The Stellar Heavens

Total Page:16

File Type:pdf, Size:1020Kb

The Stellar Heavens M ed u m 8vo h e 1 05 . 6d . i . , clot xtra, F L A M M A R I O N ’S P O P U LA R A S T R O N O M Y Tr nslated m the e c . ELLA G E a fro Fr n h by J RD OR , With 3 Plates and 288 Ill ustrations . The six books into which the b ook is d ivid ed give a very lu cid and accu rate d esc ription of t he knowledge whi ch has be e n acquired of the m v b od e o f c e b h e ec he m and h c c i o ing i s spa . ot as r sp ts t ir otions p ysi al onst in e m of f t he a we can e e . N ot tu rions. O transl tion only sp ak t r s prais d e it e e e e the a b u t M r . e has dd ed u efu e only o s w ll r pr s nt origin l , Gor a s l not s f r t he u e of b t he f m u d e and has o p rpos ringing in or ation p to at , also — — increase d the nu mber already very consid e rable o f t he e xc e lle nt illustra t ha t he is l e bec m e ul in E d it has tions , so t work ik ly to o as pop ar nglan as ' — i F A tlzene u m . bee n n rance . ‘ h M r E G e has ed E h has m The wh c . d e work i . J or translat into nglis a for itself a nam e and re pu tation in Franc e and has gone into general f hu d ed h u d c e Th f c c ircu lation t o the nu mbe r o a n r t o san opi s . is last a t is proof how well within the bou nds o f possibility it is to make t he latest d is c e e of c e c e c m ehe b e and f sc t o the c m m m d ov ri s s i n o pr nsi l a inating o on in . M Flam m ar ion has e d h u m h h u h the of his w . attain t is tri p t ro g grasp kno ed e t he u c d of his e and his e o f b i h m e t he m l g , l i ity styl , pow r ring ng o ost stu pe ndou s and c omplicated o f the things re vealed to u s in the d epths of ' ac e M Flam m ar ion s e h u d fi nd m r e cc e ce sp . pag s s o l al ost as g at a ptan in h u in his o wn S m c o f e m e and of e me ar e t is c o ntryas . i pli ity arrang nt stat nt i f s u c c ss —Seotsm an part o f h s c harm and o hi s e f . ' me if d e not d E M . Fl m m a e v u ce its h a rion s lat st ol , it o s ispla nglis rivals , a he t o wh c I i f m ay well take a high pl c e in t rank i h they b elong . t s u ll ' M r e c a e fu e d u c d and ha . e u e . l i , , t nks to Gor s r l r vision , w ll p to at ’ r r e ed c e fu b u h ab e o f the l e d c e i e M . Go s ition is so ar lly ro g t r ast at st is ov r s that the English stu d ent m ay now congratu late himself on be ing in an eve n ' ' f M Fla -Da zl l e a h m e . m mar i n Chr oni be i h t e c u o o . c e tt r posit on t n o ntry n y . You ng stu d e nts o f astronomy who wish t o obtain a general id ea o f the most wond erfu l and fasc inating of all sc ie nces will fi nd prec isely what they ’ M m m u e and e c T in F e c h e . he r see k . la arion s loq nt po ti apt rs re a e u r h e and c e t r t J- eaker many ill st ations in t is abl attra tiv ea ise Sfi . I is f sc e e d t o e e e hu d ed e and t a a inating work , xt n ing n arly s v n n r pag s , d ealing in popu lar langu age with som e of the most interesting of t he d is ' ver ies and f m e s — Dail N ews co spe cu lations o astrono r . y . M F mm is u d c c m e he has e de ed od . la arion a so n pra ti al astrono r ; r n r go and l b u e v c e the c e c e and he e e u b e f cu of a orio s s r i to s i n , poss ss s a val a l a lty u l e The u m e fu e and wel u ed me pop ar xposition . vol is pro s ly l ill strat , so ' f the be m h fi s — at u r d a R o e he e e e ce . S ev iew st plat s aking r t ir r t app aran y . ' A h h ac e m u be c c d ed t o Flam m ar ion