Homogeneous Photospheric Parameters and C Abundances in G
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Review HEAVY METAL RULES. I. EXOPLANET INCIDENCE AND METALLICITY Vardan Adibekyan1 ID 1 Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal; [email protected] Academic Editor: name Received: date; Accepted: date; Published: date Abstract: Discovery of only handful of exoplanets required to establish a correlation between giant planet occurrence and metallicity of their host stars. More than 20 years have already passed from that discovery, however, many questions are still under lively debate: What is the origin of that relation? what is the exact functional form of the giant planet – metallicity relation (in the metal-poor regime)?, does such a relation exist for terrestrial planets? All these question are very important for our understanding of the formation and evolution of (exo)planets of different types around different types of stars and are subject of the present manuscript. Besides making a comprehensive literature review about the role of metallicity on the formation of exoplanets, I also revisited most of the planet – metallicity related correlations reported in the literature using a large and homogeneous data provided by the SWEET-Cat catalog. This study lead to several new results and conclusions, two of which I believe deserve to be highlighted in the abstract: i) The hosts of sub-Jupiter mass planets (∼0.6 – 0.9 M ) are systematically less metallic than the hosts of Jupiter-mass planets. This result might be relatedX to the longer disk lifetime and higher amount of planet building materials available at high metallicities, which allow a formation of more massive Jupiter-like planets. -
Fang Family San Francisco Examiner Photograph Archive Negative Files, Circa 1930-2000, Circa 1930-2000
http://oac.cdlib.org/findaid/ark:/13030/hb6t1nb85b No online items Finding Aid to the Fang family San Francisco examiner photograph archive negative files, circa 1930-2000, circa 1930-2000 Bancroft Library staff The Bancroft Library University of California, Berkeley Berkeley, CA 94720-6000 Phone: (510) 642-6481 Fax: (510) 642-7589 Email: [email protected] URL: http://bancroft.berkeley.edu/ © 2010 The Regents of the University of California. All rights reserved. Finding Aid to the Fang family San BANC PIC 2006.029--NEG 1 Francisco examiner photograph archive negative files, circa 1930-... Finding Aid to the Fang family San Francisco examiner photograph archive negative files, circa 1930-2000, circa 1930-2000 Collection number: BANC PIC 2006.029--NEG The Bancroft Library University of California, Berkeley Berkeley, CA 94720-6000 Phone: (510) 642-6481 Fax: (510) 642-7589 Email: [email protected] URL: http://bancroft.berkeley.edu/ Finding Aid Author(s): Bancroft Library staff Finding Aid Encoded By: GenX © 2011 The Regents of the University of California. All rights reserved. Collection Summary Collection Title: Fang family San Francisco examiner photograph archive negative files Date (inclusive): circa 1930-2000 Collection Number: BANC PIC 2006.029--NEG Creator: San Francisco Examiner (Firm) Extent: 3,200 boxes (ca. 3,600,000 photographic negatives); safety film, nitrate film, and glass : various film sizes, chiefly 4 x 5 in. and 35mm. Repository: The Bancroft Library. University of California, Berkeley Berkeley, CA 94720-6000 Phone: (510) 642-6481 Fax: (510) 642-7589 Email: [email protected] URL: http://bancroft.berkeley.edu/ Abstract: Local news photographs taken by staff of the Examiner, a major San Francisco daily newspaper. -
The Angular Size of Objects in the Sky
APPENDIX 1 The Angular Size of Objects in the Sky We measure the size of objects in the sky in terms of degrees. The angular diameter of the Sun or the Moon is close to half a degree. There are 60 minutes (of arc) to one degree (of arc), and 60 seconds (of arc) to one minute (of arc). Instead of including – of arc – we normally just use degrees, minutes and seconds. 1 degree = 60 minutes. 1 minute = 60 seconds. 1 degree = 3,600 seconds. This tells us that the Rosette nebula, which measures 80 minutes by 60 minutes, is a big object, since the diameter of the full Moon is only 30 minutes (or half a degree). It is clearly very useful to know, by looking it up beforehand, what the angular size of the objects you want to image are. If your field of view is too different from the object size, either much bigger, or much smaller, then the final image is not going to look very impressive. For example, if you are using a Sky 90 with SXVF-M25C camera with a 3.33 by 2.22 degree field of view, it would not be a good idea to expect impressive results if you image the Sombrero galaxy. The Sombrero galaxy measures 8.7 by 3.5 minutes and would appear as a bright, but very small patch of light in the centre of your frame. Similarly, if you were imaging at f#6.3 with the Nexstar 11 GPS scope and the SXVF-H9C colour camera, your field of view would be around 17.3 by 13 minutes, NGC7000 would not be the best target. -
Where Are All the Sirius-Like Binary Systems?
