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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. -
Correlations Between the Stellar, Planetary, and Debris Components of Exoplanet Systems Observed by Herschel⋆
A&A 565, A15 (2014) Astronomy DOI: 10.1051/0004-6361/201323058 & c ESO 2014 Astrophysics Correlations between the stellar, planetary, and debris components of exoplanet systems observed by Herschel J. P. Marshall1,2, A. Moro-Martín3,4, C. Eiroa1, G. Kennedy5,A.Mora6, B. Sibthorpe7, J.-F. Lestrade8, J. Maldonado1,9, J. Sanz-Forcada10,M.C.Wyatt5,B.Matthews11,12,J.Horner2,13,14, B. Montesinos10,G.Bryden15, C. del Burgo16,J.S.Greaves17,R.J.Ivison18,19, G. Meeus1, G. Olofsson20, G. L. Pilbratt21, and G. J. White22,23 (Affiliations can be found after the references) Received 15 November 2013 / Accepted 6 March 2014 ABSTRACT Context. Stars form surrounded by gas- and dust-rich protoplanetary discs. Generally, these discs dissipate over a few (3–10) Myr, leaving a faint tenuous debris disc composed of second-generation dust produced by the attrition of larger bodies formed in the protoplanetary disc. Giant planets detected in radial velocity and transit surveys of main-sequence stars also form within the protoplanetary disc, whilst super-Earths now detectable may form once the gas has dissipated. Our own solar system, with its eight planets and two debris belts, is a prime example of an end state of this process. Aims. The Herschel DEBRIS, DUNES, and GT programmes observed 37 exoplanet host stars within 25 pc at 70, 100, and 160 μm with the sensitiv- ity to detect far-infrared excess emission at flux density levels only an order of magnitude greater than that of the solar system’s Edgeworth-Kuiper belt. Here we present an analysis of that sample, using it to more accurately determine the (possible) level of dust emission from these exoplanet host stars and thereafter determine the links between the various components of these exoplanetary systems through statistical analysis. -
Graham Pointer Phd Thesis
THE MAGNETIC FIELD OF AB DORADÛS Graham Richard Pointer A Thesis Submitted for the Degree of PhD at the University of St Andrews 2001 Full metadata for this item is available in St Andrews Research Repository at: http://research-repository.st-andrews.ac.uk/ Please use this identifier to cite or link to this item: http://hdl.handle.net/10023/12940 This item is protected by original copyright THE UNIVERSITY OF ST. ANDREWS The Magnetic Field of AB Doradûs Graham Richard Pointer Submitted for the degree of Ph.D. May 2001 ProQuest Number: 10171062 All rights reserved INFORMATION TO ALL USERS The quality of this reproduction is dependent upon the quality of the copy submitted. In the unlikely event that the author did not send a com plete manuscript and there are missing pages, these will be noted. Also, if material had to be removed, a note will indicate the deletion. uest ProQuest 10171062 Published by ProQuest LLO (2017). Copyright of the Dissertation is held by the Author. All rights reserved. This work is protected against unauthorized copying under Title 17, United States C ode Microform Edition © ProQuest LLO. ProQuest LLO. 789 East Eisenhower Parkway P.Q. Box 1346 Ann Arbor, Ml 48106- 1346 DECLARATION I, Graham Richard Pointer, hereby declare that this thesis, which is approximately 50000 words in length, has been written by me, that it is the record of work carried out by me and that it has not been submitted in any previous application for a higher degree. I was admitted as a research student in September 1997 and as a candidate for the degree of Ph.D . -
Arxiv:1809.10688V2 [Astro-Ph.EP] 26 Jun 2019 Ing Nearby Bright Stars (Howell Et Al
Preprint typeset using LATEX style emulateapj v. 12/16/11 A DISCRETE SET OF POSSIBLE TRANSIT EPHEMERIDES FOR TWO LONG PERIOD GAS GIANTS ORBITING HIP 41378 Juliette C. Becker1, Andrew Vanderburg2;?, Joseph E. Rodriguez3, Mark Omohundro4, Fred C. Adams1;5, Keivan G. Stassun6;7, Xinyu Yao8, Joel Hartman9, Joshua Pepper8, Gaspar Bakos9, Geert Barentsen10, Thomas G. Beatty11, Waqas Bhatti8, Ashley Chontos12, Andrew Collier Cameron13, Coel Hellier14, Daniel Huber12, David James3, Rudolf B. Kuhn15, Michael B. Lund6, Don Pollacco16, Robert J. Siverd6, Daniel J. Stevens11;17;18, Jose´ Vin´ıcius de Miranda Cardoso19, Richard West16, 1Astronomy Department, University of Michigan, 1085 S University Avenue, Ann Arbor, MI 48109, USA 2Department of Astronomy, The