Publications 2019
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Contributions of the Astronomical Observatory Skalnate´ Pleso
ASTRONOMICAL INSTITUTE SLOVAK ACADEMY OF SCIENCES CONTRIBUTIONS OF THE ASTRONOMICAL OBSERVATORY SKALNATE´ PLESO • VOLUME L • Number 3 S KA SO LNATÉ PLE July 2020 Editorial Board Editor-in-Chief August´ın Skopal, Tatransk´aLomnica, The Slovak Republic Managing Editor Richard Komˇz´ık, Tatransk´aLomnica, The Slovak Republic Editors Drahom´ır Chochol, Tatransk´aLomnica, The Slovak Republic J´ulius Koza, Tatransk´aLomnica, The Slovak Republic AleˇsKuˇcera, Tatransk´aLomnica, The Slovak Republic LuboˇsNesluˇsan, Tatransk´aLomnica, The Slovak Republic Vladim´ır Porubˇcan, Bratislava, The Slovak Republic Theodor Pribulla, Tatransk´aLomnica, The Slovak Republic Advisory Board Bernhard Fleck, Greenbelt, USA Arnold Hanslmeier, Graz, Austria Marian Karlick´y, Ondˇrejov, The Czech Republic Tanya Ryabchikova, Moscow, Russia Giovanni B. Valsecchi, Rome, Italy Jan Vondr´ak, Prague, The Czech Republic c Astronomical Institute of the Slovak Academy of Sciences 2020 ISSN: 1336–0337 (on-line version) CODEN: CAOPF8 Editorial Office: Astronomical Institute of the Slovak Academy of Sciences SK - 059 60 Tatransk´aLomnica, The Slovak Republic CONTENTS EDITORIAL A. Skopal, R. Komˇz´ık: Editorial . 647 STARS T. Pribulla, L’. Hamb´alek, E. Guenther, R. Komˇz´ık, E. Kundra, J. Nedoroˇsˇc´ık, V. Perdelwitz, M. Vaˇnko: Close eclipsing binary BDAnd: a triple system . 649 V. Andreoli, U. Munari: LAMOST J202629.80+423652.0 is not a symbiotic star . 672 M.Yu. Skulskyy: Formation of magnetized spatial structures in the Beta Lyrae system. I. Observation as a research background -
The Search for Exomoons and the Characterization of Exoplanet Atmospheres
Corso di Laurea Specialistica in Astronomia e Astrofisica The search for exomoons and the characterization of exoplanet atmospheres Relatore interno : dott. Alessandro Melchiorri Relatore esterno : dott.ssa Giovanna Tinetti Candidato: Giammarco Campanella Anno Accademico 2008/2009 The search for exomoons and the characterization of exoplanet atmospheres Giammarco Campanella Dipartimento di Fisica Università degli studi di Roma “La Sapienza” Associate at Department of Physics & Astronomy University College London A thesis submitted for the MSc Degree in Astronomy and Astrophysics September 4th, 2009 Università degli Studi di Roma ―La Sapienza‖ Abstract THE SEARCH FOR EXOMOONS AND THE CHARACTERIZATION OF EXOPLANET ATMOSPHERES by Giammarco Campanella Since planets were first discovered outside our own Solar System in 1992 (around a pulsar) and in 1995 (around a main sequence star), extrasolar planet studies have become one of the most dynamic research fields in astronomy. Our knowledge of extrasolar planets has grown exponentially, from our understanding of their formation and evolution to the development of different methods to detect them. Now that more than 370 exoplanets have been discovered, focus has moved from finding planets to characterise these alien worlds. As well as detecting the atmospheres of these exoplanets, part of the characterisation process undoubtedly involves the search for extrasolar moons. The structure of the thesis is as follows. In Chapter 1 an historical background is provided and some general aspects about ongoing situation in the research field of extrasolar planets are shown. In Chapter 2, various detection techniques such as radial velocity, microlensing, astrometry, circumstellar disks, pulsar timing and magnetospheric emission are described. A special emphasis is given to the transit photometry technique and to the two already operational transit space missions, CoRoT and Kepler. -
Abstracts of Extreme Solar Systems 4 (Reykjavik, Iceland)
