Shakespeare and the Modern Stage
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Apus Constellation Visible at Latitudes Between +5° and -90°
Apus Constellation Visible at latitudes between +5° and -90°. Best visible at 21:00 (9 p.m.) during the month of July. Apus is a small constellation in the southern sky. It represents a bird-of-paradise, and its name means "without feet" in Greek because the bird-of-paradise was once wrongly believed to lack feet. First depicted on a celestial globe by Petrus Plancius in 1598, it was charted on a star atlas by Johann Bayer in his 1603 Uranometria. The French explorer and astronomer Nicolas Louis de Lacaille charted and gave the brighter stars their Bayer designations in 1756. The five brightest stars are all reddish in hue. Shading the others at apparent magnitude 3.8 is Alpha Apodis, an orange giant that has around 48 times the diameter and 928 times the luminosity of the Sun. Marginally fainter is Gamma Apodis, another ageing giant star. Delta Apodis is a double star, the two components of which are 103 arcseconds apart and visible with the naked eye. Two star systems have been found to have planets. Apus was one of twelve constellations published by Petrus Plancius from the observations of Pieter Dirkszoon Keyser and Frederick de Houtman who had sailed on the first Dutch trading expedition, known as the Eerste Schipvaart, to the East Indies. It first appeared on a 35-cm diameter celestial globe published in 1598 in Amsterdam by Plancius with Jodocus Hondius. De Houtman included it in his southern star catalogue in 1603 under the Dutch name De Paradijs Voghel, "The Bird of Paradise", and Plancius called the constellation Paradysvogel Apis Indica; the first word is Dutch for "bird of paradise". -
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. -
A Search for Variability and Transit Signatures In
A SEARCH FOR VARIABILITY AND TRANSIT SIGNATURES IN HIPPARCOS PHOTOMETRIC DATA A thesis presented to the faculty of 3 ^ San Francisco State University Zo\% In partial fulfilment of W* The Requirements for The Degree Master of Science In Physics: Astronomy by Badrinath Thirumalachari San JVancisco, California December 2018 Copyright by Badrinath Thirumalachari 2018 CERTIFICATION OF APPROVAL I certify that I have read A SEARCH FOR VARIABILITY AND TRANSIT SIGNATURES IN HIPPARCOS PHOTOMETRIC DATA by Badrinath Thirumalachari and that in my opinion this work meets the criteria for approving a thesis submitted in partial fulfillment of the requirements for the degree: Master of Science in Physics: Astronomy at San Francisco State University. fov- Dr. Stephen Kane, Ph.D. Astrophysics Associate Professor of Planetary Astrophysics Dr. Uo&eph Barranco, Ph.D. .%trtJphysics Chairfe Associate Professor of Physics K + A Q , L a . Dr. Ron Marzke, Ph.D. Astronomy Assoc. Dean of College of Science & Engineering A SEARCH FOR VARIABILITY AND TRANSIT SIGNATURES IN HIPPARCOS PHOTOMETRIC DATA Badrinath Thirumalachari San Francisco State University 2018 The study and characterization of exoplanets has picked up pace rapidly over the past few decades with the invention of newer techniques and instruments. Detecting transits in stellar photometric data around stars already known to harbor exoplanets is crucial for exoplanet characterization. Due to these advancements we now have oceans of data and coming up with an automated way of performing exoplanet characterization is a challenge. In this thesis I describe one such method to search for transits in Hipparcos dataset containing photometric data for over 118000 stars. The radial velocity method has discovered a lot of planets around bright host stars and a follow up transit detection will give us the density of the exoplanet. -
2017 Publication Year 2020-08-04T11:06:43Z Acceptance
