Precise Doppler Monitoring of Barnard's Star
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A&A 526, A141 (2011) Astronomy DOI: 10.1051/0004-6361/201016034 & c ESO 2011 Astrophysics The HARPS search for southern extra-solar planets, XXVI. Two giant planets around M0 dwarfs T. Forveille1, X. Bonfils1,2, G. Lo Curto3,X.Delfosse1,S.Udry2, F. Bouchy4,5,C.Lovis2, M. Mayor2, C. Moutou6, D. Naef2,3,F.Pepe2, C. Perrier1,D.Queloz2, and N. Santos7,8 1 Laboratoire d’Astrophysique de Grenoble, Observatoire de Grenoble, Université Joseph Fourier, CNRS, UMR 5571, BP 53, 38041 Grenoble Cedex 9, France e-mail: [email protected] 2 Observatoire de Genève, Université de Genève, 51 ch. des Maillettes, 1290 Sauverny, Switzerland 3 European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile 4 Institut d’Astrophysique de Paris, CNRS, Université Pierre et Marie Curie, 98bis Bd Arago, 75014 Paris, France 5 Observatoire de Haute-Provence, CNRS/OAMP, 04870 St Michel l’Observatoire, France 6 Laboratoire d’Astrophysique de Marseille, 38 rue Fréderic Joliot-Curie, 13388 Marseille Cedex 13, France 7 Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal 8 Departamento de Fìsica e Astronomia, Faculdade de Ciências, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal Received 31 October 2010 / Accepted 1 December 2010 ABSTRACT Fewer giants planets are found around M dwarfs than around more massive stars, and this dependence of planetary characteristics on the mass of the central star is an important observational diagnostic of planetary formation theories. In part to improve on those statistics, we are monitoring the radial velocities of nearby M dwarfs with the HARPS spectrograph on the ESO 3.6 m telescope. -
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. -
DOUBLE STARS INFORMATION CIRCULAR No. 202 (OCTOBER 2020)
INTERNATIONAL ASTRONOMICAL UNION COMMISSION G1 (BINARY AND MULTIPLE STAR SYSTEMS) DOUBLE STARS INFORMATION CIRCULAR No. 202 (OCTOBER 2020) NEW ORBITS ADS Name P T e Ω(2000) 2020 Author(s) α2000δ n a i ! Last ob. 2021 1762 A 207 1204y6 1937.27 0.816 31◦3 358◦9 000629 SCARDIA 02182+3920 0◦2989 000950 31◦1 193◦9 2020.771 359.2 0.635 et al. (*) 1477 WRH 39 Aa,Ab 29.59 1987.66 0.608 189.5 327.3 0.081 DOCOBO 02318+8916 12.1663 0.120 146.2 123.0 2014.4856 312.1 0.093 & CAMPO - COU 1688 AB 8.638 2003.841 0.198 49.2 247.6 0.121 DOCOBO 03321+4340 41.6763 0.139 35.5 268.2 2012.7023 308.0 0.092 & LING 3303 HU 1082 53.17 2023.24 0.746 108.9 221.1 0.151 DOCOBO 04349+3908 6.7707 0.362 48.9 216.3 2007.8019 240.7 0.132 & LING 3730 BU 1047 BC 34.38 2001.21 0.944 30.9 78.1 0.357 DOCOBO 05098+2802 10.4712 0.282 122.4 114.9 2007.8184 77.0 0.357 & CAMPO 11635 STF 2382 AB 2802.8 2051.49 0.953 149.6 344.3 2.169 DOCOBO 18443+3940 0.1284 14.237 102.2 258.8 2020.7470 344.0 2.148 & CAMPO 11635 STF 2383 CD 724.3 2223.9 0.353 26.5 74.3 2.399 DOCOBO 18443+3940 0.4970 2.920 126.1 73.8 2020.7470 73.9 2.402 & CAMPO 11635 CHR 77 Ca,Cb 15.75 2008.94 0.411 42.4 48.2 0.229 DOCOBO 18443+3940 22.8571 0.191 109.9 127.2 2005.5155 42.9 0.214 & CAMPO 13950 COU 1962 AB 20.414 1999.240 0.524 116.7 108.5 0.086 DOCOBO 20311+3333 17.6350 0.201 76.0 307.2 2008.5460 121.7 0.119 & CAMPO (*) SCARDIA, PRIEUR, PANSECCHI, LING, ARGYLE, ARISTIDI, ZANUTTA, ABE, BENDJOYA, RIVET, SUAREZ & VERNET 1 SARAH LEE LIPPINCOTT (1920-2019) Sarah Lee Lippincott was born in Philadelphia in 1920 and attended the University of Pennsylvania College for Women. -
New College News Release New College, Sarasota, Florida Furman C
