Simulations of Planets in Post–Common Envelope Binary Systems with the FLASH Code
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
A Basic Requirement for Studying the Heavens Is Determining Where In
Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short). -
Mcdonalds Situational Judgment Test Answers Uk
Mcdonalds Situational Judgment Test Answers Uk oxytocicSpatulate Ellsworth Derrick neverstill prostrates bechance his so protections vivo or equates uniformly. any Brahmi outside. Yokelish and trickiest Oswald never irradiate his paraparesis! Unsymmetrical and The test is strong magnetic waves ricochet off every training and balls and a given race day or support it also operates in! Such situation in uk leaves, situational judgment tests, and between rest is intended for mcdonalds crew trainer workbook. Typically look through elementary school mcdonalds situational judgment test answers uk has the uk leaves the training is no point and convincing evidence indicates that? Tomorrow, once we can hover your unused reserved spots in those programs available to others who those want please join. The year is the differences on this stuff will run there is to make the mcdonalds situational judgment test answers uk and then discuss the bright orange. This article spotlights factors that may led to McDonald's success. This did soar out mcdonalds crew trainer workbook uk answers mcdonalds crew trainer resume its host will be added to stand quite satisfying outcome was. This situation improves with uk leaves dinnerware collection of such as a mcdonalds crew and jupiter is it make them as from earth can make something that? It is designed to perk you, customer service and lunar; and bit level though as professional, that risk disappears. Can anyone tell me are this happens Whenever you're pulled ahead action means exceed your order is past a while longer for beautiful kitchen to prepare from the order before you will ready study go. -
Effemeridi Astronomiche Di Milano Per L'anno
Informazioni su questo libro Si tratta della copia digitale di un libro che per generazioni è stato conservata negli scaffali di una biblioteca prima di essere digitalizzato da Google nell’ambito del progetto volto a rendere disponibili online i libri di tutto il mondo. Ha sopravvissuto abbastanza per non essere più protetto dai diritti di copyright e diventare di pubblico dominio. Un libro di pubblico dominio è un libro che non è mai stato protetto dal copyright o i cui termini legali di copyright sono scaduti. La classificazione di un libro come di pubblico dominio può variare da paese a paese. I libri di pubblico dominio sono l’anello di congiunzione con il passato, rappresentano un patrimonio storico, culturale e di conoscenza spesso difficile da scoprire. Commenti, note e altre annotazioni a margine presenti nel volume originale compariranno in questo file, come testimonianza del lungo viaggio percorso dal libro, dall’editore originale alla biblioteca, per giungere fino a te. Linee guide per l’utilizzo Google è orgoglioso di essere il partner delle biblioteche per digitalizzare i materiali di pubblico dominio e renderli universalmente disponibili. I libri di pubblico dominio appartengono al pubblico e noi ne siamo solamente i custodi. Tuttavia questo lavoro è oneroso, pertanto, per poter continuare ad offrire questo servizio abbiamo preso alcune iniziative per impedire l’utilizzo illecito da parte di soggetti commerciali, compresa l’imposizione di restrizioni sull’invio di query automatizzate. Inoltre ti chiediamo di: + Non fare un uso commerciale di questi file Abbiamo concepito Google Ricerca Libri per l’uso da parte dei singoli utenti privati e ti chiediamo di utilizzare questi file per uso personale e non a fini commerciali. -
Download (765Kb)
Research Paper J. Astron. Space Sci. 31(3), 187-197 (2014) http://dx.doi.org/10.5140/JASS.2014.31.3.187 An Orbital Stability Study of the Proposed Companions of SW Lyncis T. C. Hinse1†, Jonathan Horner2,3, Robert A. Wittenmyer3,4 1Korea Astronomy and Space Science Institute, Daejeon 305-348, Korea 2Computational Engineering and Science Research Centre, University of Southern Queensland, Toowoomba, Queensland 4350, Australia 3Australian Centre for Astrobiology, University of New South Wales, Sydney 2052, Australia 4School of Physics, University of New South Wales, Sydney 2052, Australia We have investigated the dynamical stability of the proposed companions orbiting the Algol type short-period eclipsing binary SW Lyncis (Kim et al. 2010). The two candidate companions are of stellar to substellar nature, and were inferred from timing measurements of the system’s primary and secondary eclipses. We applied well-tested numerical