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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. -
Arxiv:0809.1275V2
How eccentric orbital solutions can hide planetary systems in 2:1 resonant orbits Guillem Anglada-Escud´e1, Mercedes L´opez-Morales1,2, John E. Chambers1 [email protected], [email protected], [email protected] ABSTRACT The Doppler technique measures the reflex radial motion of a star induced by the presence of companions and is the most successful method to detect ex- oplanets. If several planets are present, their signals will appear combined in the radial motion of the star, leading to potential misinterpretations of the data. Specifically, two planets in 2:1 resonant orbits can mimic the signal of a sin- gle planet in an eccentric orbit. We quantify the implications of this statistical degeneracy for a representative sample of the reported single exoplanets with available datasets, finding that 1) around 35% percent of the published eccentric one-planet solutions are statistically indistinguishible from planetary systems in 2:1 orbital resonance, 2) another 40% cannot be statistically distinguished from a circular orbital solution and 3) planets with masses comparable to Earth could be hidden in known orbital solutions of eccentric super-Earths and Neptune mass planets. Subject headings: Exoplanets – Orbital dynamics – Planet detection – Doppler method arXiv:0809.1275v2 [astro-ph] 25 Nov 2009 Introduction Most of the +300 exoplanets found to date have been discovered using the Doppler tech- nique, which measures the reflex motion of the host star induced by the planets (Mayor & Queloz 1995; Marcy & Butler 1996). The diverse characteristics of these exoplanets are somewhat surprising. Many of them are similar in mass to Jupiter, but orbit much closer to their 1Carnegie Institution of Washington, Department of Terrestrial Magnetism, 5241 Broad Branch Rd. -
Ebooksspringer Contrat 4903.07.Xls Title Editors/Authors Year Book ISBN13 Book E-ISBN13 the Abcs of Gene Cloning Wong, Dominic W
EbooksSpringer_contrat_4903.07.xls Title Editors/Authors Year Book ISBN13 Book e-ISBN13 The ABCs of Gene Cloning Wong, Dominic W.S. 2006 978-0-387-28663-1 978-0-387-28679-2 Abductive Reasoning Aliseda, Atocha 2006 978-1-4020-3906-5 978-1-4020-3907-2 Abeta Peptide and Alzheimer's Disease Barrow, Colin J; Small, David H. 2007 978-1-85233-961-6 978-1-84628-440-3 Abiotic Stress Tolerance in Plants Rai, Ashwani K.; Takabe, Teruhiro 2006 978-1-4020-4388-8 978-1-4020-4389-5 Abnormal Skeletal Phenotypes Castriota-Scanderbeg, Alessandro; 2005 978-3-540-67997-4 978-3-540-30361-9 Dallapiccola, Bruno Abord clinique des malades de l'alcool Huas, Dominique; Rueff, Bernard 2005 978-2-287-59769-5 978-2-287-28577-6 Abord clinique des urgences traumatiques au cabinet Carolet, Carole; Pire, Jean-Claude 2005 978-2-287-25170-2 978-2-287-28164-8 du généraliste Abord clinique du malade âgé Moulias, Robert 2007 978-2-287-22084-5 978-2-287-31016-4 Abord clinique en urologie Cortesse, Alain; LeDuc, Alain 2006 978-2-287-25253-2 978-2-287-48614-2 About Life Agutter, Paul S.; Wheatley, Denys N. 2007 978-1-4020-5417-4 978-1-4020-5418-1 Abstract Algebra Grillet, Pierre Antoine 2007 978-0-387-71567-4 978-0-387-71568-1 Abstract Computing Machines Kluge, W. 2005 978-3-540-21146-4 978-3-540-27359-2 Abstract Harmonic Analysis of Continuous Wavelet Führ, Hartmut 2005 978-3-540-24259-8 978-3-540-31552-0 Transforms Abstraction Refinement for Large Scale Model Hachtel, Gary D.; Somenzi, Fabio; Wang, 2006 978-0-387-34155-2 978-0-387-34600-7 Abstraction,Checking Refinement and Proof for Probabilistic McIver,Chao Annabelle; Morgan, Charles C. -
COMMISSIONS 27 and 42 of the I.A.U. INFORMATION BULLETIN on VARIABLE STARS Nos. 4101{4200 1994 October { 1995 May EDITORS: L. SZ