Publication Year 2017 Acceptance in OA@INAF 2020-08-04T11:06:43Z Title Searching for chemical signatures of brown dwarf formation Authors MALDONADO PRADO, Jesus; Villaver, E. DOI 10.1051/0004-6361/201630120 Handle http://hdl.handle.net/20.500.12386/26692 Journal ASTRONOMY & ASTROPHYSICS Number 602 A&A 602, A38 (2017) DOI: 10.1051/0004-6361/201630120 Astronomy c ESO 2017 & Astrophysics Searching for chemical signatures of brown dwarf formation? J. Maldonado1 and E. Villaver2 1 INAF–Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy e-mail: [email protected] 2 Universidad Autónoma de Madrid, Dpto. Física Teórica, Módulo 15, Facultad de Ciencias, Campus de Cantoblanco, 28049 Madrid, Spain Received 22 November 2016 / Accepted 9 February 2017 ABSTRACT Context. Recent studies have shown that close-in brown dwarfs in the mass range 35–55 MJup are almost depleted as companions to stars, suggesting that objects with masses above and below this gap might have di↵erent formation mechanisms. Aims. We aim to test whether stars harbouring massive brown dwarfs and stars with low-mass brown dwarfs show any chemical peculiarity that could be related to di↵erent formation processes. Methods. Our methodology is based on the analysis of high-resolution échelle spectra (R 57 000) from 2–3 m class telescopes. We determine the fundamental stellar parameters, as well as individual abundances of C, O,⇠ Na, Mg, Al, Si, S, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, and Zn for a large sample of stars known to have a substellar companion in the brown dwarf regime. -
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. -
Determining the True Mass of Radial-Velocity Exoplanets with Gaia F
Determining the true mass of radial-velocity exoplanets with Gaia F. Kiefer, G. Hébrard, A. Lecavelier Des Etangs, E. Martioli, S. Dalal, A. Vidal-Madjar To cite this version: F. Kiefer, G. Hébrard, A. Lecavelier Des Etangs, E. Martioli, S. Dalal, et al.. Determining the true mass of radial-velocity exoplanets with Gaia: Nine planet candidates in the brown dwarf or stellar regime and 27 confirmed planets. Astronomy and Astrophysics - A&A, EDP Sciences, 2021, 645, pp.A7. 10.1051/0004-6361/202039168. hal-03085694 HAL Id: hal-03085694 https://hal.archives-ouvertes.fr/hal-03085694 Submitted on 21 Dec 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. A&A 645, A7 (2021) Astronomy https://doi.org/10.1051/0004-6361/202039168 & © F. Kiefer et al. 2020 Astrophysics Determining the true mass of radial-velocity exoplanets with Gaia Nine planet candidates in the brown dwarf or stellar regime and 27 confirmed planets? F. Kiefer1,2, G. Hébrard1,3, A. Lecavelier des Etangs1, E. Martioli1,4, S. Dalal1, and A. Vidal-Madjar1 1 Institut d’Astrophysique de Paris, Sorbonne -
1 I Articles Dans Des Revues Avec Comité De Lecture
1 I Articles dans des revues avec comité de lecture (ACL) internationales II Articles dans des revues sans comité de lecture (SCL) NB : La liste des publications est donnée de façon exhautive par équipe, ce qui signifie qu’il existe des redondances chaque fois qu’une publication est cosignée pas des membres dépendant d’équipes différentes. Par contre, certains chercheurs sont à cheval sur deux équipes, dans ce cas il leur a été demandé de rattacher leurs publications seulement à l’une ou à l’autre équipe en fonction de la nature de la publication et la raison de leur rattachement à deux équipes. I Articles dans des revues avec comité de lecture (ACL) internationales ANNÉE 2006 A / Equipe « Physique des galaxies » 1. Aguilar, J.A. et al. (the ANTARES collaboration, 214 auteurs). First results of the Instrumentation Line for the deep- sea ANTARES neturino telescope Astroparticle Physic 26, 314 2. Auld, R.; Minchin, R. F.; Davies, J. I.; Catinella, B.; van Driel, W.; Henning, P. A.; Linder, S.; Momjian, E.; Muller, E.; O'Neil, K.; Boselli, A.; et 18 coauteurs. The Arecibo Galaxy Environment Survey: precursor observations of the NGC 628 group, 2006, MNRAS,.371,1617A 3. Boselli, A.; Boissier, S.; Cortese, L.; Gil de Paz, A.; Seibert, M.; Madore, B. F.; Buat, V.; Martin, D. C. The Fate of Spiral Galaxies in Clusters: The Star Formation History of the Anemic Virgo Cluster Galaxy NGC 4569, 2006, ApJ, 651, 811B 4. Boselli, A.; Gavazzi, G. Environmental Effects on Late-Type Galaxies in Nearby Clusters -2006, PASP, 118, 517 5. -