/-·· NEW COLLEGE NEWS RELEASE NEW COLLEGE, SARASOTA, FLORIDA FURMAN C. ARTHUR - INFORMATION FOR RELEASE: Sunday, March 1, 1964 Sarasota--New College will have as its eighth lecturer in the New Perspectives in Science series Thursday at 8:00 p.m., Dutch born Dr. Peter van de Kamp, Director of the Sproul Observatory, swarthmore College. Dr. van de Kamp, the second astronomer in the series, approaches his field from a new viewpoint for the lecture at College Hall. He said that his talk will be about astronomy as a liberal art, "and by its very nature, peculiarly adapted to removing any artificial or imaginary bar- riers between the so-called sciences and the so-called liberal arts. Attendance at the lectures is by season registration although some single evening registrations are accepted. Born at Kampen in the Netherlands, Dr. van de Kamp was educated at the University of Utrecht where he studied astronomy, mathematics, and physics. Later, he obtained doctoral degrees at the University of California and the University of Groningen. Shortly after completing his education in the Netherlands, he came to this country to work at the McCormick Observatory at the University of Virginia and at the Lick Observatory at the University of California. (more) - 2 - Since 1937 he has been Director of the Sproul Observatory and Chairman of its Department of Astronomy. The Swarthmore observatory has one of the largest astronomical instruments of its kind. Dr. van de Kamp has taught or lectured a ·t many colleges in several countries. He is a former Fulbright scholar in France. During his education he was a member of Phi Beta Kappa and Sigma :· ~, honorary science research organization. -
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. -
The Search for Planets Around Other Stars by Andrew Fraknoi, Astronomical Society of the Pacific
www.astrosociety.org/uitc No. 19 - Winter 1991-92 © 1992, Astronomical Society of the Pacific, 390 Ashton Avenue, San Francisco, CA 94112 The Search for Planets Around Other Stars by Andrew Fraknoi, Astronomical Society of the Pacific The question of whether there are planets outside our Solar System has intrigued scientists, science fiction writers and poets for years. But how can we know if any really exist? We devote this issue of The Universe in the Classroom to the search for planets around other stars. What is the difference between a planet and a star? Why do we think there might be planets around other stars? Why is it so hard to see planets around other stars? If we can't see them, how can we find out if there are planets around other stars? Have any planets been detected from stellar wobbles? The Case of Barnard's Star Are there other ways to detect planets? Can we see the large disks of gas and dust around other stars out of which planets form? What about reports of planets around pulsars? Activity: Center of Mass Demonstration What is the difference between a planet and a star? Stars are huge luminous balls of gas powered by nuclear reactions at their centers. The enormously high temperatures and pressures in the core of a star force atoms of hydrogen to fuse together and become helium atoms, releasing tremendous amounts of energy in the process. Planets are much smaller with core temperatures and pressures too low for nuclear fusion to occur. Thus they emit no light of their own. -
Levensbericht P. Van De Kamp, In: Levensberichten En Herdenkingen, 1996, Amsterdam, Pp
Huygens Institute - Royal Netherlands Academy of Arts and Sciences (KNAW) Citation: E.P.J. van den Heuvel, Levensbericht P. van de Kamp, in: Levensberichten en herdenkingen, 1996, Amsterdam, pp. 49-54 This PDF was made on 24 September 2010, from the 'Digital Library' of the Dutch History of Science Web Center (www.dwc.knaw.nl) > 'Digital Library > Proceedings of the Royal Netherlands Academy of Arts and Sciences (KNAW), http://www.digitallibrary.nl' - 1 - Levensbericht door E. P.l. van den Heuvel Peter van de Kamp 26 december 1901 - 18 mei 1995 Peter van de Kamp 49 - 2 - Peter van de Kamp overleed in Middenbeemster, 18 mei 1995, op een leeftijd van 93 jaar. Hij was een wereld-autoriteit op het gebied van de astrometrie: de nauwkeurige meting van posities en bewegingen van sterren. Zijn onderzoek, dat hij sinds 1937 aan de Sproul Sterrewacht uitvoerde, betrof met name het zoeken naar de aanwezigheid van donkere begeleiders bij sterren. Hij ontdekte - door een uiterst nauwkeurige studie van de bewegingen van sterren - een groot aantal van dergelijke begeleiders, sommige met massa's slechts een tiental malen groter dan die van de planeet Jupiter. Een aanzienlijk aantal van de leidende astronomen in de Verenigde Staten werd door hem opgeleid. In 1980 keerde hij naar Neder land terug, waar hij zich vestigde in Amsterdam. Van de Kamp werd geboren in Kampen op 26 december 1901, in een eenvou dig middenstandsgezin. Zijn vader was boekhouder bij een kleine fabriek. Na het behalen van zijn IIBS-B diploma ving hij in 1918 in Utrecht zijn studie in de Wis-, Natuur- en Sterrenkunde aan. -