Abstracts of Extreme Solar Systems 4 (Reykjavik, Iceland) American Astronomical Society August, 2019 100 — New Discoveries scope (JWST), as well as other large ground-based and space-based telescopes coming online in the next 100.01 — Review of TESS’s First Year Survey and two decades. Future Plans The status of the TESS mission as it completes its first year of survey operations in July 2019 will bere- George Ricker1 viewed. The opportunities enabled by TESS’s unique 1 Kavli Institute, MIT (Cambridge, Massachusetts, United States) lunar-resonant orbit for an extended mission lasting more than a decade will also be presented. Successfully launched in April 2018, NASA’s Tran- siting Exoplanet Survey Satellite (TESS) is well on its way to discovering thousands of exoplanets in orbit 100.02 — The Gemini Planet Imager Exoplanet Sur- around the brightest stars in the sky. During its ini- vey: Giant Planet and Brown Dwarf Demographics tial two-year survey mission, TESS will monitor more from 10-100 AU than 200,000 bright stars in the solar neighborhood at Eric Nielsen1; Robert De Rosa1; Bruce Macintosh1; a two minute cadence for drops in brightness caused Jason Wang2; Jean-Baptiste Ruffio1; Eugene Chiang3; by planetary transits. This first-ever spaceborne all- Mark Marley4; Didier Saumon5; Dmitry Savransky6; sky transit survey is identifying planets ranging in Daniel Fabrycky7; Quinn Konopacky8; Jennifer size from Earth-sized to gas giants, orbiting a wide Patience9; Vanessa Bailey10 variety of host stars, from cool M dwarfs to hot O/B 1 KIPAC, Stanford University (Stanford, California, United States) giants. 2 Jet Propulsion Laboratory, California Institute of Technology TESS stars are typically 30–100 times brighter than (Pasadena, California, United States) those surveyed by the Kepler satellite; thus, TESS 3 Astronomy, California Institute of Technology (Pasadena, Califor- planets are proving far easier to characterize with nia, United States) follow-up observations than those from prior mis- 4 Astronomy, U.C. -
Infrared Imaging with COAST
Infrared Imaging with COAST John Stephen Young St John’s College, Cambridge and Cavendish Astrophysics A dissertation submitted for the degree of Doctor of Philosophy in the University of Cambridge 26 March 1999 iii Preface This dissertation describes work carried out in the Astrophysics Group of the Department of Phys- ics, University of Cambridge, between October 1995 and March 1999. Except where explicit reference is made to the work of others, this dissertation is the result of my own work, and includes nothing which is the outcome of work done in collaboration. No part of this dissertation has been submitted for a degree, diploma, or other qualification at any University. This dissertation does not exceed 60,000 words in length. v Acknowledgements Many people say that this is the only page of a PhD. thesis worth reading. I hope that is not the case here. This is, however, the only page not written in the passive voice, and the only one which might make you smile. Above all, I would like to thank my supervisor, Professor John Baldwin, for always being available to give advice and encouragement, and for assisting with many hours of alignment and even more hours of observing. The shortbread was much appreciated! Many thanks are also due for his reading of this thesis. It has been a pleasure to work with all of the members of the COAST team. None of the work described in this thesis would have been possible without the NICMOS camera built by Martin Beckett. I would like to thank him for taking the time to explain it to me. -
Observational Studies of X-Ray Binary Systems Observational Studies of X-Ray Binary Systems
mmnML mmmm AWD DE» FIOWS INIS-mf—8690 "'•'..'..-. !' ..- -'. .^: C-^;/- V'-^ ^ ^'vV?*f,>4 "' :f ,.?;•• ..f..-XV., . '4*.