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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. -
COURSE NAME CITY STATE ALBERTVILLE GOLF & COUNTRY CLUB Albertville Alabama MOUNTAIN VIEW GOLF COURSE Alden Alabama LAKEWINDS
COURSE NAME CITY STATE ALBERTVILLE GOLF & COUNTRY CLUB Albertville Alabama MOUNTAIN VIEW GOLF COURSE Alden Alabama LAKEWINDS GOLF COURSE Alex City Alabama WILLOW POINT COUNTRY CLUB Alex City Alabama ALPINE BAY GOLF CLUB Alpine Alabama WHIPPORWHILL GOLF COURSE Altoona Alabama ANDALUSIA COUNTRY CLUB Andalusia Alabama EVANS BARNES GOLF COURSE Andalusia Alabama ANDERSON CREEK GOLF COURSE Anderson Alabama ANNISTON COUNTRY CLUB Anniston Alabama ANNISTON MUNICIPAL GOLF COURSE Anniston Alabama B & J GOLF CENTER Anniston Alabama CANE CREEK GOLF COURSE Anniston Alabama CIDER RIDGE GOLF CLUB Anniston Alabama INDIAN OAKS GOLF CLUB Anniston Alabama PINE HILL COUNTRY CLUB Anniston Alabama BROOKSIDE GOLF COURSE Arab Alabama TWIN LAKES GOLF CLUB Arab Alabama UNION SPRINGS COUNTRY CLUB Armstrong Alabama CLAY COUNTY PUBLIC GOLF COURSE Ashland Alabama ATHENS GOLF & COUNTRY CLUB Athens Alabama CANEBRAKE GOLF CLUB Athens Alabama CHRISWOOD GOLF COURSE Athens Alabama SOUTHERN GALES GOLF CLUB Athens Alabama WOODLAND GOLF COURSE Athens Alabama ATMORE COUNTRY CLUB Atmore Alabama WILLS CREEK COUNTRY CLUB Attalla Alabama AUBURN LINKS AT MILL CREEK Auburn Alabama INDIAN PINES RECREATIONAL AUTHORITY Auburn Alabama MOORE'S MILL GOLF CLUB Auburn Alabama MOORE'S MILL GOLF CLUB Auburn Alabama PIN OAKS GOLF CLUB Auburn Alabama EUFAULA COUNTRY CLUB Bakerhill Alabama LAKEPOINT RESORT GOLF COURSE Bakerhill Alabama RED EAGLE GOLF COURSE Bakerhill Alabama WARRIOR POINT GOLF CLUB Barney Alabama HOLLY HILLS COUNTRY CLUB Bay Minette Alabama BENT BROOK GOLF COURSE Bess Alabama -
IAU Division C Working Group on Star Names 2019 Annual Report
IAU Division C Working Group on Star Names 2019 Annual Report Eric Mamajek (chair, USA) WG Members: Juan Antonio Belmote Avilés (Spain), Sze-leung Cheung (Thailand), Beatriz García (Argentina), Steven Gullberg (USA), Duane Hamacher (Australia), Susanne M. Hoffmann (Germany), Alejandro López (Argentina), Javier Mejuto (Honduras), Thierry Montmerle (France), Jay Pasachoff (USA), Ian Ridpath (UK), Clive Ruggles (UK), B.S. Shylaja (India), Robert van Gent (Netherlands), Hitoshi Yamaoka (Japan) WG Associates: Danielle Adams (USA), Yunli Shi (China), Doris Vickers (Austria) WGSN Website: https://www.iau.org/science/scientific_bodies/working_groups/280/ WGSN Email: [email protected] The Working Group on Star Names (WGSN) consists of an international group of astronomers with expertise in stellar astronomy, astronomical history, and cultural astronomy who research and catalog proper names for stars for use by the international astronomical community, and also to aid the recognition and preservation of intangible astronomical heritage. The Terms of Reference and membership for WG Star Names (WGSN) are provided at the IAU website: https://www.iau.org/science/scientific_bodies/working_groups/280/. WGSN was re-proposed to Division C and was approved in April 2019 as a functional WG whose scope extends beyond the normal 3-year cycle of IAU working groups. The WGSN was specifically called out on p. 22 of IAU Strategic Plan 2020-2030: “The IAU serves as the internationally recognised authority for assigning designations to celestial bodies and their surface features. To do so, the IAU has a number of Working Groups on various topics, most notably on the nomenclature of small bodies in the Solar System and planetary systems under Division F and on Star Names under Division C.” WGSN continues its long term activity of researching cultural astronomy literature for star names, and researching etymologies with the goal of adding this information to the WGSN’s online materials. -
Mètodes De Detecció I Anàlisi D'exoplanetes
MÈTODES DE DETECCIÓ I ANÀLISI D’EXOPLANETES Rubén Soussé Villa 2n de Batxillerat Tutora: Dolors Romero IES XXV Olimpíada 13/1/2011 Mètodes de detecció i anàlisi d’exoplanetes . Índex - Introducció ............................................................................................. 5 [ Marc Teòric ] 1. L’Univers ............................................................................................... 6 1.1 Les estrelles .................................................................................. 6 1.1.1 Vida de les estrelles .............................................................. 7 1.1.2 Classes espectrals .................................................................9 1.1.3 Magnitud ........................................................................... 