s P u A m ig pl st a or op lar strono y. Never be fore has the science o f the heave ns b ee n treate d with su ch fu lness and interest as in this fascinating book ; for Flammarion is a m an of lette rs e m an of c e ce—a m an o f e e t oo e d wed w h the as w ll as a s i n l tt rs , , n o it wondrou s gifts of lu cidity and charm which d istingu ish the best French ’ i e . F m m i b is mu c h m e b b h m e wr t rs la ar on s ook or a sor ing t an ost nov ls , m e m c h m m c e m e e c h m e m et or ro anti t an ost ro an s , or po ti t an ost po s , y ' c and c e fi c c — u d l r c u e . L ate M onth st i tly s i nti ally a rat g y . I m u be c fe s ed h M F am m h . not e s t e e t st on s t at l arion only arr st att ntion , — b u t assists the read er to grasp astronom ical theories a task in whic h le ss ’ ’ u a e s f e fa he he m ak e t h m —Lzfem ¢ or ld e e W . pop l r writ r o t n il w n t y att pt. y The b is m f c o ne and h d t he e d e f m t o ook a ost as inating , ol s r a r ro start h As m u f r h finis . a an al o t ose who wish t o obtain a good gener al know ' ed e of m h l be f u d u e — i S c enc Goss . l g astrono y t is work wil o n nsu rpass d . i e p ’ L N D N CH ATT W N DU S 1 1 1 ST MART N S LAN E W O O O I , . I , . C. TH E STELLA R H EA V EN S ' ‘ A N I T RO U CT IO T O T H E Sf TUDY O F N D N , T HE ST A RS A ND NEBU LZE L E L L ARD GORE H onor ar y [Member of Me Liv erpool A str onom ic a l Soc iety A ssoc iate of Me A str onom ical Soc iety of Wales ; Cor r esponding ( t/ze lo t a t y Tor on A s r onom ic l S ocie y, A U T H O R O F ‘ ’ ‘ T H E SCEN ERY OF T H E H e A VE N s H E VI SI B LE N IV ER E , T U S , ’ ’ ' ‘ T H E WORLDS OF SI ACE S A R G ROU Ps E TC.
Recommended publications
  • Stsci Newsletter: 1997 Volume 014 Issue 01
    January 1997 • Volume 14, Number 1 SPACE TELESCOPE SCIENCE INSTITUTE Highlights of this issue: • AURA science and functional awards to Leitherer and Hanisch — pages 1 and 23 • Cycle 7 to be extended — page 5 • Cycle 7 approved Newsletter program listing — pages 7-13 Astronomy with HST Climbing the Starburst Distance Ladder C. Leitherer Massive stars are an important and powerful star formation events in sometimes dominant energy source for galaxies. Even the most luminous star- a galaxy. Their high luminosity, both in forming regions in our Galaxy are tiny light and mechanical energy, makes on a cosmic scale. They are not them detectable up to cosmological dominated by the properties of an distances. Stars ~100 times more entire population but by individual massive than the Sun are one million stars. Therefore stochastic effects times more luminous. Except for stars prevail. Extinction represents a severe of transient brightness, like novae and problem when a reliable census of the supernovae, hot, massive stars are Galactic high-mass star-formation the most luminous stellar objects in history is atempted, especially since the universe. massive stars belong to the extreme Massive stars are, however, Population I, with correspondingly extremely rare: The number of stars small vertical scale heights. Moreover, formed per unit mass interval is the proximity of Galactic regions — roughly proportional to the -2.35 although advantageous for detailed power of mass. We expect to find very studies of individual stars — makes it few massive stars compared to, say, difficult to obtain integrated properties, solar-type stars. This is consistent with such as total emission-line fluxes of observations in our solar neighbor- the ionized gas.