> • OBSERVATIONAL STUDIES OF X-RAY BINARY SYSTEMS OBSERVATIONAL STUDIES OF X-RAY BINARY SYSTEMS PROPERTIES OF THE NEUTRON STAR AND ITS COMPANION ORBITAL MOTION AND MASS FLOWS ACADEMISCH PROEFSCHRIFT ter verkrijging van de graad van doctor in de Wiskunde en Natuurwetenschappen aan de Universiteit van Amsterdam, op gezag van de Rector Magnificus, Dr. D.W. Bresters, hoogleraar in de Faculteit der Wiskunde en Natuurwetenschappen, in het openbaar te verdedigen in de Aula der Universiteit (tijdelijk in de Lutherse Kerk, ingang Singel 411, hoek Spui) op woensdag 2 februari 1983 te 13:30 uur door Michiel Baidur Maximiliaan van der Klis geboren te 's Gravenhage PROMOTOR : Prof. Dr. E.P.J, van den Heuvel CO-REFERENT : Dr. Ir. J.A.H. Bieeker CONTENTS 0. Introduction and summary 7 1. Mass-Flux Induced Orbital-Period Changes In X-Ray Binaries 17 2. Cygnus X-3 2.1 A Change In Light Curve Asymmetry and the Ephemeris of Cygnus X-3 31 2.2 The X-Ray Modulation of Cygnus X-3 34 2.3 The Cycle-to-Cycle Variability of Cygnus X-3 40 3. Mass Transfer and Accretion in Centaurus X-3 and SMC X-l 3.1 The Accretion Picture of Cen X-3 as Inferred from One Month of Continuous X-Ray Observations 55 3.2 Long Term X-Ray Observations of SMC X-l Including a Turn-On 62 4. Pulsation and Orbital Parameters of Centaurus X-3 and Vela X-l 4.1 Characteristics of the Cen X-3 Neutron Star from Correlated Spin-Up and X-Ray Luminosity Measurements 69 4.2 The Orbital Parameters and the X-Ray Pulsation of Vela X-l (4U 0900-40) 76 5. -
Exoplanets Finding Extrasolar Planets
Exoplanets Finding Extrasolar Planets. I Direct Searches Direct searches are difficult because stars are so bright. How Bright are Planets? Planets shine by reflected light. The amount reflected is the amount received (the solar constant) - times the area of the planet - times the albedo (fraction reflected) L = L /4πd2 x albedo x πR 2 ~ L (R /d)2 p * p * p 2 8 For the Earth, (Rp/d) ~5 x 10 2 8 For Jupiter, (Rp/d) ~10 How Bright are Planets? You gain by going to long wavelengths The Rayleigh-Jeans Tail 7 • λmax = 2.897x 10 /T Å/K 4 • For λmax >> λmax, Iλ~ A 2ckBT/λ – A: area – IJ ~ 0.002 I¤ How Far are Planets from Stars? 1 au = 1“ at 1 pc (definition of the parsec) • 1 pc (parsec) = 3.26 light years • 1“ (arcsec) = 1/3600 degree As seen from α Centauri (4.3 ly): • Earth is 0.75 arcsec from Sol • Jupiter is 4 arcsec from Sol 2 3 2 4π a /P = G (M*+MP) 2 2 1/3 θ = (G P (M*+MP)/4π D) Aside: Telescope ResoluKon • The spaal profile of the intensity of light passing through an aperture is the Fourier Transform of that aperture. 2 2 • the intensity of the light, as a funcKon of the off-axis distance θ from a slit is I = I0 sin (u)/u – u = π D sin(θ)/λ, – D is the diameter of the aperture – λ is the wavelength of the light. • I peaks at θ=0, and has nulls at sin(θ)=n λ/D, for all n not equal to 0. -
A New24 Mu M Phase Curve for Upsilon Andromedae B
University of Central Florida STARS Faculty Bibliography 2010s Faculty Bibliography 1-1-2010 A New24 Mu M Phase Curve for Upsilon Andromedae B Ian J. M. Crossfield Brad M. S. Hansen Joseph Harrington University of Central Florida James Y. -K. Cho Drake Deming See next page for additional authors Find similar works at: https://stars.library.ucf.edu/facultybib2010 University of Central Florida Libraries http://library.ucf.edu This Article is brought to you for free and open access by the Faculty Bibliography at STARS. It has been accepted for inclusion in Faculty Bibliography 2010s by an authorized administrator of STARS. For more information, please contact [email protected]. Recommended Citation Crossfield, Ian J. M.; Hansen, Brad M. S.; Harrington, Joseph; Cho, James Y. -K.; Deming, Drake; Menou, Kristen; and Seager, Sara, "A New24 Mu M Phase Curve for Upsilon Andromedae B" (2010). Faculty Bibliography 2010s. 71. https://stars.library.ucf.edu/facultybib2010/71 Authors Ian J. M. Crossfield, Brad M. S. Hansen, Joseph Harrington, James Y. -K. Cho, Drake Deming, Kristen Menou, and Sara Seager This article is available at STARS: https://stars.library.ucf.edu/facultybib2010/71 The Astrophysical Journal, 723:1436–1446, 2010 November 10 doi:10.1088/0004-637X/723/2/1436 C 2010. The American Astronomical Society. All rights reserved. Printed in the U.S.A. ANEW24μm PHASE CURVE FOR υ ANDROMEDAE b Ian J. M. Crossfield1, Brad M. S. Hansen1,2, Joseph Harrington3, James Y.-K. Cho4, Drake Deming5, Kristen Menou6, and Sara Seager7 1 Department of Physics and -
Other Planetary Systems the New Science of Distant Worlds