Mon. Not. R. Astron. Soc. 000, 1-22 (2013) Printed 20/08/2013 (MAB WORD template V1.0) Where are all the Sirius-Like Binary Systems? 1* 2 3 4 4 J. B. Holberg , T. D. Oswalt , E. M. Sion , M. A. Barstow and M. R. Burleigh ¹ Lunar and Planetary Laboratory, Sonnett Space Sciences Bld., University of Arizona, Tucson, AZ 85721, USA 2 Florida Institute of Technology, Melbourne, FL. 32091, USA 3 Department of Astronomy and Astrophysics, Villanova University, 800 Lancaster Ave. Villanova University, Villanova, PA, 19085, USA 4 Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH, UK 1st September 2011 ABSTRACT Approximately 70% of the nearby white dwarfs appear to be single stars, with the remainder being members of binary or multiple star systems. The most numerous and most easily identifiable systems are those in which the main sequence companion is an M star, since even if the systems are unresolved the white dwarf either dominates or is at least competitive with the luminosity of the companion at optical wavelengths. Harder to identify are systems where the non-degenerate component has a spectral type earlier than M0 and the white dwarf becomes the less luminous component. Taking Sirius as the prototype, these latter systems are referred to here as ‘Sirius-Like’. There are currently 98 known Sirius-Like systems. Studies of the local white dwarf population within 20 pc indicate that approximately 8 per cent of all white dwarfs are members of Sirius-Like systems, yet beyond 20 pc the frequency of known Sirius-Like systems declines to between 1 and 2 per cent, indicating that many more of these systems remain to be found. -
Numerical Simulations of Jets from Active Galactic Nuclei
galaxies Review Numerical Simulations of Jets from Active Galactic Nuclei José-María Martí Departament d’Astronomia i Astrofísica and Observatori Astronòmic, Universitat de València, 46100 Burjassot (València), Spain; [email protected] Received: 12 November 2018; Accepted: 14 January 2019; Published: 22 January 2019 Abstract: Numerical simulations have been playing a crucial role in the understanding of jets from active galactic nuclei (AGN) since the advent of the first theoretical models for the inflation of giant double radio galaxies by continuous injection in the late 1970s. In the almost four decades of numerical jet research, the complexity and physical detail of simulations, based mainly on a hydrodynamical/magneto-hydrodynamical description of the jet plasma, have been increasing with the pace of the advance in theoretical models, computational tools and numerical methods. The present review summarizes the status of the numerical simulations of jets from AGNs, from the formation region in the neighborhood of the supermassive central black hole up to the impact point well beyond the galactic scales. Special attention is paid to discuss the achievements of present simulations in interpreting the phenomenology of jets as well as their current limitations and challenges. Keywords: active galactic nuclei; relativistic jets; magneto-hydrodynamics; plasma physics; numerical methods 1. Introduction Theoretical models of jets from active galactic nuclei (AGN) motivated by observations have been the subject of thorough testing by numerical simulations for almost forty years, since the simulations of supersonic jets performed in the early 1980s by Norman and collaborators [1] confirmed the viability of the beam model proposed by Scheuer [2], and Blandford and Rees [3] one decade before to explain the powering of lobes of extended radio sources and quasars (classic doubles or symmetric doubles, as these sources were known at those dates). -
List of Symbols
