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Where Are the Distant Worlds? Star Maps
W here Are the Distant Worlds? Star Maps Abo ut the Activity Whe re are the distant worlds in the night sky? Use a star map to find constellations and to identify stars with extrasolar planets. (Northern Hemisphere only, naked eye) Topics Covered • How to find Constellations • Where we have found planets around other stars Participants Adults, teens, families with children 8 years and up If a school/youth group, 10 years and older 1 to 4 participants per map Materials Needed Location and Timing • Current month's Star Map for the Use this activity at a star party on a public (included) dark, clear night. Timing depends only • At least one set Planetary on how long you want to observe. Postcards with Key (included) • A small (red) flashlight • (Optional) Print list of Visible Stars with Planets (included) Included in This Packet Page Detailed Activity Description 2 Helpful Hints 4 Background Information 5 Planetary Postcards 7 Key Planetary Postcards 9 Star Maps 20 Visible Stars With Planets 33 © 2008 Astronomical Society of the Pacific www.astrosociety.org Copies for educational purposes are permitted. Additional astronomy activities can be found here: http://nightsky.jpl.nasa.gov Detailed Activity Description Leader’s Role Participants’ Roles (Anticipated) Introduction: To Ask: Who has heard that scientists have found planets around stars other than our own Sun? How many of these stars might you think have been found? Anyone ever see a star that has planets around it? (our own Sun, some may know of other stars) We can’t see the planets around other stars, but we can see the star. -
Ultra-High-Resolution Spectroscopy of the ISM Towards Orion
Ultra-High-Resolution Spectroscopy of the ISM Towards Orion Richard John Price Thesis submitted for the Degree of Doctor of Philosophy of the University of London UCL Department of Physics & Astronomy UNIVERSITY COLLEGE LONDON March 2002 ProQuest Number: U643002 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 complete 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 U643002 Published by ProQuest LLC(2015). Copyright of the Dissertation is held by the Author. All rights reserved. This work is protected against unauthorized copying under Title 17, United States Code. Microform Edition © ProQuest LLC. ProQuest LLC 789 East Eisenhower Parkway P.O. Box 1346 Ann Arbor, Ml 48106-1346 To my parents “If we knew what it was we were doing, it would not be called research, would it?” Albert Einstein. ’ * • A b s t r a c t Firstly, we report ultra-high-resolution observations {R % 880,000) of Na I Di, Ca II if, K I, CH and CH+ for interstellar sightlines towards twelve bright stars in Orion, including four stars in the M42 region. Secondly, we report high-resolution observations {R py 110, 000) of Na I Di Sz. Ü2 and Ca, u H k. K towards twelve stars with various locations in and around the A Orionis association. Model fits have been constructed for the absorption-line profiles, providing estimates for the column density, velocity dispersion, and central velocity for each constituent veloc ity component. -
![Arxiv:2105.11583V2 [Astro-Ph.EP] 2 Jul 2021 Keck-HIRES, APF-Levy, and Lick-Hamilton Spectrographs](https://docslib.b-cdn.net/cover/4203/arxiv-2105-11583v2-astro-ph-ep-2-jul-2021-keck-hires-apf-levy-and-lick-hamilton-spectrographs-364203.webp)
Arxiv:2105.11583V2 [Astro-Ph.EP] 2 Jul 2021 Keck-HIRES, APF-Levy, and Lick-Hamilton Spectrographs
Draft version July 6, 2021 Typeset using LATEX twocolumn style in AASTeX63 The California Legacy Survey I. A Catalog of 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades Lee J. Rosenthal,1 Benjamin J. Fulton,1, 2 Lea A. Hirsch,3 Howard T. Isaacson,4 Andrew W. Howard,1 Cayla M. Dedrick,5, 6 Ilya A. Sherstyuk,1 Sarah C. Blunt,1, 7 Erik A. Petigura,8 Heather A. Knutson,9 Aida Behmard,9, 7 Ashley Chontos,10, 7 Justin R. Crepp,11 Ian J. M. Crossfield,12 Paul A. Dalba,13, 14 Debra A. Fischer,15 Gregory W. Henry,16 Stephen R. Kane,13 Molly Kosiarek,17, 7 Geoffrey W. Marcy,1, 7 Ryan A. Rubenzahl,1, 7 Lauren M. Weiss,10 and Jason T. Wright18, 19, 20 1Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 2IPAC-NASA Exoplanet Science Institute, Pasadena, CA 91125, USA 3Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA 4Department of Astronomy, University of California Berkeley, Berkeley, CA 94720, USA 5Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 6Department of Astronomy & Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA 7NSF Graduate Research Fellow 8Department of Physics & Astronomy, University of California Los Angeles, Los Angeles, CA 90095, USA 9Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA 10Institute for Astronomy, University of Hawai`i, -