    [Show full text]
  • BRAS Newsletter August 2013
    www.brastro.org August 2013 Next meeting Aug 12th 7:00PM at the HRPO Dark Site Observing Dates: Primary on Aug. 3rd, Secondary on Aug. 10th Photo credit: Saturn taken on 20” OGS + Orion Starshoot - Ben Toman 1 What's in this issue: PRESIDENT'S MESSAGE....................................................................................................................3 NOTES FROM THE VICE PRESIDENT ............................................................................................4 MESSAGE FROM THE HRPO …....................................................................................................5 MONTHLY OBSERVING NOTES ....................................................................................................6 OUTREACH CHAIRPERSON’S NOTES .........................................................................................13 MEMBERSHIP APPLICATION .......................................................................................................14 2 PRESIDENT'S MESSAGE Hi Everyone, I hope you’ve been having a great Summer so far and had luck beating the heat as much as possible. The weather sure hasn’t been cooperative for observing, though! First I have a pretty cool announcement. Thanks to the efforts of club member Walt Cooney, there are 5 newly named asteroids in the sky. (53256) Sinitiere - Named for former BRAS Treasurer Bob Sinitiere (74439) Brenden - Named for founding member Craig Brenden (85878) Guzik - Named for LSU professor T. Greg Guzik (101722) Pursell - Named for founding member Wally Pursell
    [Show full text]
  • Arxiv:2107.05688V1 [Astro-Ph.GA] 12 Jul 2021
    FERMILAB-PUB-21-274-AE-LDRD Draft version September 6, 2021 Typeset using LATEX twocolumn style in AASTeX63 RR Lyrae stars in the newly discovered ultra-faint dwarf galaxy Centaurus I∗ C. E. Mart´ınez-Vazquez´ ,1 W. Cerny ,2, 3 A. K. Vivas ,1 A. Drlica-Wagner ,4, 2, 3 A. B. Pace ,5 J. D. Simon,6 R. R. Munoz,7 A. R. Walker ,1 S. Allam,4 D. L. Tucker,4 M. Adamow´ ,8 J. L. Carlin ,9 Y. Choi,10 P. S. Ferguson ,11, 12 A. P. Ji,6 N. Kuropatkin,4 T. S. Li ,6, 13, 14 D. Mart´ınez-Delgado,15 S. Mau ,16, 17 B. Mutlu-Pakdil ,2, 3 D. L. Nidever,18 A. H. Riley,11, 12 J. D. Sakowska ,19 D. J. Sand ,20 G. S. Stringfellow ,21 (DELVE Collaboration) 1Cerro Tololo Inter-American Observatory, NSF's NOIRLab, Casilla 603, La Serena, Chile 2Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637, USA 3Department of Astronomy and Astrophysics, University of Chicago, Chicago IL 60637, USA 4Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USA 5McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Ave, Pittsburgh, PA 15213, USA 6Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USA 7Departamento de Astronom´ıa,Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chile 8Center for Astrophysical Surveys, National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA 9Rubin Observatory/AURA, 950 North Cherry Avenue, Tucson, AZ, 85719, USA 10Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 11George P.
