satellite Overview Reference Number: SAI/2000-035/Dc Issue: Version 2.0 Issue Date: November 2003 Authors: M.F. Kessler, T. M¨uller, K. Leech et al. Editors: T. M¨uller, J. Blommaert & P. Garc´ıa-Lario Web-Editor: J. Matagne Document History The ISO Handbook, Volume I: ISO – Mission & Satellite Overview is mainly based on the following documents: • The ISO Handbook, Volume I: ISO – Mission Overview, Kessler M.F., M¨uller T.G., Arviset C. et al., earlier versions, SAI-2000-035/Dc. • The ISO Handbook, Volume II: ISO – The Satellite and its Data, K. Leech & A.M.T. Pollock, earlier versions, SAI-99-082/Dc. • The following ESA Bulletin articles: The ISO Mission – A Scientific Overview, M.F. Kessler, A.
    [Show full text]
  • University of Birmingham the TESS Light Curve of AI Phoenicis
    University of Birmingham The TESS light curve of AI Phoenicis Maxted, P. F. L.; Gaulme, Patrick; Graczyk, D.; Heminiak, K. G.; Johnston, C.; Orosz, Jerome A.; Prša, Andrej; Southworth, John; Torres, Guillermo; Davies, Guy R.; Ball, Warrick; Chaplin, William J DOI: 10.1093/mnras/staa1662 License: None: All rights reserved Document Version Publisher's PDF, also known as Version of record Citation for published version (Harvard): Maxted, PFL, Gaulme, P, Graczyk, D, Heminiak, KG, Johnston, C, Orosz, JA, Prša, A, Southworth, J, Torres, G, Davies, GR, Ball, W & Chaplin, WJ 2020, 'The TESS light curve of AI Phoenicis', Monthly Notices of the Royal Astronomical Society, vol. 498, no. 1, pp. 332–343. https://doi.org/10.1093/mnras/staa1662 Link to publication on Research at Birmingham portal Publisher Rights Statement: This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2020 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. General rights Unless a licence is specified above, all rights (including copyright and moral rights) in this document are retained by the authors and/or the copyright holders. The express permission of the copyright holder must be obtained for any use of this material other than for purposes permitted by law. •Users may freely distribute the URL that is used to identify this publication. •Users may download and/or print one copy of the publication from the University of Birmingham research portal for the purpose of private study or non-commercial research. •User may use extracts from the document in line with the concept of ‘fair dealing’ under the Copyright, Designs and Patents Act 1988 (?) •Users may not further distribute the material nor use it for the purposes of commercial gain.
    [Show full text]
  • Magnetic Pumping in the Cataclysmic Variable AE Aquarii
    FKuijpers, J.M.E., Fletcher, L., Abada-Simon, M, Horne, K.D., Raadu, M.A., Ramsay, G., and Steeghs, D. (1997) Magnetic pumping in the cataclysmic variable AE Aquarii. Astronomy and Astrophysics, 322 . pp. 242-255. ISSN 0004-6361 Copyright © 1997 EDP Sciences. A copy can be downloaded for personal non-commercial research or study, without prior permission or charge The content must not be changed in any way or reproduced in any format or medium without the formal permission of the copyright holder(s) When referring to this work, full bibliographic details must be given http://eprints.gla.ac.uk/91461/ Deposited on: 28 February 2014 Enlighten – Research publications by members of the University of Glasgow http://eprints.gla.ac.uk Astron. Astrophys. 322, 242–255 (1997) ASTRONOMY AND ASTROPHYSICS Magnetic pumping in the cataclysmic variable AE Aquarii J. Kuijpers1,2,3, L. Fletcher?1,2, M. Abada-Simon1,2, K.D. Horne4, M.A. Raadu5, G.Ramsay1,2, and D. Steeghs1,2,4 1 Sterrekundig Instituut, Universiteit Utrecht, Postbus 80 000, 3508 TA Utrecht, The Netherlands 2 CHEAF (Centrum voor Hoge Energie Astrofysica), Postbus 41882, 1009 DB Amsterdam 3 Dep. of Experimental High Energy Physics, University of Nijmegen, Toernooiveld 1, 6525 ED Nijmegen 4 School of Physics and Astronomy, The University, St. Andrews, Fife KY16 9SS, Scotland, UK 5 Division of Plasma Physics, Alfven´ Laboratory, The Royal Institute of Technology, S-10044 Stockholm, Sweden Received 10 June 1996 / Accepted 12 November 1996 Abstract. We propose that the radio outbursts of the cata- Table 1. Some of the most important system parameters of AE Aqr clysmic variable AE Aqr are caused by eruptions of bubbles (most of which are taken from Welsh et al.
    [Show full text]