Analytic Stability Maps of Unknown Exoplanet Companions for Imaging Prioritization
Bachelor's degree thesis ANALYTIC STABILITY MAPS OF UNKNOWN EXOPLANET COMPANIONS FOR IMAGING PRIORITIZATION Carlos Gasc´on Alvarez´ Advised by Dmitry Savransky (Cornell University) Miquel Sureda (UPC) In partial fulfillment of the requirements for the Bachelor's Degree in Mathematics Bachelor's Degree in Aerospace Technology Engineering July 2019 ABSTRACT Identifying which systems are more likely to host an imageable planet can play an important role in the construction of an optimized target list for future direct imaging missions, such as the planned technology demonstration for the Wide Field Infrared Survey Telescope (WFIRST). For single-planet systems, the presence of an already detected exoplanet can severely restrict the target's stable region and should therefore be considered when searching for unknown companions. To do so, we first analyze the performance and robustness of several two-planet stability criteria by comparing them with long-term numerical simulations. We then derive the necessary formulation for the computation of (a, R) analytic stability maps, which can be used in conjunction with depth- of-search grids in order to define the stable-imageable region of a system. The dynamically stable completeness (i.e., the expected number of imageable and stable planets) can then be calculated via convolution with the selected occurrence grid, obtaining a metric that can be directly compared for imaging prioritization. Applying this procedure to all the currently known single-planet systems within a distance of 50 pc, we construct a ranked target list based on the WFIRST CGI's predicted performance and SAG13 occurrence rates. Keywords| numerical simulations - analytic stability maps - dynamical evolution and stability - direct imaging - exoplanets 1 CONTENTS 1 Introduction 3 2 Analytic Stability Criteria for Two-Planet Systems 4 2.1 Criteria Based on the Outer Pericenter to Inner Apocenter Ratio . -
JRASC, October 1998 Issue (PDF)
Publications from October/octobre 1998 Volume/volume 92 Number/numero 5 [673] The Royal Astronomical Society of Canada NEW LARGER SIZE! Observers Calendar — 1999 This calendar was created by members of the RASC. All photographs were taken by amateur astronomers using ordinary camera lenses and small The Journal of the Royal Astronomical Society of Canada Le Journal de la Société royale d’astronomie du Canada telescopes and represent a wide spectrum of objects. An informative caption accompanies every photograph. This year all of the photos are in full colour. It is designed with the observer in mind and contains comprehensive astronomical data such as daily Moon rise and set times, significant lunar and planetary conjunctions, eclipses, and meteor showers. (designed and produced by Rajiv Gupta) Price: $14 (includes taxes, postage and handling) The Beginner’s Observing Guide This guide is for anyone with little or no experience in observing the night sky. Large, easy to read star maps are provided to acquaint the reader with the constellations and bright stars. Basic information on observing the moon, planets and eclipses through the year 2000 is provided. There is also a special section to help Scouts, Cubs, Guides and Brownies achieve their respective astronomy badges. Written by Leo Enright (160 pages of information in a soft-cover book with a spiral binding which allows the book to lie flat). Price: $12 (includes taxes, postage and handling) Looking Up: A History of the Royal Astronomical Society of Canada Published to commemorate the 125th anniversary of the first meeting of the Toronto Astronomical Club, “Looking Up — A History of the RASC” is an excellent overall history of Canada’s national astronomy organization. -