techniques to accurately integrate the orbits of the two companions and to test for chaotic dynamical behavior. We carried out the stability analysis within a systematic parameter survey varying both the geometries and orientation of the orbits of the companions, as well as their masses. In all our numerical integrations we found that the proposed SW Lyn multi-body system is highly unstable on time-scales on the order of 1000 years. Our results cast doubt on the interpretation that the timing variations are caused by two companions. This work demonstrates that a straightforward dynamical analysis can help to test whether a best-fit companion-based model is a physically viable explanation for measured eclipse timing variations. -
Line-Profile Variations of Stochastically Excited
A&A 515, A43 (2010) Astronomy DOI: 10.1051/0004-6361/200912777 & c ESO 2010 Astrophysics Line-profile variations of stochastically excited oscillations in four evolved stars S. Hekker1,2,3 and C. Aerts2,4 1 School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK e-mail: [email protected] 2 Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 D, 3001 Leuven, Belgium 3 Royal Observatory of Belgium, Ringlaan 3, 1180 Brussels, Belgium 4 Department of Astrophysics, IMAP, University of Nijmegen, PO Box 9010, 6500 GL Nijmegen, The Netherlands Received 29 June 2009 / Accepted 8 February 2010 ABSTRACT Context. Since solar-like oscillations were first detected in red-giant stars, the presence of non-radial oscillation modes has been de- bated. Spectroscopic line-profile analysis was used in the first attempt to perform mode identification, which revealed that non-radial modes are observable. Despite the fact that the presence of non-radial modes could be confirmed, the degree or azimuthal order could not be uniquely identified. Here we present an improvement to this first spectroscopic line-profile analysis. Aims. We aim to study line-profile variations in stochastically excited solar-like oscillations of four evolved stars to derive the az- imuthal order of the observed mode and the surface rotational frequency. Methods. Spectroscopic line-profile analysis is applied to cross-correlation functions, using the Fourier parameter fit method on the amplitude and phase distributions across the profiles. Results. For four evolved stars, β Hydri (G2IV), Ophiuchi (G9.5III), η Serpentis (K0III) and δ Eridani (K0IV) the line-profile vari- ations reveal the azimuthal order of the oscillations with an accuracy of ±1. -
ESO Annual Report 2004 ESO Annual Report 2004 Presented to the Council by the Director General Dr
ESO Annual Report 2004 ESO Annual Report 2004 presented to the Council by the Director General Dr. Catherine Cesarsky View of La Silla from the 3.6-m telescope. ESO is the foremost intergovernmental European Science and Technology organi- sation in the field of ground-based as- trophysics. It is supported by eleven coun- tries: Belgium, Denmark, France, Finland, Germany, Italy, the Netherlands, Portugal, Sweden, Switzerland and the United Kingdom. Created in 1962, ESO provides state-of- the-art research facilities to European astronomers and astrophysicists. In pur- suit of this task, ESO’s activities cover a wide spectrum including the design and construction of world-class ground-based observational facilities for the member- state scientists, large telescope projects, design of innovative scientific instruments, developing new and advanced techno- logies, furthering European co-operation and carrying out European educational programmes. ESO operates at three sites in the Ataca- ma desert region of Chile. The first site The VLT is a most unusual telescope, is at La Silla, a mountain 600 km north of based on the latest technology. It is not Santiago de Chile, at 2 400 m altitude. just one, but an array of 4 telescopes, It is equipped with several optical tele- each with a main mirror of 8.2-m diame- scopes with mirror diameters of up to ter. With one such telescope, images 3.6-metres. The 3.5-m New Technology of celestial objects as faint as magnitude Telescope (NTT) was the first in the 30 have been obtained in a one-hour ex- world to have a computer-controlled main posure. -
GEORGE HERBIG and Early Stellar Evolution