University of Texas at Austin, Austin, TX 78712, USA 3Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA 4Citizen Scientist 5Physics Department, University of Michigan, Ann Arbor, MI 48109, USA 6Department of Physics and Astronomy, Vanderbilt University, 6301 Stevenson Center, Nashville, TN:37235, USA 7Department of Physics, Fisk University, 1000 17th Avenue North, Nashville, TN:37208, USA 8Department of Physics, Lehigh University, 16 Memorial Drive East, Bethlehem, PA 18015, USA 9Department of Astrophysical Sciences, 4 Ivy Lane, Princeton University, Princeton, NJ 08544 10NASA Ames Research Center, Moffett Blvd, Mountain View, CA 94035, USA 11Center for Exoplanets and Habitable Worlds, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802 -
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. -
Arxiv:2101.08801V1 [Astro-Ph.EP] 21 Jan 2021 Target Selection and Expanded Observational Techniques Have Type Stars (Zhou Et Al
DRAFT VERSION JANUARY 25, 2021 Typeset using LATEX twocolumn style in AASTeX63 A decade of radial-velocity monitoring of Vega and new limits on the presence of planets 1 2 2 3 2 SPENCER A. HURT , SAMUEL N. QUINN , DAVID W. LATHAM , ANDREW VANDERBURG , GILBERT A. ESQUERDO , 2 2 4, 5 2 2, ∗ MICHAEL L. CALKINS , PERRY BERLIND, RUTH ANGUS , CHRISTIAN A. LATHAM, AND GEORGE ZHOU 1Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309, USA 2Center for Astrophysics | Harvard & Smithsonian, 60 Garden St, Cambridge, MA 02138, USA 3Department of Astronomy, University of Wisconsin -Madison, 475 North Charter Street, Madison, WI 53706, USA 4Department of Astrophysics, American Museum of Natural History, 200 Central Park West, Manhattan, NY, USA 5Center for Computational Astrophysics, Flatiron Institute, 162 5th Avenue, Manhattan, NY, USA ABSTRACT We present an analysis of 1524 spectra of Vega spanning 10 years, in which we search for periodic radial velocity variations. A signal with a periodicity of 0.676 days and a semi-amplitude of ∼10 m s-1 is consistent with the rotation period measured over much shorter time spans by previous spectroscopic and spectropolari- metric studies, confirming the presence of surface features on this A0 star. The timescale of evolution of these features can provide insight into the mechanism that sustains the weak magnetic fields in normal A type stars. Modeling the radial velocities with a Gaussian process using a quasi-periodic kernel suggests that the charac- teristic spot evolution timescale is ∼180 days, though we cannot exclude the possibility that it is much longer. -
Culmination of a Constellation
Culmination of a Constellation Over any night, stars and constellations in the sky will appear to move from east to west due to the Earth’s rotation on its axis. A constellation will culminate (reach its highest point in the sky for your location) when it centres on the meridian - an imaginary line that runs across the sky from north to south and also passes through the zenith (the point high in the sky directly above your head). For example: When to Observe Constellations The taBle shows the approximate time (AEST) constellations will culminate around the middle (15th day) of each month. Constellations will culminate 2 hours earlier for each successive month. Note: add an hour to the given time when daylight saving time is in effect. The time “12” is midnight. Sunrise/sunset times are rounded off to the nearest half an hour. Sun- Jan Feb Mar Apr May Jun Jul Aug Sep Oct Nov Dec Rise 5am 5:30 6am 6am 7am 7am 7am 6:30 6am 5am 4:30 4:30 Set 7pm 6:30 6pm 5:30 5pm 5pm 5pm 5:30 6pm 6pm 6:30 7pm And 5am 3am 1am 11pm 9pm Aqr 5am 3am 1am 11pm 9pm Aql 4am 2am 12 10pm 8pm Ara 4am 2am 12 10pm 8pm Ari 5am 3am 1am 11pm 9pm Aur 10pm 8pm 4am 2am 12 Boo 3am 1am 11pm 9pm 7pm Cnc 1am 11pm 9pm 7pm 3am CVn 3am 1am 11pm 9pm 7pm CMa 11pm 9pm 7pm 3am 1am Cap 5am 3am 1am 11pm 9pm 7pm Car 2am 12 10pm 8pm 6pm Cen 4am 2am 12 10pm 8pm 6pm Cet 4am 2am 12 10pm 8pm Cha 3am 1am 11pm 9pm 7pm Col 10pm 8pm 4am 2am 12 Com 3am 1am 11pm 9pm 7pm CrA 3am 1am 11pm 9pm 7pm CrB 4am 2am 12 10pm 8pm Crv 3am 1am 11pm 9pm 7pm Cru 3am 1am 11pm 9pm 7pm Cyg 5am 3am 1am 11pm 9pm 7pm Del -
EPSC2018-1115-2, 2018 European Planetary Science Congress 2018 Eeuropeapn Planetarsy Science Ccongress C Author(S) 2018
