Kidger M. Cosmological Enigmas.. Pulsars, Quasars, and Other Deep
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Dynamics and Stability of Telluric Planets Within the Habitable Zone of Extrasolar Planetary Systems
A&A 488, 1133–1147 (2008) Astronomy DOI: 10.1051/0004-6361:200809822 & c ESO 2008 Astrophysics Dynamics and stability of telluric planets within the habitable zone of extrasolar planetary systems Numerical simulations of test particles within the HD 4208 and HD 70642 systems T. C. Hinse1,2, R. Michelsen1,U.G.Jørgensen1 ,K.Go´zdziewski3, and S. Mikkola4 1 Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Ø, Denmark e-mail: [tobiash; rm]@astro.ku.dk 2 Armagh Observatory, College Hill, BT61 9DG Armagh, Northern Ireland, UK 3 Nicolaus Copernicus University, Torun Centre for Astronomy, Gagarin Str. 11, 87-100 Torun, Poland 4 Turku University Observatory, Väisäläntie 20, Piikkiö, Finland Received 20 March 2008 / Accepted 3 June 2008 ABSTRACT Aims. We study gravitational perturbation effects of observed giant extrasolar planets on hypothetical Earth-like planets in the context of the three-body problem. This paper considers a large parameter survey of different orbital configuration of two extrasolar giant planets (HD 70642b and HD 4208b) and compares their dynamical effect on Earth-mass planetary orbits initially located within the respective habitable terrestrial region. We are interested in determining giant-planet orbit (and mass) parameters that favor the condi- tion to render an Earth-mass planet to remain on a stable and bounded orbit within the continuous habitable zone. Methods. We applied symplectic numerical integration techniques to studying the short and long term time evolution of hypothetical Earth-mass planets that are treated as particles. In addition, we adopt the MEGNO technique to obtain a complete dynamical picture of the terrestrial phase space environment. -
Naming the Extrasolar Planets
Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named. -
Radio and Millimeter Continuum Surveys and Their Astrophysical Implications
The Astronomy and Astrophysics Review (2011) DOI 10.1007/s00159-009-0026-0 REVIEWARTICLE Gianfranco De Zotti · Marcella Massardi · Mattia Negrello · Jasper Wall Radio and millimeter continuum surveys and their astrophysical implications Received: 13 May 2009 c Springer-Verlag 2009 Abstract We review the statistical properties of the main populations of radio sources, as emerging from radio and millimeter sky surveys. Recent determina- tions of local luminosity functions are presented and compared with earlier esti- mates still in widespread use. A number of unresolved issues are discussed. These include: the (possibly luminosity-dependent) decline of source space densities at high redshifts; the possible dichotomies between evolutionary properties of low- versus high-luminosity and of flat- versus steep-spectrum AGN-powered radio sources; and the nature of sources accounting for the upturn of source counts at sub-milli-Jansky (mJy) levels. It is shown that straightforward extrapolations of evolutionary models, accounting for both the far-IR counts and redshift distribu- tions of star-forming galaxies, match the radio source counts at flux-density levels of tens of µJy remarkably well. We consider the statistical properties of rare but physically very interesting classes of sources, such as GHz Peak Spectrum and ADAF/ADIOS sources, and radio afterglows of γ-ray bursts. We also discuss the exploitation of large-area radio surveys to investigate large-scale structure through studies of clustering and the Integrated Sachs–Wolfe effect. Finally, we briefly describe the potential of the new and forthcoming generations of radio telescopes. A compendium of source counts at different frequencies is given in Supplemen- tary Material. -
Tvsnews 02 09.Qxd (Page 1)