9 1.2 Sistemes planetaris: El Sistema Solar .............................................. 10 1.2.1 Formació ......................................................................... 11 1.2.2 Planetes .......................................................................... 13 2. Planetes extrasolars ............................................................................ 19 2.1 Denominació .............................................................................. 19 2.2 Història dels exoplanetes .............................................................. 20 2.3 Mètodes per detectar-los i saber-ne les característiques ..................... 26 2.3.1 Oscil·lació Doppler ........................................................... 27 2.3.2 Trànsits -
Stellar Variability of the Exoplanet Hosting Star Hd 63454
The Astrophysical Journal, 737:58 (5pp), 2011 August 20 doi:10.1088/0004-637X/737/2/58 C 2011. The American Astronomical Society. All rights reserved. Printed in the U.S.A. STELLAR VARIABILITY OF THE EXOPLANET HOSTING STAR HD 63454 Stephen R. Kane1, Diana Dragomir1,2, David R. Ciardi1, Jae-Woo Lee3, Gaspare Lo Curto4, Christophe Lovis5, Dominique Naef5, Suvrath Mahadevan6,7, Genady Pilyavsky6, Stephane Udry5, Xuesong Wang6, and Jason Wright6,7 1 NASA Exoplanet Science Institute, Caltech, MS 100-22, 770 South Wilson Avenue, Pasadena, CA 91125, USA; [email protected] 2 Department of Physics & Astronomy, University of British Columbia, Vancouver, BC V6T1Z1, Canada 3 Department of Astronomy & Space Science, Sejong University, 143-747 Seoul, Republic of Korea 4 ESO, Karl-Schwarzschild Strasse, 2, Garching bei Munchen,¨ Germany 5 Observatoire de Geneve,` UniversitedeGen´ eve,` 51 ch.des Maillettes, 1290 Sauverny, Switzerland 6 Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USA 7 Center for Exoplanets & Habitable Worlds, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USA Received 2011 April 23; accepted 2011 May 27; published 2011 August 3 ABSTRACT Of the hundreds of exoplanets discovered using the radial velocity (RV) technique, many are orbiting close to their host stars with periods less than 10 days. One of these, HD 63454, is a young active K dwarf which hosts a Jovian planet in a 2.82 day period orbit. The planet has a 14% transit probability and a predicted transit depth of 1.2%. Here we provide a re-analysis of the RV data to produce an accurate transit ephemeris. -
Problem Set 2 Due: 3 Feb 2012
Astronomy 62 Ann Esin Introduction to Astrophysics 27 Jan 2012 Problem Set 2 Due: 3 Feb 2012 Please staple 1+2 and 3+4. 1. Planet Around HD 63454 HD 63454 is a 0:7M star known to have an extrasolar planet orbit- ing it in a circular orbit with an or- bital period of 2.82 days. The dis- tance to this system is 35.8 pc and the measured radial velocity curve for HD 63454 is shown in Figure 1. Use this information to determine: (a) the minimum mass of the planet; (b) the radii of the star's and the planet's orbits; (c) the maximum astrometric shift Figure 1: The radial velocity of HD 63454 plotted as a of the star due to its orbital mo- function of orbital phase. (Figure from Moutou et al. tion, expressed in arcseconds. 2005, A&A, 439, 367.) 2. Sun-Jupiter System (a) Assuming that the Sun interacts only with Jupiter, calculate the total orbital angular momentum of the Sun-Jupiter system. The semi-major axis of Jupiter's orbit is a = 5:2 AU, its orbital eccentricity is e = 0:048, and its orbital period is P = 11:86 yr. (b) Starting with the cross product definition of angular momentum, prove that in a binary system L M 1 = 2 ; (1) L2 M1 where L1 and L2 are the contributions of the two masses to the total orbital angular mo- mentum of the Sun-Jupiter system. (c) Use your results from parts (a) and (b) to calculate the Sun's and Jupiter's contributions to the total orbital angular momentum of the Sun-Jupiter system. -
IAU WGSN 2019 Annual Report
IAU Division C Working Group on Star Names 2019 Annual Report Eric Mamajek (chair, USA) WG Members: Juan Antonio Belmote Avilés (Spain), Sze-leung Cheung (Thailand), Beatriz García (Argentina), Steven Gullberg (USA), Duane Hamacher (Australia), Susanne M. Hoffmann (Germany), Alejandro López (Argentina), Javier Mejuto (Honduras), Thierry Montmerle (France), Jay Pasachoff (USA), Ian Ridpath (UK), Clive Ruggles (UK), B.S. Shylaja (India), Robert van Gent (Netherlands), Hitoshi Yamaoka (Japan) WG Associates: Danielle Adams (USA), Yunli Shi (China), Doris Vickers (Austria) WGSN Website: https://www.iau.org/science/scientific_bodies/working_groups/280/ WGSN Email: [email protected] The Working Group on Star Names (WGSN) consists of an international group of astronomers with expertise in stellar astronomy, astronomical history, and cultural astronomy who research and catalog proper names for stars for use by the international astronomical community, and also to aid the recognition and preservation of intangible astronomical heritage. The Terms of Reference and membership for WG Star Names (WGSN) are provided at the IAU website: https://www.iau.org/science/scientific_bodies/working_groups/280/. WGSN was re-proposed to Division C and was approved in April 2019 as a functional WG whose scope extends beyond the normal 3-year cycle of IAU working groups. The WGSN was specifically called out on p. 22 of IAU Strategic Plan 2020-2030: “The IAU serves as the internationally recognised authority for assigning designations to celestial bodies and their surface features. To do so, the IAU has a number of Working Groups on various topics, most notably on the nomenclature of small bodies in the Solar System and planetary systems under Division F and on Star Names under Division C.” WGSN continues its long term activity of researching cultural astronomy literature for star names, and researching etymologies with the goal of adding this information to the WGSN’s online materials. -
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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. -
License Fee Distribution by Municipality
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IV. Three Close-In Planets Around HD 2638, HD 27894 and HD 63454
A&A 439, 367–373 (2005) Astronomy DOI: 10.1051/0004-6361:20052826 & c ESO 2005 Astrophysics The HARPS search for southern extra-solar planets IV. Three close-in planets around HD 2638, HD 27894 and HD 63454 C. Moutou1, M. Mayor2, F. Bouchy1,C.Lovis2,F.Pepe2,D.Queloz2,N.C.Santos3,S.Udry2,W.Benz4, G. Lo Curto5, D. Naef2,5, D. Ségransan2, and J.-P. Sivan1 1 Laboratoire d’Astrophysique de Marseille, Traverse du Siphon, 13376 Marseille Cedex 12, France e-mail: [email protected] 2 Observatoire de Genève, 51 ch. des Maillettes, 1290 Sauverny, Switzerland 3 Centro de Astronomia e Astrofísica da Universidade de Lisboa, Observatório Astronómico de Lisboa, Tapada da Ajuda, 1349-018 Lisboa, Portugal 4 Physikalisches Institut Universität Bern, Sidlerstrasse 5, 3012 Bern, Switzerland 5 ESO, Alonso de Cordoba 3107, Vitacura Casilla 19001, Santiago, Chile Received 7 February 2005 / Accepted 22 March 2005 Abstract. We report the discovery of three new planets, detected through Doppler measurements with the instrument installed on the ESO 3.6 m telescope, La Silla, Chile. These planets are orbiting the main-sequence stars HD 2638, HD 27894, and HD 63454. The orbital characteristics that best fit the observed data are depicted in this paper, as well as the stellar and plan- etary parameters. The planets’ minimum mass is 0.48, 0.62, and 0.38 MJup for respectively HD 2638, HD 27894, and HD 63454; the orbital periods are 3.4442, 17.991, and 2.817822 days, corresponding to semi-major axis of 0.044, 0.122, and 0.036 AU, respectively. -
Annual Report Publications 2011
Publications Publications in refereed journals based on ESO data (2011) The ESO Library maintains the ESO Telescope Bibliography (telbib) and is responsible for providing paper-based statistics. Access to the database for the years 1996 to present as well as information on basic publication statistics are available through the public interface of telbib (http://telbib.eso.org) and from the “Basic ESO Publication Statistics” document (http://www.eso.org/sci/libraries/edocs/ESO/ESOstats.pdf), respectively. In the list below, only those papers are included that are based on data from ESO facilities for which observing time is evaluated by the Observing Programmes Committee (OPC). Publications that use data from non-ESO telescopes or observations obtained during ‘private’ observing time are not listed here. Absil, O., Le Bouquin, J.-B., Berger, J.-P., Lagrange, A.-M., Chauvin, G., Alecian, E., Kochukhov, O., Neiner, C., Wade, G.A., de Batz, B., Lazareff, B., Zins, G., Haguenauer, P., Jocou, L., Kern, P., Millan- Henrichs, H., Grunhut, J.H., Bouret, J.-C., Briquet, M., Gagne, M., Gabet, R., Rochat, S., Traub, W., 2011, Searching for faint Naze, Y., Oksala, M.E., Rivinius, T., Townsend, R.H.D., Walborn, companions with VLTI/PIONIER. I. Method and first results, A&A, N.R., Weiss, W., Mimes Collaboration, M.C., 2011, First HARPSpol 535, 68 discoveries of magnetic fields in massive stars, A&A, 536, L6 Adami, C., Mazure, A., Pierre, M., Sprimont, P.G., Libbrecht, C., Allen, D.M. & Porto de Mello, G.F. 2011, Mn, Cu, and Zn abundances in Pacaud, F.,