COMMISSIONS AND OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS Nos Octob er May EDITORS L SZABADOS and K OLAH TECHNICAL EDITOR A HOLL TYPESETTING K ORI KONKOLY OBSERVATORY H BUDAPEST PO Box HUNGARY IBVSogyallakonkolyhu URL httpwwwkonkolyhuIBVSIBVShtml HU ISSN 2 CONTENTS 1994 No page E F GUINAN J J MARSHALL F P MALONEY A New Apsidal Motion Determination For DI Herculis ::::::::::::::::::::::::::::::::::::: D TERRELL D H KAISER D B WILLIAMS A Photometric Campaign on OW Geminorum :::::::::::::::::::::::::::::::::::::::::::: B GUROL Photo electric Photometry of OO Aql :::::::::::::::::::::::: LIU QUINGYAO GU SHENGHONG YANG YULAN WANG BI New Photo electric Light Curves of BL Eridani :::::::::::::::::::::::::::::::::: S Yu MELNIKOV V S SHEVCHENKO K N GRANKIN Eclipsing Binary V CygS Former InsaType Variable :::::::::::::::::::: J A BELMONTE E MICHEL M ALVAREZ S Y JIANG Is Praesep e KW Actually a Delta Scuti Star ::::::::::::::::::::::::::::: V L TOTH Ch M WALMSLEY Water Masers in L :::::::::::::: R L HAWKINS K F DOWNEY Times of Minimum Light for Four Eclipsing of Four Binary Systems :::::::::::::::::::::::::::::::::::::::::: B GUROL S SELAN Photo electric Photometry of the ShortPeriod Eclipsing Binary HW Virginis :::::::::::::::::::::::::::::::::::::::::::::: M P SCHEIBLE E F GUINAN The Sp otted Young Sun HD EK Dra ::::::::::::::::::::::::::::::::::::::::::::::::::: ::::::::::::: M BOS Photo electric Observations of AB Doradus ::::::::::::::::::::: YULIAN GUO A New VR Cyclic Change of H in Tau :::::::::::::: -
Statistical Properties of Exoplanets
A&A 398, 363–376 (2003) Astronomy DOI: 10.1051/0004-6361:20021637 & c ESO 2003 Astrophysics Statistical properties of exoplanets II. Metallicity, orbital parameters, and space velocities N. C. Santos1, G. Israelian2, M. Mayor1,R.Rebolo2,3,andS.Udry1 1 Observatoire de Gen`eve, 51 ch. des Maillettes, 1290 Sauverny, Switzerland 2 Instituto de Astrof´ısica de Canarias, 38200 La Laguna, Tenerife, Spain 3 Consejo Superior de Investigaciones Cient´ıficas, Spain Received 19 September 2002 / Accepted 7 November 2002 Abstract. In this article we present a detailed spectroscopic analysis of more than 50 extra-solar planet host stars. Stellar atmospheric parameters and metallicities are derived using high resolution and high S/N spectra. The spectroscopy results, added to the previous studies, imply that we have access to a large and uniform sample of metallicities for about 80 planet hosts stars. We make use of this sample to confirm the metal-rich nature of stars with planets, and to show that the planetary frequency is rising as a function of the [Fe/H]. Furthermore, the source of this high metallicity is shown to have most probably a “primordial” source, confirming previous results. The comparison of the orbital properties (period and eccentricity) and minimum masses of the planets with the stellar properties also reveal some emerging but still not significant trends. These are discussed and some explanations are proposed. Finally, we show that the planet host stars included in the CORALIE survey have similar kinematical properties as the whole CORALIE volume-limited planet search sample. Planet hosts simply seem to occupy the metal-rich envelope of this latter population. -
KP Funds Form N-Q Filed 2017-05-30