    [Show full text]
  • 10. Scientific Programme 10.1
    10. SCIENTIFIC PROGRAMME 10.1. OVERVIEW (a) Invited Discourses Plenary Hall B 18:00-19:30 ID1 “The Zoo of Galaxies” Karen Masters, University of Portsmouth, UK Monday, 20 August ID2 “Supernovae, the Accelerating Cosmos, and Dark Energy” Brian Schmidt, ANU, Australia Wednesday, 22 August ID3 “The Herschel View of Star Formation” Philippe André, CEA Saclay, France Wednesday, 29 August ID4 “Past, Present and Future of Chinese Astronomy” Cheng Fang, Nanjing University, China Nanjing Thursday, 30 August (b) Plenary Symposium Review Talks Plenary Hall B (B) 8:30-10:00 Or Rooms 309A+B (3) IAUS 288 Astrophysics from Antarctica John Storey (3) Mon. 20 IAUS 289 The Cosmic Distance Scale: Past, Present and Future Wendy Freedman (3) Mon. 27 IAUS 290 Probing General Relativity using Accreting Black Holes Andy Fabian (B) Wed. 22 IAUS 291 Pulsars are Cool – seriously Scott Ransom (3) Thu. 23 Magnetars: neutron stars with magnetic storms Nanda Rea (3) Thu. 23 Probing Gravitation with Pulsars Michael Kremer (3) Thu. 23 IAUS 292 From Gas to Stars over Cosmic Time Mordacai-Mark Mac Low (B) Tue. 21 IAUS 293 The Kepler Mission: NASA’s ExoEarth Census Natalie Batalha (3) Tue. 28 IAUS 294 The Origin and Evolution of Cosmic Magnetism Bryan Gaensler (B) Wed. 29 IAUS 295 Black Holes in Galaxies John Kormendy (B) Thu. 30 (c) Symposia - Week 1 IAUS 288 Astrophysics from Antartica IAUS 290 Accretion on all scales IAUS 291 Neutron Stars and Pulsars IAUS 292 Molecular gas, Dust, and Star Formation in Galaxies (d) Symposia –Week 2 IAUS 289 Advancing the Physics of Cosmic
    [Show full text]
  • GU Monocerotis: a High-Mass Eclipsing Overcontact Binary in the Young Open Cluster Dolidze 25? J
    A&A 590, A45 (2016) Astronomy DOI: 10.1051/0004-6361/201628224 & c ESO 2016 Astrophysics GU Monocerotis: A high-mass eclipsing overcontact binary in the young open cluster Dolidze 25? J. Lorenzo1, I. Negueruela1, F. Vilardell2, S. Simón-Díaz3; 4, P. Pastor5, and M. Méndez Majuelos6 1 Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Escuela Politécnica Superior, Universidad de Alicante, Carretera de San Vicente del Raspeig s/n, 03690 San Vicente del Raspeig, Alicante, Spain e-mail: [email protected] 2 Institut d’Estudis Espacials de Catalunya, Edifici Nexus, c/ Capitá, 2−4, desp. 201, 08034 Barcelona, Spain 3 Instituto de Astrofísica de Canarias, Vía Láctea s/n, 38200 La Laguna, Tenerife, Spain 4 Departamento de Astrofísica, Universidad de La Laguna, Facultad de Física y Matemáticas, Avda. Astrofísico Francisco Sánchez s/n, 38205 La Laguna, Tenerife, Spain 5 Departamento de Lenguajes y Sistemas Informáticos, Universidad de Alicante, Apdo. 99, 03080 Alicante, Spain 6 Departamento de Ciencias, IES Arroyo Hondo, c/ Maestro Manuel Casal 2, 11520 Rota, Cádiz, Spain Received 30 January 2016 / Accepted 3 March 2016 ABSTRACT Context. The eclipsing binary GU Mon is located in the star-forming cluster Dolidze 25, which has the lowest metallicity measured in a Milky Way young cluster. Aims. GU Mon has been identified as a short-period eclipsing binary with two early B-type components. We set out to derive its orbital and stellar parameters. Methods. We present a comprehensive analysis, including B and V light curves and 11 high-resolution spectra, to verify the orbital period and determine parameters.