Shakespeare and the Modern Stage, with Other Essays
SHAKESPEARE AND THE MODERN STAGE .SHAKESPEARE AND THE MODERN STAGE WITH OTHER ESSAYS BY SIDNEY LEE ATJTHOE OF " GKEAT ENGLISHMEN OF THE SIXTEENTH CENTURY, "a LIFE OF WILLIAM SHAKESPEARE," ETC. NEW YORK CHARLES SCRIBNER'S SONS 1906 5> COPYBIGHT, 1900, BY CHARLES SCRIBNEE'.S SONS Published, October, 1906 TROW OIRECTORV PRINTING AND BOOKBINDING COMPANr NEW YORK PREFACE The eleven papers which are collected here were written between 1899 and 1905. With the excep- tion of one, entitled ''Aspects of Shakespeare's Phil- osophy," which is now printed for the first time, all were published in periodicals in the course of those six years. The articles treat of varied aspects of Shakespearean drama, its influences and tradi- tions, but I think that all may be credited with sufficient unity of intention to warrant their com- bination in a single volume. Their main endeavour is to survey Shakespearean drama in relation to modern life, and to illustrate its Hving force in current affairs. Even in the papers which embody researches in sixteenth- or seventeenth-century dra- matic history, I have sought to keep in view the bearings of the past on the present. A large portion of the book discusses, as its title indicates, methods of representing Shakespeare on the modern stage. The attempt is there made to define, in the fight of experience, the conditions which are best calculated to conserve or increase Shakespeare's genuine vitafity in the theatre of our own day. In revising the work for the press, I have deemed it advisable to submit the papers to a somewhat rigorous verbal revision. -
Determining the True Mass of Radial-Velocity Exoplanets with Gaia 9 Planet Candidates in the Brown-Dwarf/Stellar Regime and 27 Confirmed Planets
Astronomy & Astrophysics manuscript no. exoplanet_mass_gaia c ESO 2020 September 30, 2020 Determining the true mass of radial-velocity exoplanets with Gaia 9 planet candidates in the brown-dwarf/stellar regime and 27 confirmed planets F. Kiefer1; 2, G. Hébrard1; 3, A. Lecavelier des Etangs1, E. Martioli1; 4, S. Dalal1, and A. Vidal-Madjar1 1 Institut d’Astrophysique de Paris, Sorbonne Université, CNRS, UMR 7095, 98 bis bd Arago, 75014 Paris, France 2 LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, 5 place Jules Janssen, 92195 Meudon, France? 3 Observatoire de Haute-Provence, CNRS, Universiteé d’Aix-Marseille, 04870 Saint-Michel-l’Observatoire, France 4 Laboratório Nacional de Astrofísica, Rua Estados Unidos 154, 37504-364, Itajubá - MG, Brazil Submitted on 2020/08/20 ; Accepted for publication on 2020/09/24 ABSTRACT Mass is one of the most important parameters for determining the true nature of an astronomical object. Yet, many published exoplan- ets lack a measurement of their true mass, in particular those detected thanks to radial velocity (RV) variations of their host star. For those, only the minimum mass, or m sin i, is known, owing to the insensitivity of RVs to the inclination of the detected orbit compared to the plane-of-the-sky. The mass that is given in database is generally that of an assumed edge-on system (∼90◦), but many other inclinations are possible, even extreme values closer to 0◦ (face-on). In such case, the mass of the published object could be strongly underestimated by up to two orders of magnitude. -