SECURITIES AND EXCHANGE COMMISSION FORM N-Q Quarterly schedule of portfolio holdings of registered management investment company filed on Form N-Q Filing Date: 2017-05-30 | Period of Report: 2017-03-31 SEC Accession No. 0001193125-17-187477 (HTML Version on secdatabase.com) FILER KP Funds Mailing Address Business Address ONE FREEDOM VALLEY ONE FREEDOM VALLEY CIK:1573386| IRS No.: 000000000 | State of Incorp.:MA DRIVE DRIVE Type: N-Q | Act: 40 | File No.: 811-22838 | Film No.: 17877909 OAKS PA 19456 OAKS PA 19456 (800) 342-5734 Copyright © 2017 www.secdatabase.com. All Rights Reserved. Please Consider the Environment Before Printing This Document UNITED STATES SECURITIES AND EXCHANGE COMMISSION Washington, D.C. 20549 FORM N-Q QUARTERLY SCHEDULE OF PORTFOLIO HOLDINGS OF REGISTERED MANAGEMENT INVESTMENT COMPANY Investment Company Act file number 811-22838 The KP Funds (Exact name of registrant as specified in charter) CT Corporation 101 Federal Street Boston, MA 02110 (Address of principal executive offices) (Zip code) SEI Investments One Freedom Valley Drive Oaks, PA 19456 (Name and address of agent for service) Registrants telephone number, including area code: 800-342-5734 Date of fiscal year end: December 31, 2017 Date of reporting period: March 31, 2017 Copyright © 2017 www.secdatabase.com. All Rights Reserved. Please Consider the Environment Before Printing This Document Item 1. Schedules of Investments Copyright © 2017 www.secdatabase.com. All Rights Reserved. Please Consider the Environment Before Printing This Document KP Retirement -
Filing Port Code Filing Port Name Manifest Number Filing Date Last Domestic Port Vessel Name Last Foreign Port Call Sign Number
Filing Last Port Call Sign Foreign Trade Official Voyage Vessel Type Dock Code Filing Port Name Manifest Number Filing Date Last Domestic Port Vessel Name Last Foreign Port Number IMO Number Country Code Number Number Vessel Flag Code Agent Name PAX Total Crew Operator Name Draft Tonnage Owner Name Dock Name InTrans 2704 LOS ANGELES, CA 2704-2021-00295 12/11/2020 - PRESIDENT KENNEDY BUSAN WPKW 9295218 KR 3 1284572. 23 US 310 NORTON LILLY INT'L AGENCY 0 22 APL MARITIME LTD 42'4" 48047 PRESIDENT KENNEDY TRUST LOS ANGELES BERTH 304 DL 4122 ASHTABULA/CONNEAUT 4122-2021-00027 12/11/2020 - CSL TADOUSSAC PORT COLBORNE, ONT VDWB 6918716 CA 1 325750 039 CA 229 PICKANDS & MATHER LAKE SERVICES 0 24 V-SHIPS CANADA INC. 25'2" 6030 THE CSL GROUP INC. THE PITTSBURGH & CONNEAUT DOCK NO 4 (R IRON ORE) L 1303 BALTIMORE, MD 1303-2021-00369 12/11/2020 - VIKING QUEEN EX. HOEGH DELHI VERACRUZ 9V2633 9318462 MX 3 399246 0047h SG 333 CAPES SHIPPING AGENCIES, INC. 0 20 OSM SHIP MANAGEMENT PTE. LTD. 35'6" 21359 GCC (CUE) SHIPPING PTE. LTD. ANNAPOLIS ANCHORAGE SHIPSIDE DFL 1303 BALTIMORE, MD 1303-2021-00371 12/11/2020 NORFOLK, VA GUNDE MAERSK - OUIY2 9359014 - 6 D4249 001 DK 310 NORTON LILLY INT., INC. 0 21 MAERSK LINE A/S 42'9" 57019 MAERSK LINE A/S SEAGIRT MARINE TERMINAL DFLX 1511 BEAUFORT-MOREHEAD CTY,NC 1511-2021-00015 12/11/2020 - NIOVI.GR SAN PEDRO V7A2644 9827322 AR 2 90556 306 MH 229 Terminal Shipping (Wilmington/Morehead City) 0 18 M/MARITIME CORP. -
A Link Between the Semimajor Axis of Extrasolar Gas Giant Planets and Stellar Metallicity
Mon. Not. R. Astron. Soc. 364, 29–36 (2005) doi:10.1111/j.1365-2966.2005.09491.x A link between the semimajor axis of extrasolar gas giant planets and stellar metallicity , R. Pinotti,1,2 L. Arany-Prado,1 W. Lyra1 3 and G. F. Porto de Mello1 1Observatorio´ do Valongo, Universidade Federal do Rio de Janeiro, Lad. Pedro Antonioˆ 43, RJ, 20080-090, Brazil 2PETROBRAS, REDUC/OT, Rod. Washington Luiz km 113,7, Duque de Caxias, RJ, 25225-010, Brazil 3Department of Astronomy & Space Physics, Uppsala Astronomical Observatory, Box 515, 751 20, Sweden Accepted 2005 August 1. Received 2005 July 14; in original form 2005 January 14 Downloaded from ABSTRACT The fact that most extrasolar planets found to date are orbiting metal-rich stars lends credence to the core accretion mechanism of gas giant planet formation over its competitor, the disc instability mechanism. However, the core accretion mechanism is not refined to the point of explaining orbital parameters such as the unexpected semimajor axes and eccentricities. We http://mnras.oxfordjournals.org/ propose a model that correlates the metallicity of the host star with the original semimajor axis of its most massive planet, prior to migration, assuming that the core accretion scenario governs giant gas planet formation. The model predicts that the optimum regions for planetary formation shift inwards as stellar metallicity decreases, providing an explanation for the observed absence of long-period planets in metal-poor stars. We compare our predictions with the available data on extrasolar planets for stars with masses similar to the mass of the Sun. -