    [Show full text]
  • A Handbook of Double Stars, with a Catalogue of Twelve Hundred
    The original of this bool< is in the Cornell University Library. There are no known copyright restrictions in the United States on the use of the text. http://www.archive.org/details/cu31924064295326 3 1924 064 295 326 Production Note Cornell University Library pro- duced this volume to replace the irreparably deteriorated original. It was scanned using Xerox soft- ware and equipment at 600 dots per inch resolution and com- pressed prior to storage using CCITT Group 4 compression. The digital data were used to create Cornell's replacement volume on paper that meets the ANSI Stand- ard Z39. 48-1984. The production of this volume was supported in part by the Commission on Pres- ervation and Access and the Xerox Corporation. Digital file copy- right by Cornell University Library 1991. HANDBOOK DOUBLE STARS. <-v6f'. — A HANDBOOK OF DOUBLE STARS, WITH A CATALOGUE OF TWELVE HUNDRED DOUBLE STARS AND EXTENSIVE LISTS OF MEASURES. With additional Notes bringing the Measures up to 1879, FOR THE USE OF AMATEURS. EDWD. CROSSLEY, F.R.A.S.; JOSEPH GLEDHILL, F.R.A.S., AND^^iMES Mt^'^I^SON, M.A., F.R.A.S. "The subject has already proved so extensive, and still ptomises so rich a harvest to those who are inclined to be diligent in the pursuit, that I cannot help inviting every lover of astronomy to join with me in observations that must inevitably lead to new discoveries." Sir Wm. Herschel. *' Stellae fixac, quae in ccelo conspiciuntur, sunt aut soles simplices, qualis sol noster, aut systemata ex binis vel interdum pluribus solibus peculiari nexu physico inter se junccis composita.
    [Show full text]
  • Variable Star Classification and Light Curves Manual
    Variable Star Classification and Light Curves An AAVSO course for the Carolyn Hurless Online Institute for Continuing Education in Astronomy (CHOICE) This is copyrighted material meant only for official enrollees in this online course. Do not share this document with others. Please do not quote from it without prior permission from the AAVSO. Table of Contents Course Description and Requirements for Completion Chapter One- 1. Introduction . What are variable stars? . The first known variable stars 2. Variable Star Names . Constellation names . Greek letters (Bayer letters) . GCVS naming scheme . Other naming conventions . Naming variable star types 3. The Main Types of variability Extrinsic . Eclipsing . Rotating . Microlensing Intrinsic . Pulsating . Eruptive . Cataclysmic . X-Ray 4. The Variability Tree Chapter Two- 1. Rotating Variables . The Sun . BY Dra stars . RS CVn stars . Rotating ellipsoidal variables 2. Eclipsing Variables . EA . EB . EW . EP . Roche Lobes 1 Chapter Three- 1. Pulsating Variables . Classical Cepheids . Type II Cepheids . RV Tau stars . Delta Sct stars . RR Lyr stars . Miras . Semi-regular stars 2. Eruptive Variables . Young Stellar Objects . T Tau stars . FUOrs . EXOrs . UXOrs . UV Cet stars . Gamma Cas stars . S Dor stars . R CrB stars Chapter Four- 1. Cataclysmic Variables . Dwarf Novae . Novae . Recurrent Novae . Magnetic CVs . Symbiotic Variables . Supernovae 2. Other Variables . Gamma-Ray Bursters . Active Galactic Nuclei 2 Course Description and Requirements for Completion This course is an overview of the types of variable stars most commonly observed by AAVSO observers. We discuss the physical processes behind what makes each type variable and how this is demonstrated in their light curves. Variable star names and nomenclature are placed in a historical context to aid in understanding today’s classification scheme.