PRIMEFOCUS 2002 Tri-Valley Stargazers September September Meeting Mirror testing: An overview of amateur mirror testing techniques with an in depth look at the new lateral wire test Meeting Info: OR What So you want to test a mirror… So you want to test a mirror… Figure 1 Who John Swenson John Swenson Amateur mirror testing is a bit of a black art. Many books describe it, but no matter how When many books you read, actually performing September 20, 2002 the test is a surprise. This talk will actually Conversation at 7:00 p.m. perform several of the common mirror tests Lecture at 7:30 p.m. with what you see projected on a TV screen so you can get a “feel” for what it’s like to Where squint at fleeting shadows. Unitarian Universalist I will go into detail on the new “lateral wire Church in Livermore test”, a very simple test that is MUCH easier 1893 N. Vasco Road to perform than the others, and is valid for a Figure 2 much broader range of mirrors. I’ll run a mirror or two through the process and come Inside up with a surface error chart for them. Hopefully this presentation will demystify the News & Notes 2 art of mirror testing enough so that some of Calendar of Events 2 you will dive in and make your own mirror. Star Parties 5 Astronomical Insights 5 Figures 1-3 What’s Up 6 The images on the right show three different types Membership/Renewal of mirror testing. Note that these test images are not from the same mirror. -
The State of Anthro–Earth
The Rosette Gazette Volume 22,, IssueIssue 7 Newsletter of the Rose City Astronomers July, 2010 RCA JULY 19 GENERAL MEETING The State Of Anthro–Earth THE STATE OF ANTHRO-EARTH: A Visitor From Far, Far Away Reviews the Status of Our Planet In This Issue: A Talk (in Earth-English) By Richard Brenne 1….General Meeting Enrico Fermi famously wondered why we hadn't heard from any other planetary 2….Club Officers civilizations, and Richard Brenne, who we'd always suspected was probably from another planet, thinks he might know the answer. Carl Sagan thought it was likely …...Magazines because those on other planets blew themselves up with nuclear weapons, but Richard …...RCA Library thinks its more likely that burning fossil fuels changed the climates and collapsed the 3….Local Happenings civilizations of those we might otherwise have heard from. Only someone from another planet could discuss this most serious topic with Richard's trademark humor 4…. Telescope (in a previous life he was an award-winning screenwriter - on which planet we're not Transformation sure) and bemused detachment. 5….Special Interest Groups Richard Brenne teaches a NASA-sponsored Global Climate Change class, serves on 6….Star Party Scene the American Meteorological Society's Committee to Communicate Climate Change, has written and produced documentaries about climate change since 1992, and has 7.…Observers Corner produced and moderated 50 hours of panel discussions about climate change with 18...RCA Board Minutes many of the world's top climate change scientists. Richard writes for the blog "Climate Progress" and his forthcoming book is titled "Anthro-Earth", his new name 20...Calendars for his adopted planet. -
Dynamical Stability and Habitability of a Terrestrial Planet in HD74156
A dynamic search for potential habitable planets amongst the extrasolar planets 1,2 1 1 1,3 1, 4 P. Hinds , A. Munro , S. T. Maddison , C. Tan , and M. C. Gino [1] Swinburne University, Australia [2] Pierce College, USA [3] Methodist Ladies’ College, Australia [4] Dudley Observatory, USA ABSTRACT: While the detection of habitable terrestrial planets around nearby stars is currently beyond our observational capabilities, dynamical studies can help us locate potential candidates. Following from the work of Menou & Tabachnik (2003), we use a symplectic integrator to search for potential stable terrestrial planetary orbits in the habitable zones of known extrasolar planetary systems. A swarm of massless test particles is initially used to identify stability zones, and then an Earth-mass planet is placed within these zones to investigate their dynamical stability. We investigate 22 new systems discovered since the work of Menou & Tabachnik, as well as simulate some of the previous 85 extrasolar systems whose orbital parameters have been more precisely constrained. In particular, we model three systems that are now confirmed or potential double planetary systems: HD169830, HD160691 and eps Eridani. The results of these dynamical studies can be used as a potential target list for the Terrestrial Planet Finder. Introduction Numerical Technique Results & Discussion To date 122 extrasolar planets have been detected around 107 stars, with 13 of them To follow the evolution of the planetary systems, we use the SWIFT integration software package1. This The systems we have investigated broadly fall in four categories: (1) unstable being multiple planet systems (Schneider, 2004). Observational evidence for the allows us to model a planetary system and a swarm of massless test particles in orbit around a central star. -