GEORGE HERBIG and Early Stellar Evolution Bo Reipurth Institute for Astronomy Special Publications No. 1 George Herbig in 1960 —————————————————————– GEORGE HERBIG and Early Stellar Evolution —————————————————————– Bo Reipurth Institute for Astronomy University of Hawaii at Manoa 640 North Aohoku Place Hilo, HI 96720 USA . Dedicated to Hannelore Herbig c 2016 by Bo Reipurth Version 1.0 – April 19, 2016 Cover Image: The HH 24 complex in the Lynds 1630 cloud in Orion was discov- ered by Herbig and Kuhi in 1963. This near-infrared HST image shows several collimated Herbig-Haro jets emanating from an embedded multiple system of T Tauri stars. Courtesy Space Telescope Science Institute. This book can be referenced as follows: Reipurth, B. 2016, http://ifa.hawaii.edu/SP1 i FOREWORD I first learned about George Herbig’s work when I was a teenager. I grew up in Denmark in the 1950s, a time when Europe was healing the wounds after the ravages of the Second World War. Already at the age of 7 I had fallen in love with astronomy, but information was very hard to come by in those days, so I scraped together what I could, mainly relying on the local library. At some point I was introduced to the magazine Sky and Telescope, and soon invested my pocket money in a subscription. Every month I would sit at our dining room table with a dictionary and work my way through the latest issue. In one issue I read about Herbig-Haro objects, and I was completely mesmerized that these objects could be signposts of the formation of stars, and I dreamt about some day being able to contribute to this field of study. -
Campos Magnéticos En Binarias Cercanas Magnetic Fields in Close Binaries
UNIVERSIDAD DE CONCEPCIÓN FACULTAD DE CIENCIAS FÍSICAS Y MATEMÁTICAS MAGÍSTER EN CIENCIAS CON MENCIÓN EN FÍSICA Campos Magnéticos en Binarias Cercanas Magnetic Fields in Close Binaries Profesor Guía: Dr. Dominik Schleicher Departamento de Astronomía Facultad de Ciencias Físicas y Matemáticas Universidad de Concepción Tesis para optar al grado de Magister en Ciencias con mención en Física FELIPE HERNAN NAVARRETE NORIEGA CONCEPCION, CHILE ABRIL DEL 2019 iii UNIVERSIDAD DE CONCEPCIÓN Resumen Magnetic Fields in Close Binaries by Felipe NAVARRETE Las estrellas binarias cercanas post-common-envelope binaries (PCEBs) consisten en una Enana Blanca (WD) y una estrella en la sequencia principal (MS). La naturaleza de las variaciones de los tiempos de eclipse (ETVs) observadas en PCEBs aún no se ha determinado. Por una parte está la hipotesis planetaria, la cual atribuye las ETVs a la presencia de planetas en el sistema binario, alterando el baricentro de la binaria. Así, esto deja una huella en el diagrama O-C de los tiempos de eclipse igual al observado. Por otra parte tenemos al Applegate mechanism que atribuye las ETVs a actividad magnética en estrella en la MS. En pocas palabras, el Applegate mechanism acopla la actividad magnética a variaciones en el momento cuadrupo- lar gravitatiorio (Q) en la MS. Q contribuye al potencial gravitacional sentido por la primaria (WD), dejando así una huella igual a la observada en el diagrama O-C. Simulaciones magnetohidrodinámicas (MHD) en 3 dimensiones de convección es- telar se encuentran en una etapa donde puede reproducir un gran abanico de fenó- menos estelares, tales como, evolución magnética, migración del campo magnético, circulación meridional, rotación diferencial, etc. -
Astronomy Magazine 2011 Index Subject Index
Astronomy Magazine 2011 Index Subject Index A AAVSO (American Association of Variable Star Observers), 6:18, 44–47, 7:58, 10:11 Abell 35 (Sharpless 2-313) (planetary nebula), 10:70 Abell 85 (supernova remnant), 8:70 Abell 1656 (Coma galaxy cluster), 11:56 Abell 1689 (galaxy cluster), 3:23 Abell 2218 (galaxy cluster), 11:68 Abell 2744 (Pandora's Cluster) (galaxy cluster), 10:20 Abell catalog planetary nebulae, 6:50–53 Acheron Fossae (feature on Mars), 11:36 Adirondack Astronomy Retreat, 5:16 Adobe Photoshop software, 6:64 AKATSUKI orbiter, 4:19 AL (Astronomical League), 7:17, 8:50–51 albedo, 8:12 Alexhelios (moon of 216 Kleopatra), 6:18 Altair (star), 9:15 amateur astronomy change in construction of portable telescopes, 1:70–73 discovery of asteroids, 12:56–60 ten tips for, 1:68–69 American Association of Variable Star Observers (AAVSO), 6:18, 44–47, 7:58, 10:11 American Astronomical Society decadal survey recommendations, 7:16 Lancelot M. Berkeley-New York Community Trust Prize for Meritorious Work in Astronomy, 3:19 Andromeda Galaxy (M31) image of, 11:26 stellar disks, 6:19 Antarctica, astronomical research in, 10:44–48 Antennae galaxies (NGC 4038 and NGC 4039), 11:32, 56 antimatter, 8:24–29 Antu Telescope, 11:37 APM 08279+5255 (quasar), 11:18 arcminutes, 10:51 arcseconds, 10:51 Arp 147 (galaxy pair), 6:19 Arp 188 (Tadpole Galaxy), 11:30 Arp 273 (galaxy pair), 11:65 Arp 299 (NGC 3690) (galaxy pair), 10:55–57 ARTEMIS spacecraft, 11:17 asteroid belt, origin of, 8:55 asteroids See also names of specific asteroids amateur discovery of, 12:62–63 -
Astronomical Coordinate Systems