Baneke-NL Astr 1921-56.Pptx
Dutch Astronomy between 1921 and 1956 David Baneke, VU Amsterdam Symposium honoring Adriaan Blaauw Groningen, 7 April 2014 Leiden Observatory staff (incl. computers and graduate students), 1933 Oosterhoff Kuiper Wesselink Oort Hertzsprung De Sier Woltjer Leiden Observatory, 1920s: - New staff: Pannekoek, Hertzsprung, Woltjer, Oort Willem de SiPer Adriaan Blaauw to DB: Ejnar Hertzsprung “At that Yme, the reputaon of Leiden Observatory was the reputaon of Hertzsprung” Frank Schlesinger to De Sier, 1927: “I have long felt, and I think I have expressed to you, a warm admiraon for the way in which you have made it possible for Hertzsprung to work effecYvely.” Leiden Observatory, 1920s: - New staff: Pannekoek, Hertzsprung, Woltjer, Oort - New graduate program Harlow Shapley to De Sier, 1928: Willem de SiPer “I remember your frequent statement that one principal funcon of your Observatory is to train and export highly capable young astronomers.” Meanwhile … Marcel Minnaert, Amsterdam Utrecht 2 main research tradiYons in Dutch astronomy: Groningen, Leiden: Kapteyn, Hertzsprung, Oort & students, successors Stellar & galacYc astronomy Amsterdam and Utrecht: Pannekoek, Minnaert & students, successors Astrophysics, solar physics Complete astronomy faculty in NL, 1920-1940: Groningen: Minnaert Kapteyn (unYl 1921) Amsterdam: Pannekoek Van Rhijn (from 1921) * Leiden: De Sier (unl 1934) * Hertzsprung * Woltjer Oort (from 1924) * Utrecht: Nijland (unl 1936) Van der Bilt * * * GM RAS P.J. van Rhijn and P. Oosterhoff 1939 Four former Groningen assistants: Bart Bok, Jan Oort, Peter van de Kamp, Jan Schilt 1939 1945: Jan Oort emerges as uncontested leader of Dutch astronomy Post-War plans: - Kenya expedition - ESO - Radio astronomy NAC colloquium on radio astronomy and the 21-cm line, 15 April 1944 Minutes by Adriaan Blaauw, secretary of the NAC Planning ahead: WSRT Jan Oort to Blaauw, 1956: Plenty of opportuniYes; plans for a new giant radio telescope, but NFRA board does not know about it yet. -
Article (Published Version)
Article Long-term magnetic activity of a sample of M-dwarf stars from the HARPS program. II. Activity an radial velocity GOMES DA SILVA, J., et al. Reference GOMES DA SILVA, J., et al. Long-term magnetic activity of a sample of M-dwarf stars from the HARPS program. II. Activity an radial velocity. Astronomy and Astrophysics, 2012, vol. 541, p. A9 DOI : 10.1051/0004-6361/201118598 Available at: http://archive-ouverte.unige.ch/unige:33880 Disclaimer: layout of this document may differ from the published version. 1 / 1 A&A 541, A9 (2012) Astronomy DOI: 10.1051/0004-6361/201118598 & c ESO 2012 Astrophysics Long-term magnetic activity of a sample of M-dwarf stars from the HARPS program II. Activity and radial velocity,, J. Gomes da Silva1,2,N.C.Santos1,2, X. Bonfils3, X. Delfosse3, T. Forveille3,S.Udry4, X. Dumusque1,4, and C. Lovis4 1 Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal e-mail: [email protected] 2 Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Portugal 3 UJF-Grenoble 1 / CNRS-INSU, Institut de Planétologie et d’Astrophysique de Grenoble (IPAG) UMR 5274, 38041 Grenoble, France 4 Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Versoix, Switzerland Received 6 December 2011 / Accepted 7 February 2012 ABSTRACT Owing to their low mass and luminosity, M dwarfs are ideal targets if one hopes to find low-mass planets similar to Earth using the radial velocity (RV) method. However, stellar magnetic cycles could add noise or even mimic the RV signal of a long-period companion. -
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.