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 ::::::::::::::::::::::::::::::::::::::: -
Exoplanet Community Report
JPL Publication 09‐3 Exoplanet Community Report Edited by: P. R. Lawson, W. A. Traub and S. C. Unwin National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology Pasadena, California March 2009 The work described in this publication was performed at a number of organizations, including the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). Publication was provided by the Jet Propulsion Laboratory. Compiling and publication support was provided by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not constitute or imply its endorsement by the United States Government, or the Jet Propulsion Laboratory, California Institute of Technology. © 2009. All rights reserved. The exoplanet community’s top priority is that a line of probeclass missions for exoplanets be established, leading to a flagship mission at the earliest opportunity. iii Contents 1 EXECUTIVE SUMMARY.................................................................................................................. 1 1.1 INTRODUCTION...............................................................................................................................................1 1.2 EXOPLANET FORUM 2008: THE PROCESS OF CONSENSUS BEGINS.....................................................2 -
The 1.4 Ghz Light Curve of GRB 970508
The 1.4 GHz light curve of GRB 970508 T.J. Galama1, R.A.M.J. Wijers2, M. Bremer3, P.J. Groot1, R.G. Strom1,4, A.G. de Bruyn4,5, C. Kouveliotou6,7, C.R. Robinson6,7, J. van Paradijs1,8 ABSTRACT We report on Westerbork 1.4 GHz radio observations of the radio counterpart to γ-ray burst GRB 970508, between 0.80 and 138 days after this event. The 1.4 GHz light curve shows a transition from optically thick to thin emission between 39 and 54 days after the event. We derive the slope p of the spectrum of injected ∝ −p electrons (dN/dγe γe ) in two independent ways which yield values very close to p = 2.2. This is in agreement with a relativistic dynamically near-adiabatic blast wave model whose emission is dominated by synchrotron radiation and in which a significant fraction of the electrons cool fast. Subject headings: gamma rays: bursts — gamma rays: individual (GRB 970508) — radio continuum: general 1. Introduction The peak luminosities of γ-ray bursts (GRBs) are highly super-Eddington and require relativistic outflows (Paczy´nski 1986; Goodman 1986). Paczy´nski and Rhoads (1993) pointed out that radio emission is expected as a result of the interaction between such arXiv:astro-ph/9804190v1 20 Apr 1998 1Astronomical Institute ‘Anton Pannekoek’, University of Amsterdam, & Center for High Energy Astrophysics, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands 2Institute of Astronomy, Madingley Road, Cambridge, UK 3Institut de Radio Astronomie Millim´etrique, 300 rue de la Piscine, F–38406 Saint-Martin d’H`eres, France 4NFRA, Postbus 2, 7990 AA Dwingeloo, The Netherlands 5Kapteyn Astronomical Institute, Postbus 800, 9700 AV, Groningen, The Netherlands 6Universities Space Research Asociation 7NASA/MSFC, Code ES-84, Huntsville AL 35812, USA 8Physics Department, University of Alabama in Huntsville, Huntsville AL 35899, USA –2– a relativistic outflow and an external medium, as is, e.g., observed in extragalactic jet sources (see also Katz 1994; M´esz´aros and Rees 1997). -
Exploring the Realm of Scaled Solar System Analogues with HARPS?,?? D
A&A 615, A175 (2018) Astronomy https://doi.org/10.1051/0004-6361/201832711 & c ESO 2018 Astrophysics Exploring the realm of scaled solar system analogues with HARPS?;?? D. Barbato1,2, A. Sozzetti2, S. Desidera3, M. Damasso2, A. S. Bonomo2, P. Giacobbe2, L. S. Colombo4, C. Lazzoni4,3 , R. Claudi3, R. Gratton3, G. LoCurto5, F. Marzari4, and C. Mordasini6 1 Dipartimento di Fisica, Università degli Studi di Torino, via Pietro Giuria 1, 10125, Torino, Italy e-mail: [email protected] 2 INAF – Osservatorio Astrofisico di Torino, Via Osservatorio 20, 10025, Pino Torinese, Italy 3 INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122, Padova, Italy 4 Dipartimento di Fisica e Astronomia “G. Galilei”, Università di Padova, Vicolo dell’Osservatorio 3, 35122, Padova, Italy 5 European