    [Show full text]
  • Gaia Data Release 2 Special Issue
    A&A 623, A110 (2019) Astronomy https://doi.org/10.1051/0004-6361/201833304 & © ESO 2019 Astrophysics Gaia Data Release 2 Special issue Gaia Data Release 2 Variable stars in the colour-absolute magnitude diagram?,?? Gaia Collaboration, L. Eyer1, L. Rimoldini2, M. Audard1, R. I. Anderson3,1, K. Nienartowicz2, F. Glass1, O. Marchal4, M. Grenon1, N. Mowlavi1, B. Holl1, G. Clementini5, C. Aerts6,7, T. Mazeh8, D. W. Evans9, L. Szabados10, A. G. A. Brown11, A. Vallenari12, T. Prusti13, J. H. J. de Bruijne13, C. Babusiaux4,14, C. A. L. Bailer-Jones15, M. Biermann16, F. Jansen17, C. Jordi18, S. A. Klioner19, U. Lammers20, L. Lindegren21, X. Luri18, F. Mignard22, C. Panem23, D. Pourbaix24,25, S. Randich26, P. Sartoretti4, H. I. Siddiqui27, C. Soubiran28, F. van Leeuwen9, N. A. Walton9, F. Arenou4, U. Bastian16, M. Cropper29, R. Drimmel30, D. Katz4, M. G. Lattanzi30, J. Bakker20, C. Cacciari5, J. Castañeda18, L. Chaoul23, N. Cheek31, F. De Angeli9, C. Fabricius18, R. Guerra20, E. Masana18, R. Messineo32, P. Panuzzo4, J. Portell18, M. Riello9, G. M. Seabroke29, P. Tanga22, F. Thévenin22, G. Gracia-Abril33,16, G. Comoretto27, M. Garcia-Reinaldos20, D. Teyssier27, M. Altmann16,34, R. Andrae15, I. Bellas-Velidis35, K. Benson29, J. Berthier36, R. Blomme37, P. Burgess9, G. Busso9, B. Carry22,36, A. Cellino30, M. Clotet18, O. Creevey22, M. Davidson38, J. De Ridder6, L. Delchambre39, A. Dell’Oro26, C. Ducourant28, J. Fernández-Hernández40, M. Fouesneau15, Y. Frémat37, L. Galluccio22, M. García-Torres41, J. González-Núñez31,42, J. J. González-Vidal18, E. Gosset39,25, L. P. Guy2,43, J.-L. Halbwachs44, N. C. Hambly38, D.
    [Show full text]
  • Tracing the Outer Structure of the Sagittarius Dwarf Galaxy: Detections at Angular Distances Between 10 and 34 Degrees ∗
    Tracing the Outer Structure of the Sagittarius Dwarf Galaxy: Detections at Angular Distances Between 10 and 34 Degrees ∗ Mario Mateo1 e-mail: [email protected] Edward W. Olszewski2 e-mail: [email protected] Heather L. Morrison3 e-mail: [email protected] Received ; accepted ∗BasedonobservationsobtainedwiththeBlancoTelescopeatCTIO,whichisoperated by the National Optical Astronomy Observatory, under contract to AURA. 1Department of Astronomy, University of Michigan, 821 Dennison Bldg., Ann Arbor, MI 48109–1090 2Steward Observatory, 933 N. Cherry, University of Arizona, Tucson, AZ 85721-0065 3Cottrell Scholar of Research Corporation, and NSF Career Fellow; Department of Astronomy and Department of Physics, Case Western Reserve University, Cleveland OH 44106 –2– ABSTRACT We have obtained deep photometric data in 24 fields along the southeast extension of the major axis of the Sagittarius dwarf spheroidal (Sgr dSph) galaxy, and in four fields along the northwest extension. Using star counts at the expected position of the Sgr upper main-sequence within the resulting color-magnitude diagrams (CMDs), we unambiguously detect Sgr stars in the southeast over the range 10–34◦ from the galaxy’s center. If Sgr is symmetric, this implies a true major-axis diameter of at least 68◦, or nearly 30 kpc if all portions of Sgr are equally distant from the Sun. Star counts parallel to the galaxy’s minor-axis reveal that Sgr remains quite broad far from its center. This suggests that the outer portions of Sgr resemble a stream rather than an extension of the ellipsoidal inner regions of the galaxy. The inferred V-band surface brightness (SB) profile ranges from 27.3-30.5 mag arcsec−2 over this radial range and exhibits a change in slope ∼ 20◦ from the center of Sgr.