Astronomy Astrophysics
A&A 470, 191–210 (2007) Astronomy DOI: 10.1051/0004-6361:20077168 & c ESO 2007 Astrophysics The Mira variable S Orionis: relationships between the photosphere, molecular layer, dust shell, and SiO maser shell at 4 epochs,,,† M. Wittkowski1,D.A.Boboltz2, K. Ohnaka3,T.Driebe3, and M. Scholz4,5 1 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany e-mail: [email protected] 2 United States Naval Observatory, 3450 Massachusetts Avenue, NW, Washington, DC 20392-5420, USA e-mail: [email protected] 3 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany 4 Institut für Theoretische Astrophysik der Univ. Heidelberg, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany 5 Institute of Astronomy, School of Physics, University of Sydney, Sydney NSW 2006, Australia Received 25 January 2007 / Accepted 18 April 2007 ABSTRACT Aims. We present the first multi-epoch study that includes concurrent mid-infrared and radio interferometry of an oxygen-rich Mira star. Methods. We obtained mid-infrared interferometry of S Ori with VLTI/MIDI at four epochs in December 2004, February/March 2005, November 2005, and December 2005. We concurrently observed v = 1, J = 1−0 (43.1 GHz), and v = 2, J = 1−0 (42.8 GHz) SiO maser emission toward S Ori with the VLBA in January, February, and November 2005. The MIDI data are analyzed using self-excited dynamic model atmospheres including molecular layers, complemented by a radiative transfer model of the circumstellar dust shell. The VLBA data are reduced to the spatial structure and kinematics of the maser spots. -
VSS Newsletter 2018-1 1 from the Director - Mark Blackford Happy New Year to You All, Welcome to 2018
Newsletter 2018-1 January 2018 www.variablestarssouth.org Observations and model light curve of the eclipsing binary V871 Ara. Col Bembrick, Tony Ainsworth and Jeff Byron collaborated on this project in 2001 and have now updated it with a model light curve and new stellar parameters. See their article on page 17 for details. Contents From the director - Mark Blackford ......................................................................................................... 2 2018 RASNZ conference and 5th VSS symposium .............................................................................. 2 Astrometric Positions for SMC Variables – Mati Morel ......................................................................... 3 A look at Mira in 2018 – Stan Walker ..................................................................................................... 8 The DY Per star V487 Vel – Andrew Pearce .........................................................................................11 V382 Carinae - a yellow hypergiant star – Stan Walker ....................................................................... 13 Photometry & initial modelling of the eclipsing binary V871 Ara – C Bembrick, T Ainsworth* & J Byron ...... 17 Changes in the pulsating variables projects - Mira stars with long periods – Stan Walker .................. 23 V0454 Car spectroscopic and photometric campaign – Mark Blackford .............................................. 26 Request for cooperation ...................................................................................................................... -
A Review on Substellar Objects Below the Deuterium Burning Mass Limit: Planets, Brown Dwarfs Or What?
geosciences Review A Review on Substellar Objects below the Deuterium Burning Mass Limit: Planets, Brown Dwarfs or What? José A. Caballero Centro de Astrobiología (CSIC-INTA), ESAC, Camino Bajo del Castillo s/n, E-28692 Villanueva de la Cañada, Madrid, Spain; [email protected] Received: 23 August 2018; Accepted: 10 September 2018; Published: 28 September 2018 Abstract: “Free-floating, non-deuterium-burning, substellar objects” are isolated bodies of a few Jupiter masses found in very young open clusters and associations, nearby young moving groups, and in the immediate vicinity of the Sun. They are neither brown dwarfs nor planets. In this paper, their nomenclature, history of discovery, sites of detection, formation mechanisms, and future directions of research are reviewed. Most free-floating, non-deuterium-burning, substellar objects share the same formation mechanism as low-mass stars and brown dwarfs, but there are still a few caveats, such as the value of the opacity mass limit, the minimum mass at which an isolated body can form via turbulent fragmentation from a