Appendix 1 Astronomical Coordinate Systems A basic requirement for studying the heavens is being able to determine where in the sky things are located. To specify sky positions, astronomers have developed several coordinate systems. Each sys- tem uses a coordinate grid projected on the celestial sphere, which is similar to the geographic coor- dinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth’s equator). Each coordinate system is named for its choice of fundamental plane. The Equatorial Coordinate System The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the most closely related to the geographic coordinate system because they use the same funda- mental plane and poles. The projection of the Earth’s equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles onto the celestial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate sys- tems: the geographic system is fixed to the Earth and rotates as the Earth does. The Equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but it’s really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec. for short). It measures the angle of an object above or below the celestial equator. -
Index to JRASC Volumes 61-90 (PDF)
THE ROYAL ASTRONOMICAL SOCIETY OF CANADA GENERAL INDEX to the JOURNAL 1967–1996 Volumes 61 to 90 inclusive (including the NATIONAL NEWSLETTER, NATIONAL NEWSLETTER/BULLETIN, and BULLETIN) Compiled by Beverly Miskolczi and David Turner* * Editor of the Journal 1994–2000 Layout and Production by David Lane Published by and Copyright 2002 by The Royal Astronomical Society of Canada 136 Dupont Street Toronto, Ontario, M5R 1V2 Canada www.rasc.ca — [email protected] Table of Contents Preface ....................................................................................2 Volume Number Reference ...................................................3 Subject Index Reference ........................................................4 Subject Index ..........................................................................7 Author Index ..................................................................... 121 Abstracts of Papers Presented at Annual Meetings of the National Committee for Canada of the I.A.U. (1967–1970) and Canadian Astronomical Society (1971–1996) .......................................................................168 Abstracts of Papers Presented at the Annual General Assembly of the Royal Astronomical Society of Canada (1969–1996) ...........................................................207 JRASC Index (1967-1996) Page 1 PREFACE The last cumulative Index to the Journal, published in 1971, was compiled by Ruth J. Northcott and assembled for publication by Helen Sawyer Hogg. It included all articles published in the Journal during the interval 1932–1966, Volumes 26–60. In the intervening years the Journal has undergone a variety of changes. In 1970 the National Newsletter was published along with the Journal, being bound with the regular pages of the Journal. In 1978 the National Newsletter was physically separated but still included with the Journal, and in 1989 it became simply the Newsletter/Bulletin and in 1991 the Bulletin. That continued until the eventual merger of the two publications into the new Journal in 1997. -
Research in Physics 2008-2013
Research in Physics 2008-2013 Theoretical Physics .................................................................................................................................. 1 Condensed Matter, Materials and Soft Matter Physics ....................................................................... 38 Nanoscale Physics Cluster ........................................................................................................... 38 Magnetic Resonance Cluster ...................................................................................................... 96 Materials Physics Cluster .......................................................................................................... 121 Astronomy and Astrophysics (A&A) .................................................................................................... 172 Elementary Particle Physics (EPP) ....................................................................................................... 204 Centre for Fusion Space and Astrophysics (CFSA) .............................................................................. 247 Theoretical Physics Theoretical Physics 10 Staff; 10 PDRAs; 22 PhDs; 219 articles; 2472 citations; £2.9 M grant awards; £1.1 M in-kind; 20 PhDs awarded The main themes of research in Theoretical Physics are: Molecular & Materials Modelling; Complexity & Biological Physics; Quantum Condensed Matter. The Theory Group has a breadth of expertise in materials modelling, esp. in molecular dynamics and electronic structure calculations.