    [Show full text]
  • Arxiv:2006.10868V2 [Astro-Ph.SR] 9 Apr 2021 Spain and Institut D’Estudis Espacials De Catalunya (IEEC), C/Gran Capit`A2-4, E-08034 2 Serenelli, Weiss, Aerts Et Al
    Noname manuscript No. (will be inserted by the editor) Weighing stars from birth to death: mass determination methods across the HRD Aldo Serenelli · Achim Weiss · Conny Aerts · George C. Angelou · David Baroch · Nate Bastian · Paul G. Beck · Maria Bergemann · Joachim M. Bestenlehner · Ian Czekala · Nancy Elias-Rosa · Ana Escorza · Vincent Van Eylen · Diane K. Feuillet · Davide Gandolfi · Mark Gieles · L´eoGirardi · Yveline Lebreton · Nicolas Lodieu · Marie Martig · Marcelo M. Miller Bertolami · Joey S.G. Mombarg · Juan Carlos Morales · Andr´esMoya · Benard Nsamba · KreˇsimirPavlovski · May G. Pedersen · Ignasi Ribas · Fabian R.N. Schneider · Victor Silva Aguirre · Keivan G. Stassun · Eline Tolstoy · Pier-Emmanuel Tremblay · Konstanze Zwintz Received: date / Accepted: date A. Serenelli Institute of Space Sciences (ICE, CSIC), Carrer de Can Magrans S/N, Bellaterra, E- 08193, Spain and Institut d'Estudis Espacials de Catalunya (IEEC), Carrer Gran Capita 2, Barcelona, E-08034, Spain E-mail: [email protected] A. Weiss Max Planck Institute for Astrophysics, Karl Schwarzschild Str. 1, Garching bei M¨unchen, D-85741, Germany C. Aerts Institute of Astronomy, Department of Physics & Astronomy, KU Leuven, Celestijnenlaan 200 D, 3001 Leuven, Belgium and Department of Astrophysics, IMAPP, Radboud University Nijmegen, Heyendaalseweg 135, 6525 AJ Nijmegen, the Netherlands G.C. Angelou Max Planck Institute for Astrophysics, Karl Schwarzschild Str. 1, Garching bei M¨unchen, D-85741, Germany D. Baroch J. C. Morales I. Ribas Institute of· Space Sciences· (ICE, CSIC), Carrer de Can Magrans S/N, Bellaterra, E-08193, arXiv:2006.10868v2 [astro-ph.SR] 9 Apr 2021 Spain and Institut d'Estudis Espacials de Catalunya (IEEC), C/Gran Capit`a2-4, E-08034 2 Serenelli, Weiss, Aerts et al.
    [Show full text]
  • A Terrestrial Planet Candidate in a Temperate Orbit Around Proxima Centauri
    A terrestrial planet candidate in a temperate orbit around Proxima Centauri Guillem Anglada-Escude´1∗, Pedro J. Amado2, John Barnes3, Zaira M. Berdinas˜ 2, R. Paul Butler4, Gavin A. L. Coleman1, Ignacio de la Cueva5, Stefan Dreizler6, Michael Endl7, Benjamin Giesers6, Sandra V. Jeffers6, James S. Jenkins8, Hugh R. A. Jones9, Marcin Kiraga10, Martin Kurster¨ 11, Mar´ıa J. Lopez-Gonz´ alez´ 2, Christopher J. Marvin6, Nicolas´ Morales2, Julien Morin12, Richard P. Nelson1, Jose´ L. Ortiz2, Aviv Ofir13, Sijme-Jan Paardekooper1, Ansgar Reiners6, Eloy Rodr´ıguez2, Cristina Rodr´ıguez-Lopez´ 2, Luis F. Sarmiento6, John P. Strachan1, Yiannis Tsapras14, Mikko Tuomi9, Mathias