EPSC Abstracts Vol. 12, EPSC2018-1115-2, 2018 European Planetary Science Congress 2018 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2018 Ultra-short Period Rocky Super-Earths Luca Malavolta (1,2) , Andrew W. Mayo (3,4) , Tom Louden (5) , Vinesh M. Rajpaul (6) , Aldo S. Bonomo (7) , Lars A. Buchhave (4) , Laura Kreidberg (3,8) , Martti H. Kristiansen (9,10), Mercedes Lopez-Morales (3) , Annelies Mortier (11) , Andrew Vanderburg (3,12) , Adrien Coffinet (13), David Ehrenreich (13) , Christophe Lovis (13), Francois Bouchy (13), David Charbonneau (3) , David R. Ciardi (14), Andrew Collier Cameron (11) , Rosario Cosentino (15), Ian J. M. Crossfield (16,17), Mario Damasso (7) , Courtney D. Dressing (18) , Xavier Dumusque(13) , Mark E. Everett (19) , Pedro Figueira (20), Aldo F. M. Fiorenzano (15), Erica J. Gonzales (16,28), Raphaëlle D. Haywood (3,27) , Avet Harutyunyan (15), Lea Hirsch (18) , Steve B. Howell (21) , John Asher Johnson (3) , David W. Latham (3) , Eric Lopez (22), Michel Mayor (13), Giusi Micela (23), Emilio Molinari (15,24) , Valerio Nascimbeni (1,2) , Francesco Pepe (13), David F. Phillips (3) , Giampaolo Piotto (1,2) , Ken Rice (25), Dimitar Sasselov (3) , Damien Ségransan (13) , Alessandro Sozzetti (7) , Stéphane Udry (13), and Chris Watson (26) (1) Dipartimento di Fisica e Astronomia “Galileo Galilei,” Università di Padova, Italy ([email protected]) (2) INAF— Osservatorio Astronomico di Padova, Italy (3) Harvard-Smithsonian Center for Astrophysics, USA (4) Centre for Star and Planet Formation, Denmark (5) Department -
Planets in Spin-Orbit Misalignment and the Search for Stellar
Planets in Spin-Orbit Misalignment and the Search for Stellar Companions Brett C. Addison∗†, C. G. Tinney∗†, Duncan J. Wright∗†, Graeme Salter∗†, Daniel Bayliss‡ and George Zhou‡ ∗ School of Physics, University of New South Wales, Sydney, NSW 2052, Australia; [email protected] † Australian Centre for Astrobiology, University of New South Wales, NSW 2052, Australia ‡ Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australia Summary: The discovery of giant planets orbiting close to their host stars was one of the most unexpected results of early exoplanetary science. Astronomers have since found that a significant fraction of these ‘Hot Jupiters’ move on orbits substantially misaligned with the rotation axis of their host star. We recently reported the measurement of the spin- orbit misalignment for WASP-79b by using data from the 3.9 m Anglo-Australian Telescope. Contemporary models of planetary formation produce planets on nearly coplanar orbits with respect to their host star’s equator. We discuss the mechanisms which could drive planets into spin-orbit misalignment. The most commonly proposed being the Kozai mechanism, which requires the presence of a distant, massive companion to the star-planet system. We therefore describe a volume-limited direct-imaging survey of Hot Jupiter systems with measured spin- orbit angles, to search for the presence of stellar companions and test the Kozai hypothesis. Keywords: planets and satellites: dynamical evolution and stability stars: individual (WASP- 79) techniques: radial velocities and direct imaging Introduction Exoplanetary science is possibly the most exciting and rapidly developing branch of modern astronomy. Just over 1000 planets1 have been discovered to date, mainly through radial velocity and transit searches. -
CCD Double Star Measurements - Personal Observations: #Report 1
Vol. 8 No. 3 July 1, 2012 Journal of Double Star Observations Page 193 CCD Double Star Measurements - Personal Observations: #Report 1 Giuseppe Micello Bologna Emilia Romagna - Italy EMAIL: [email protected] Abstract: This report submits CCD measurements of 49 pairs, observed in the period No- vember 2011 – January 2012. Possible new pairs, not cataloged in the Washington Double Star Catalog, are suggested. Orionis (precise coordinate from the Aladin Sky At- Introduction las: 05:19:06.14 +02:34:27.0, Figure 3) and new pair Between November 2011 and January 2012, I in system STF 721/GUI 7/BU 557 (precise coordinate made measurements of 49 double and multiple stars. from the Aladin Sky Atlas: 05:29:39.01 +03:06:47.5, For these measurements, I used a Schmidt- Figure 4). Cassegrain 235/2350 and a Maksutov-Cassegrain In this system, GUI 7AD is a neglected double 150/1800 on equatorial mount and the optical train star and we have only one measurement, dating back composed of a CCD camera, Imaging Source to 1904. DMK21AU, and an IR Cut Filter on Flip Mirror. The method is the same that I reported in a pre- Acknowledgements vious papers [1, 2] where I used Reduc by Florent This research has made use of the catalogs pre- Losse for data reduction,. sent in The Aladin Sky Atlas. Astrometric measurements and references to im- I thank Florent Losse for excellent software Re- ages and notes, are included in Table 1. duc. This paper also includes new possible pairs not I thank the Washington Double Star Catalog and cataloged in the Washington Double Star Catalog [3]. -