BENN6189_05_C13_PR5_V3_TT.QXD 10/31/07 8:03 AM Page 394 13 Other Planetary Systems The New Science of Distant Worlds LEARNING GOALS 13.1 Detecting Extrasolar Planets 13.3 The Formation of Other Solar Systems ◗ Why is it so difficult to detect planets around other stars? ◗ Can we explain the surprising orbits of many extrasolar ◗ How do we detect planets around other stars? planets? ◗ Do we need to modify our theory of solar system 13.2 The Nature of Extrasolar Planets formation? ◗ What have we learned about extrasolar planets? ◗ How do extrasolar planets compare with planets in our 13.4 Finding More New Worlds solar system? ◗ How will we search for Earth-like planets? 394 BENN6189_05_C13_PR5_V3_TT.QXD 10/31/07 8:03 AM Page 395 How vast those Orbs must be, and how inconsiderable Before we begin, it’s worth noting that these discoveries this Earth, the Theatre upon which all our mighty have further complicated the question of precisely how we Designs, all our Navigations, and all our Wars are define a planet. Recall that the 2005 discovery of the Pluto- transacted, is when compared to them. A very fit like world Eris [Section 12.3] forced astronomers to recon- consideration, and matter of Reflection, for those sider the minimum size of a planet, and the International Kings and Princes who sacrifice the Lives of so many Astronomical Union (IAU) now defines Pluto and Eris as People, only to flatter their Ambition in being Masters dwarf planets. In much the same way that Pluto and Eris of some pitiful corner of this small Spot. -
Isaac Newton Institute of Chile in Eastern Europe and Eurasia Casilla 8-9, Correo 9, Santiago, Chile E-Mail: [email protected] Web-Address
1 Isaac Newton Institute of Chile in Eastern Europe and Eurasia Casilla 8-9, Correo 9, Santiago, Chile e-Mail: [email protected] Web-address: www.ini.cl The Isaac Newton Institute, ͑INI͒ for astronomical re- law obtaining significantly different slopes, down to the last search was founded in 1978 by the undersigned. The main reliable magnitude bin, i.e. where completeness drops below office is located in the eastern outskirts of Santiago. Since 50%. The slope of the internal annulus is flatter than the 1992, it has expanded into several countries of the former outer indicating the presence of different mass distributions Soviet Union in Eastern Europe and Eurasia. at different radial distances. This is a clear mark of mass As of the year 2003 the Institute is composed of fifteen segregations, as expected in dinamically relaxed systems as Branches in nine countries. ͑see figure on following page͒. GCs; These are: Armenia ͑20͒, Bulgaria ͑26͒, Crimea ͑29͒, Kaza- 4.- In order to further clarify the situation, we applied two khstan ͑17͒, Kazan ͑12͒, Kiev ͑11͒, Moscow ͑22͒, Odessa different mass-luminosity relations from the models of Mon- ͑34͒, Petersburg ͑31͒, Poland ͑13͒, Pushchino ͑23͒, Special talvan et al. ͑2000͒ and Baraffe et al. ͑1997͒, for two differ- Astrophysical Observatory, ‘‘SAO’’ ͑49͒, Tajikistan ͑9͒, ent metallicities, ͓Fe/H͔ϭϪ1.5 and ͓Fe/H͔ϭϪ2.0. The ͑ ͒ ͑ ͒ Uzbekistan 24 , and Yugoslavia 22 . The quantities in pa- two models, although very similar, give slightly different rentheses give the number of scientific staff, the grand total slopes. Both, however, confirm the difference in slopes be- of which is 342 members. -
Saul J. Adelman
SAUL J. ADELMAN Department of Physics 1434 Fairfield Avenue The Citadel Charleston, SC 29407 Charleston, SC 29409 (843) 766-5348 (843) 953-6943 CURRENT POSITION: Professor of Physics, The Citadel (Aug. 22, 1989 - to date) PAST POSITIONS: Associate Professor of Physics, The Citadel (Aug. 23, 1983 to Aug. 21, 1989) NRC-NASA Research Associate, NASA Goddard Space Flight Center (Aug. 1, 1984 - July 31, 1986) Assistant Professor of Physics, The Citadel (Aug. 21, 1978 - Aug. 22, 1983) Assistant Professor of Astronomy, Boston University (Sept. 1, 1974 - Aug. 31, 1978) NAS/NRC Postdoctoral Resident Research Associate, NASA Goddard SpaceFlight Center (Aug. 1, 1972 - Aug. 31, 1974) EDUCATION: Ph.D. in Astronomy, California Institute of Technology, June 1972; Thesis: A Study of Twenty- One Sharp-lined Non-Variable Cool Peculiar A Stars, December 1971 (Dissertation Abstracts International 