Zechmeister6. July 13, 2016 1School of Physics and Astronomy, Queen Mary University of London, 327 Mile End Road, London E1 4NS, UK 2Instituto de Astrofsica de Andaluca - CSIC, Glorieta de la Astronoma S/N, E-18008 Granada, Spain 3Department of Physical Sciences, Open University, Walton Hall, Milton Keynes MK7 6AA, UK 4Carnegie Institution of Washington, Department of Terrestrial Magnetism 5241 Broad Branch Rd. NW, Washington, DC 20015, USA 5Astroimagen, Ibiza, Spain 6Institut fur¨ Astrophysik, Georg-August-Universitat¨ Gottingen¨ Friedrich-Hund-Platz 1, 37077 Gottingen,¨ Germany 7The University of Texas at Austin and Department of Astronomy and McDonald Observatory 2515 Speedway, C1400, Austin, TX 78712, USA 8Departamento de Astronoma, Universidad de Chile Camino El Observatorio 1515, Las Condes, Santiago, Chile 9Centre for Astrophysics Research, Science & Technology Research Institute, University of Hert- fordshire, Hatfield AL10 9AB, UK 10Warsaw University Observatory, Aleje Ujazdowskie 4, Warszawa, Poland 11Max-Planck-Institut fur¨ Astronomie Konigstuhl¨ 17, 69117 Heidelberg, Germany 12Laboratoire Univers et Particules de Montpellier, Universit de Montpellier, Pl.
    [Show full text]
  • Commission 27 of the I.A.U. Information Bulletin On
    COMMISSION 27 OF THE I.A.U. INFORMATION BULLETIN ON VARIABLE STARS Nos. 2101 - 2200 1982 March - 1982 September EDITOR: B. SZEIDL, KONKOLY OBSERVATORY 1525 BUDAPEST, Box 67, HUNGARY HU ISSN 0374-0676 2101 PHOTOELECTRIC PHOTOMETRY OF THE ECLIPSING BINARY DM PERSEI C. Sezer 4 March 1982 2102 PHOTOELECTRIC OBSERVATION OF W UMa (BD +56d1400) E. Hamzaoglu, V. Keskin, T. Eker 8 March 1982 2103 PHOTOELECTRIC PHOTOMETRY OF Ap STARS IN THE GALACTIC CLUSTER NGC 2516: PRELIMINARY RESULTS P. North, F. Rufener, P. Bartholdi 8 March 1982 2104 BV PHOTOMETRY OF BETELGEUSE OCT. 1979 TO APR. 1981 K. Krisciunas 8 March 1982 2105 ON THE NOVA-LIKE OBJECTS IN THE CENTRAL REGION OF M31 A.S. Sharov 9 March 1982 2106 HD 65227: A NEW SHORT PERIOD CEPHEID OF VERY SMALL AMPLITUDE O.J. Eggen 12 March 1982 2107 1981 UBVR PHOTOMETRIC OBSERVATIONS OF ER Vul M. Zeilik, R. Elston, G. Henson, P. Schmolke, P. Smith 12 March 1982 2108 PHOTOELECTRIC OBSERVATIONS OF VW CEPHEI T. Abe 15 March 1982 2109 29 DRACONIS: A NEW VARIABLE STAR D.S. Hall, G.W. Henry, H. Louth, Th.R. Renner, S.N. Shore 17 March 1982 2110 HD 26337: A NEW RS CVn VARIABLE STAR F.C. Fekel, D.S. Hall, G.W. Henry, H.J. Landis, Th.R. Renner 17 March 1982 2111 HD 136905: A NEW RS CVn VARIABLE STAR E.W. Burke, J.E. Baker, F.C. Fekel, D.S. Hall, G.W. Henry 17 March 1982 2112 VARIABLE STARS IN THE NORTHERN LUMINOUS STARS CATALOGUES W.P. Bidelman 17 March 1982 2113 CENTRAL STAR OF PLANETARY NEBULA NGC 2346: NEW ECLIPSING BINARY L.
    [Show full text]