Binocular Challenges
This page intentionally left blank Cosmic Challenge Listing more than 500 sky targets, both near and far, in 187 challenges, this observing guide will test novice astronomers and advanced veterans alike. Its unique mix of Solar System and deep-sky targets will have observers hunting for the Apollo lunar landing sites, searching for satellites orbiting the outermost planets, and exploring hundreds of star clusters, nebulae, distant galaxies, and quasars. Each target object is accompanied by a rating indicating how difficult the object is to find, an in-depth visual description, an illustration showing how the object realistically looks, and a detailed finder chart to help you find each challenge quickly and effectively. The guide introduces objects often overlooked in other observing guides and features targets visible in a variety of conditions, from the inner city to the dark countryside. Challenges are provided for viewing by the naked eye, through binoculars, to the largest backyard telescopes. Philip S. Harrington is the author of eight previous books for the amateur astronomer, including Touring the Universe through Binoculars, Star Ware, and Star Watch. He is also a contributing editor for Astronomy magazine, where he has authored the magazine’s monthly “Binocular Universe” column and “Phil Harrington’s Challenge Objects,” a quarterly online column on Astronomy.com. He is an Adjunct Professor at Dowling College and Suffolk County Community College, New York, where he teaches courses in stellar and planetary astronomy. Cosmic Challenge The Ultimate Observing List for Amateurs PHILIP S. HARRINGTON CAMBRIDGE UNIVERSITY PRESS Cambridge, New York, Melbourne, Madrid, Cape Town, Singapore, Sao˜ Paulo, Delhi, Dubai, Tokyo, Mexico City Cambridge University Press The Edinburgh Building, Cambridge CB2 8RU, UK Published in the United States of America by Cambridge University Press, New York www.cambridge.org Information on this title: www.cambridge.org/9780521899369 C P. -
Shorter Communications a Reconstruction of a Tahitian Star Compass Based on Tupaia's “Chart for the Society Islands With
SHORTER COMMUNICATIONS A RECONSTRUCTION OF A TAHITIAN STAR COMPASS BASED ON TUPAIA’S “CHART FOR THE SOCIETY ISLANDS WITH OTAHEITE IN THE CENTER” ANNE DI PIAZZA Centre National de Recherche Scientifique—Centre de Recherche et de Documentation sur l’Océanie, Marseille When Europeans first ventured into the Pacific they had to grapple with three almost inconceivable notions: (i) that Pacific Islanders could guide their canoes successfully over long distances without instruments, while they, the Europeans, had spent centuries developing the compass, the sextant and the chronometer for navigation; (ii) that the islanders could hold mental maps, while they, the Europeans, had spent centuries developing ways of representing a curved world on a flat map; and (iii) that Pacific islanders could memorise and transmit knowledge of numerous star paths, as well as “wind” or “island compasses” orally, in contrast to the almanacs and various mathematical tables created over centuries in Europe. This encounter of two schools of navigation, one technically sophisticated and based largely on written knowledge, the other an oral system, has lead to considerable “méconnaissance” (Turnbull 1998)—not the least concerns methods of way finding and mental cartography. It is perhaps no surprise that Tupaia, the high priest and navigator encountered by Cook in Tahiti in 1769, had some difficulty convincing the Captain of the accuracy of the “situation of the islands” he knew of since hidden behind the Chart he drew was a body of local knowledge encompassing indigenous geography, astronomy and navigation. All of these domains were confounded into one “art of navigation” by Europeans. In Oceania, the “… art of navigation includes a sizable body of knowledge developed to meet the needs of ocean voyaging… local navigators have had to commit to memory their knowledge of the stars, sailing directions, seamarks…” (Goodenough and Thomas 1987: 3).