Southern Observatory, Alonso de Córdova 3107, Vitacura, Santiago, Chile 6 Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012, Bern, Switzerland Received 8 February 2018 / Accepted 21 April 2018 ABSTRACT Context. The assessment of the frequency of planetary systems reproducing the solar system’s architecture is still an open problem in exoplanetary science. Detailed study of multiplicity and architecture is generally hampered by limitations in quality, temporal extension and observing strategy, causing difficulties in detecting low-mass inner planets in the presence of outer giant planets. Aims. We present the results of high-cadence and high-precision HARPS observations on 20 solar-type stars known to host a single long-period giant planet in order to search for additional inner companions and estimate the occurence rate fp of scaled solar system analogues – in other words, systems featuring lower-mass inner planets in the presence of long-period giant planets. -
On the Hunt for Excited States
INTERNATIONAL JOURNAL OF HIGH-ENERGY PHYSICS CERN COURIER VOLUME 45 NUMBER 10 DECEMBER 2005 On the hunt for excited states HOMESTAKE DARK MATTER SNOWMASS Future assured for Galactic gamma rays US workshop gets underground lab p5 may hold the key p 17 ready for the ILC p24 www.vectorfields.comi Music to your ears 2D & 3D electromagnetic modellinj If you're aiming for design excellence, demanding models. As a result millions you'll be pleased to hear that OPERA, of elements can be solved in minutes, the industry standard for electromagnetic leaving you to focus on creating modelling, gives you the most powerful outstanding designs. Electron trajectories through a TEM tools for engineering and scientific focussing stack analysis. Fast, accurate model analysis • Actuators and sensors - including Designed for parameterisation and position and NDT customisation, OPERA is incredibly easy • Magnets - ppm accuracy using TOSCA to use and has an extensive toolset, making • Electron devices - space charge analysis it ideal for a wide range of applications. including emission models What's more, its high performance analysis • RF Cavities - eigen modes and single modules work at exceptional levels of speed, frequency response accuracy and stability, even with the most • Motors - dynamic analysis including motion Don't take our word for it - order your free trial and check out OPERA yourself. B-field in a PMDC motor Vector Fields Ltd Culham Science Centre, Abingdon, Oxon, 0X14 3ED, U.K. Tel: +44 (0)1865 370151 Fax: +44 (0)1865 370277 Email: [email protected] Vector Fields Inc 1700 North Famsworth Avenue, Aurora, IL, 60505. -
• August the 26Th 2004 Detection of the Radial-Velocity Signal Induced by OGLE-TR-111 B Using UVES/FLAMES on the VLT (See Pont Et Al
2004 • August the 26th 2004 Detection of the radial-velocity signal induced by OGLE-TR-111 b using UVES/FLAMES on the VLT (see Pont et al. 2004, A&A in press, astro-ph/0408499). • August the 25th 2004 TrES-1b: A new transiting exoplanet detected by the Trans-Atlantic Exoplanet Survey (TreS) team . (see Boulder Press release or Alonso et al.) • August the 25th 2004 HD 160691 c : A 14 Earth-mass planet detected with HARPS (see ESO Press Release or Santos et al.) • July the 8th 2004 HD 37605 b: The first extra-solar planet detected with HRS on the Hobby- Eberly Telescope (Cochran et al.) • May the 3rd 2004 HD 219452 Bb withdrawn by Desidera et al. • April the 28th 2004 Orbital solution for OGLE-TR-113 confirmed by Konacki et al • April the 15th 2004 OGLE 2003-BLG-235/MOA 2003-BLG-53: a planetary microlensing event (Bond et al.) • April the 14th 2004 FLAMES-UVES spectroscopic orbits for two OGLE III transiting candidates: OGLE-TR-113 and OGLE-TR-132 (Bouchy et al.) • February 2004 Detection of Carbon and Oxygen in the evaporating atmosphere of HD 209458 b by A. Vidal-Madjar et al. (from HST observations). • January the 5th 2004 Two planets orbiting giant stars announced by Mitchell et al. during the AAS meeting: HD 59686 b and 91 Aqr b (HD 219499 b). Two other more massive companions, Tau Gem b (HD 54719 b) and nu Oph b (HD 163917 b), have also been announced by the same authors. 2003 • December 2003 First planet detected with HARPS: HD 330075 b (see Mayor et al., in the ESO Messenger No 114) • July the 3rd 2003 A long-period planet on a circular orbit around HD 70642 announced by the AAT team (Carter et al.