The Anglo-Australian Planet Search XXIV: the Frequency of Jupiter
The Anglo-Australian Planet Search XXIV: The Frequency of Jupiter Analogs Robert A. Wittenmyer1,2,3, R.P. Butler4, C.G. Tinney1,2, Jonathan Horner3,2, B.D. Carter3, D.J. Wright1,2, H.R.A. Jones5, J. Bailey1,2, Simon J. O’Toole6 [email protected] ABSTRACT We present updated simulations of the detectability of Jupiter analogs by the 17- year Anglo-Australian Planet Search. The occurrence rate of Jupiter-like planets that have remained near their formation locations beyond the ice line is a critical datum necessary to constrain the details of planet formation. It is also vital in our quest to fully understand how common (or rare) planetary systems like our own are in the Galaxy. From a sample of 202 solar-type stars, and correcting for +2.8 imperfect detectability on a star-by-star basis, we derive a frequency of 6.2−1.6% for giant planets in orbits from 3-7 AU. When a consistent definition of “Jupiter analog” is used, our results are in agreement with those from other legacy radial velocity surveys. Subject headings: planetary systems — techniques: radial velocities 1. Introduction Much attention has been brought to bear in recent years on the occurrence rate of Earth-like planets (e.g. Howard et al. 2012; Wittenmyer et al. 2011b; Kopparapu 2013). arXiv:1601.05465v1 [astro-ph.EP] 20 Jan 2016 1School of Physics, University of New South Wales, Sydney 2052, Australia 2Australian Centre for Astrobiology, University of New South Wales, Sydney 2052, Australia 3Computational Engineering and Science Research Centre, University of Southern Queensland, Toowoomba, Queensland 4350, Australia 4Department of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road, NW, Washington, DC 20015-1305, USA 5Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield, Herts AL10 9AB, UK 6Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia –2– This is due in large part to the flood of data from the Kepler spacecraft mission, which has provided evidence that small planets are exceedingly common (e.g. -
1 Mass Loss of Highly Irradiated Extra-Solar
Mass Loss of Highly Irradiated Extra-Solar Giant Planets Item Type text; Electronic Thesis Authors Hattori, Maki Publisher The University of Arizona. Rights Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author. Download date 06/10/2021 10:24:45 Link to Item http://hdl.handle.net/10150/193323 1 Mass Loss of Highly Irradiated Extra-Solar Giant Planets by Maki Funato Hattori _____________________ A Thesis Submitted to the Faculty of the DEPARTMENT OF PLANETARY SCIENCES In Partial Fulfillment of the Requirements For the Degree of MASTER OF SCIENCE In the Graduate College THE UNIVERSITY OF ARIZONA 2008 2 STATEMENT BY AUTHOR This thesis has been submitted in partial fulfillment of requirements for an advanced degree at The University of Arizona and is deposited in the University Library to be made available to borrowers under rules of the Library. Brief quotations from this thesis are allowable without special permission, provided that accurate acknowledgment of source is made. Requests for permission for extended quotation from or reproduction of this manuscript in whole or in part may be granted by the head of the major department or the Dean of the Graduate College when in his or her judgment the proposed use of the material is in the interests of scholarship. In all other instances, however, permission must be obtained from the author. SIGNED: ________________________________ Maki F. Hattori APPROVAL BY THESIS DIRECTOR This thesis has been approved on the date shown below: _________________________________ ______7/25/08_____ Dr. -