Appendix A List of Symbols For convenience, many symbols frequently used in the text are listed below alphabetically. Some of the symbols may play a dual role, in which case the meaning should be obvious from the context. A number in parentheses refers to an Eq. number (or the text or footnote near that Eq. number) in which the symbol is defined or appears for the first time; in a few cases a page number, Table number, Sect. number, footnote (fn.) number, or Fig. number is given instead. Quantum number is abbreviated as q. n. Quantum numbers (atomic): Symbol Description Eq. No. j D l ˙ s Inner q. n. of an electron (3.13) J D L C S Inner (total angular momentum) q. n. of a state (5.51b) l P Azimuthal (orbital) q. n. of an electron (3.1) and (3.2) L D l Azimuthal (orbital) q. n. of a state (5.51c) ml Magnetic orbital q. n. of an electron (3.1) ms Magnetic spin q. n. of an electron (3.1) M Total magnetic q. n. (5.51d) n Principal q. n. of an electron (3.1) s P Spin q. n. of an electron (3.13) S D s Spin q. n. of a state (5.51e) Relativistic azimuthal q. n. of an electron (3.15a) and (3.15b) Relativistic magnetic q. n. of an electron (3.18a) and (3.18b) W.F. Huebner and W.D. Barfield, Opacity, Astrophysics and Space Science Library 402, 457 DOI 10.1007/978-1-4614-8797-5, © Springer Science+Business Media New York 2014 458 Appendix A: List of Symbols Quantum numbers (molecular)1: Symbol Description Eq. -
Information Bulletin on Variable Stars
COMMISSIONS AND OF THE I A U INFORMATION BULLETIN ON VARIABLE STARS Nos April November EDITORS L SZABADOS K OLAH TECHNICAL EDITOR A HOLL TYPESETTING MB POCS ADMINISTRATION Zs KOVARI EDITORIAL BOARD E Budding HW Duerb eck EF Guinan P Harmanec chair D Kurtz KC Leung C Maceroni NN Samus advisor C Sterken advisor H BUDAPEST XI I Box HUNGARY URL httpwwwkonkolyhuIBVSIBVShtml HU ISSN 2 IBVS 4701 { 4800 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 IBVS 4701 { 4800 3 CONTENTS WOLFGANG MOSCHNER ENRIQUE GARCIAMELENDO GSC A New Variable in the Field of V Cassiop eiae :::::::::: JM GOMEZFORRELLAD E GARCIAMELENDO J GUARROFLO J NOMENTORRES J VIDALSAINZ Observations of Selected HIPPARCOS Variables ::::::::::::::::::::::::::: JM GOMEZFORRELLAD HD a New Low Amplitude Variable Star :::::::::::::::::::::::::: ME VAN DEN ANCKER AW VOLP MR PEREZ D DE WINTER NearIR Photometry and Optical Sp ectroscopy of the Herbig Ae Star AB Au rigae ::::::::::::::::::::::::::::::::::::::::::::::::::: -
Extrasolar Planets
Extrasolar Planets Edited by Rudolf Dvorak Related Titles S.N. Shore Astrophysical Hydrodynamics An Introduction 2007 ISBN 978-3-527-40669-2 M. Salaris Evolution of Stars and Stellar Populations 2005 E-Book ISBN: 978-0-470-09222-4 S.N. Shore The Tapestry of Modern Astrophysics 2003 ISBN 978-0-471-16816-4 Extrasolar Planets Formation, Detection and Dynamics Edited by Rudolf Dvorak WILEY-VCH Verlag GmbH & Co. KGaA The Editor All books published by Wiley-VCH are carefully produced. Nevertheless, authors, editors, and publisher do not warrant the information contained in these Prof. Dr. Rudolf Dvorak books, including this book, to be free of errors. Readers University of Vienna are advised to keep in mind that statements, data, illustrations, procedural details or other items may Institute for Astronomy inadvertently be inaccurate. Tuerkenschanzstrasse 17 1180 Wien Library of Congress Card No.: applied for Austria British Library Cataloguing-in-Publication Data A catalogue record for this book is available from the British Library. Bibliographic information published by the Deutsche Nationalbibliothek Die Deutsche Nationalbibliothek lists this publication in the Deutsche Nationalbibliografie; detailed bibliographic data are available on the Internet at http://dnb.d-nb.de ¤ 2008 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim All rights reserved (including those of translation into other languages). No part of this book may be reproduced in any form – by photoprinting, microfilm, or any other means – nor transmitted or translated into a machine language without written permission from the publishers. Registered names, trademarks, etc. used in this book, even when not specifically marked as such, are not to be considered unprotected by law. -