33, 543-13, number 77-22, 597) B.S. in Physics with high honors and high honors in physics, University of Maryland, June 1966 ACADEMIC HONORS: Phi Beta Kappa Phi Kappa Phi Sigma Pi Sigma Sigma Xi Summer Institute in Space Physics at Columbia University 1965 NDEA Title IV Fellowship 1966-69 ARCS Foundation Fellowship 1970-71 Citadel Development Foundation Faculty Fellowship 1987-93 Faculty Achievement Award 1989, 1997 Governor’s Award for Excellence in Scientific Research at a Primarily Undergraduate Institution 2011 OBSERVING EXPERIENCE: Guest Investigator, Dominion Astrophysical Observatory 1984-2018 Guest Investigator, Hubble Space Telescope 2003-05, 2011-18 Participant -
FY12 High-Level Deliverables
National Optical Astronomy Observatory Fiscal Year Annual Report for FY 2012 (1 October 2011 – 30 September 2012) Submitted to the National Science Foundation Pursuant to Cooperative Support Agreement No. AST-0950945 21 December 2012 NOAO is operated by the Association of Universities for Research in Astronomy under cooperative agreement with the National Science Foundation Contents NOAO MISSION PROFILE ................................................................................................. IV 1 EXECUTIVE SUMMARY ................................................................................................ 1 2 NOAO ACCOMPLISHMENTS ....................................................................................... 3 2.1 Achievements ..................................................................................................... 3 2.2 Status of Vision and Goals ................................................................................. 4 2.2.1 Status of FY12 High-Level Deliverables ............................................ 5 2.2.2 FY12 Planned vs. Actual Spending and Revenues .............................. 7 2.3 Challenges and Their Impacts .......................................................................... 10 3 SCIENTIFIC ACTIVITIES AND FINDINGS .............................................................. 12 3.1 Cerro Tololo Inter-American Observatory ....................................................... 12 3.2 Kitt Peak National Observatory ...................................................................... -
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Arxiv:0706.1988V3 [Physics.Ed-Ph] 15 Jun 2016 M ~R + M ~R R~ = 1 1 2 2
Lectures on Astronomy, Astrophysics, and Cosmology Luis A. Anchordoqui Department of Physics and Astronomy, Lehman College, City University of New York, NY 10468, USA Department of Physics, Graduate Center, City University of New York, 365 Fifth Avenue, NY 10016, USA Department of Astrophysics, American Museum of Natural History, Central Park West 79 St., NY 10024, USA (Dated: Spring 2016) This is a written version of a series of lectures aimed at undergraduate students in astrophysics/particle theory/particle experiment. We summarize the important progress made in recent years towards understanding high energy astrophysical processes and we survey the state of the art regarding the concordance model of cosmology. I. ACROSS THE UNIVERSE changed after Galileo’s first telescopic observations: we no longer place ourselves at the center and we view the A look at the night sky provides a strong impression of universe as vastly larger [1–3]. a changeless universe. We know that clouds drift across In the early 1600s, Kepler proposed three laws that the Moon, the sky rotates around the polar star, and on described the motion of planets in a sun-centered solar longer times, the Moon itself grows and shrinks and the system [4]. The laws are: Moon and planets move against the background of stars. 1. Planets orbit the Sun in ellipses, with the Sun in Of course we know that these are merely local phenom- one of the two focuses. ena caused by motions within our solar system. Far beyond the planets, the stars appear motionless. Herein 2. The line connecting the Sun and a planet sweeps we are going to see that this impression of changeless- out equal area in equal time.