A SUB-SATURN MASS PLANET ORBITING HD 36511 Debra A
The Astrophysical Journal, 590:1081–1087, 2003 June 20 E # 2003. The American Astronomical Society. All rights reserved. Printed in U.S.A. A SUB-SATURN MASS PLANET ORBITING HD 36511 Debra A. Fischer,2 R. Paul Butler,3 Geoffrey W. Marcy,2 Steven S. Vogt,4 and Gregory W. Henry5 Received 2003 January 5; accepted 2003 February 25 ABSTRACT We report precise Doppler velocities of HD 3651 obtained at Lick and Keck Observatories. The velocities reveal evidence of a planetary companion with an orbital period of 62:23 Æ 0:03 days, an eccentricity of À1 0:63 Æ 0:04, and a velocity semiamplitude of 15:9 Æ 1:7ms .With an assumed mass of 0.79 M for this K0 V star, we derive M sin i ¼ 0:20MJ and a semimajor axis of 0.284 AU. The star is chromospherically inactive, 0 with log RHK À5:01, and 10 years of observations at Fairborn Observatory show it to be photometrically stable to better than 0.001 mag. In particular, there is no photometric variability on the 62.23 day radial velocity period to a limit of 0.0002 mag, supporting the planetary interpretation of the radial velocity varia- bility. Photometric transits of the planetary companion across the star are ruled out with a probability of 87%. Subject headings: planetary systems — stars: individual (HD 3651, HR 166) On-line material: machine-readable table 1. INTRODUCTION ing yields Teff ¼ 5210 Æ 30 K, ½Fe=H0:05 Æ 0:05, and v sin i 1 7 0 5kmsÀ1.Based on the mass calibration More than 100 extrasolar planets6 have been discovered ¼ : Æ : tabulated in Allens Astrophysical Quantities (Drilling & orbiting solar-type stars (see references in Butler et al. -
Recovering the Colour-Dependent Albedo of Exoplanets with High-Resolution Spectroscopy: from ESPRESSO to the ELT
MNRAS 000,1{27 (2018) Preprint 6 August 2018 Compiled using MNRAS LATEX style file v3.0 Recovering the colour-dependent albedo of exoplanets with high-resolution spectroscopy: from ESPRESSO to the ELT. J. H. C. Martins1;2;3,? P. Figueira2;1, N. C. Santos1;3, C. Melo2, A. Garcia Mu~noz4, J. Faria1;3, F. Pepe5, and C. Lovis5 1Instituto de Astrof´ısica e Ci^encias do Espa¸co, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal 2European Southern Observatory, Alonso de C´ordova 3107, Vitacura, Regi´on Metropolitana, Chile 3Departamento de F´ısica e Astronomia, Faculdade de Ci^encias, Universidade do Porto, Rua do Campo Alegre, 4169-007 Porto, Portugal 4Zentrum fur¨ Astronomie und Astrophysik, Technische Universit¨at Berlin, D-10623 Berlin, Germany 5Observatoire de Gen`eve, Universit´ede Gen`eve, 51 ch. des Maillettes, CH-1290 Sauverny, Switzerland Accepted 2018 May 21. Received 2018 May 18; in original form 2017 September 8 ABSTRACT The characterization of planetary atmospheres is a daunting task, pushing current observing facilities to their limits. The next generation of high-resolution spectrographs mounted on large telescopes { such as ESPRESSO@VLT and HIRES@ELT { will allow us to probe and characterize exoplanetary atmospheres in greater detail than possible to this point. We present a method that permits the recovery of the colour-dependent reflectivity of exoplanets from high-resolution spectroscopic observations. Determining the wavelength-dependent albedo will provide insight into the chemical properties and weather of the exoplanet atmospheres. For this work, we simulated ESPRESSO@VLT and HIRES@ELT high-resolution observations of known planetary systems with several albedo configurations.