cloud. The least massive free-floating substellar objects found to date have masses of about 0.004 Msol, but current and future surveys should aim at breaking this record. For that, we may need LSST, Euclid and WFIRST. Keywords: planetary systems; stars: brown dwarfs; stars: low mass; galaxy: solar neighborhood; galaxy: open clusters and associations 1. Introduction I can’t answer why (I’m not a gangstar) But I can tell you how (I’m not a flam star) We were born upside-down (I’m a star’s star) Born the wrong way ’round (I’m not a white star) I’m a blackstar, I’m not a gangstar I’m a blackstar, I’m a blackstar I’m not a pornstar, I’m not a wandering star I’m a blackstar, I’m a blackstar Blackstar, F (2016), David Bowie The tenth star of George van Biesbroeck’s catalogue of high, common, proper motion companions, vB 10, was from the end of the Second World War to the early 1980s, and had an entry on the least massive star known [1–3]. -
Meeting Program
A A S MEETING PROGRAM 211TH MEETING OF THE AMERICAN ASTRONOMICAL SOCIETY WITH THE HIGH ENERGY ASTROPHYSICS DIVISION (HEAD) AND THE HISTORICAL ASTRONOMY DIVISION (HAD) 7-11 JANUARY 2008 AUSTIN, TX All scientific session will be held at the: Austin Convention Center COUNCIL .......................... 2 500 East Cesar Chavez St. Austin, TX 78701 EXHIBITS ........................... 4 FURTHER IN GRATITUDE INFORMATION ............... 6 AAS Paper Sorters SCHEDULE ....................... 7 Rachel Akeson, David Bartlett, Elizabeth Barton, SUNDAY ........................17 Joan Centrella, Jun Cui, Susana Deustua, Tapasi Ghosh, Jennifer Grier, Joe Hahn, Hugh Harris, MONDAY .......................21 Chryssa Kouveliotou, John Martin, Kevin Marvel, Kristen Menou, Brian Patten, Robert Quimby, Chris Springob, Joe Tenn, Dirk Terrell, Dave TUESDAY .......................25 Thompson, Liese van Zee, and Amy Winebarger WEDNESDAY ................77 We would like to thank the THURSDAY ................. 143 following sponsors: FRIDAY ......................... 203 Elsevier Northrop Grumman SATURDAY .................. 241 Lockheed Martin The TABASGO Foundation AUTHOR INDEX ........ 242 AAS COUNCIL J. Craig Wheeler Univ. of Texas President (6/2006-6/2008) John P. Huchra Harvard-Smithsonian, President-Elect CfA (6/2007-6/2008) Paul Vanden Bout NRAO Vice-President (6/2005-6/2008) Robert W. O’Connell Univ. of Virginia Vice-President (6/2006-6/2009) Lee W. Hartman Univ. of Michigan Vice-President (6/2007-6/2010) John Graham CIW Secretary (6/2004-6/2010) OFFICERS Hervey (Peter) STScI Treasurer Stockman (6/2005-6/2008) Timothy F. Slater Univ. of Arizona Education Officer (6/2006-6/2009) Mike A’Hearn Univ. of Maryland Pub. Board Chair (6/2005-6/2008) Kevin Marvel AAS Executive Officer (6/2006-Present) Gary J. Ferland Univ. of Kentucky (6/2007-6/2008) Suzanne Hawley Univ. -
Stars and Their Spectra: an Introduction to the Spectral Sequence Second Edition James B
Cambridge University Press 978-0-521-89954-3 - Stars and Their Spectra: An Introduction to the Spectral Sequence Second Edition James B. Kaler Index More information Star index Stars are arranged by the Latin genitive of their constellation of residence, with other star names interspersed alphabetically. Within a constellation, Bayer Greek letters are given first, followed by Roman letters, Flamsteed numbers, variable stars arranged in traditional order (see Section 1.11), and then other names that take on genitive form. Stellar spectra are indicated by an asterisk. The best-known proper names have priority over their Greek-letter names. Spectra of the Sun and of nebulae are included as well. Abell 21 nucleus, see a Aurigae, see Capella Abell 78 nucleus, 327* ε Aurigae, 178, 186 Achernar, 9, 243, 264, 274 z Aurigae, 177, 186 Acrux, see Alpha Crucis Z Aurigae, 186, 269* Adhara, see Epsilon Canis Majoris AB Aurigae, 255 Albireo, 26 Alcor, 26, 177, 241, 243, 272* Barnard’s Star, 129–130, 131 Aldebaran, 9, 27, 80*, 163, 165 Betelgeuse, 2, 9, 16, 18, 20, 73, 74*, 79, Algol, 20, 26, 176–177, 271*, 333, 366 80*, 88, 104–105, 106*, 110*, 113, Altair, 9, 236, 241, 250 115, 118, 122, 187, 216, 264 a Andromedae, 273, 273* image of, 114 b Andromedae, 164 BDþ284211, 285* g Andromedae, 26 Bl 253* u Andromedae A, 218* a Boo¨tis, see Arcturus u Andromedae B, 109* g Boo¨tis, 243 Z Andromedae, 337 Z Boo¨tis, 185 Antares, 10, 73, 104–105, 113, 115, 118, l Boo¨tis, 254, 280, 314 122, 174* s Boo¨tis, 218* 53 Aquarii A, 195 53 Aquarii B, 195 T Camelopardalis, -
The Mira Variable S Orionis: Relationships Between the Photosphere, Molecular Layer, Dust Shell, and Sio Maser Shell at 4 Epochs , , ,†
A&A 470, 191–210 (2007) Astronomy DOI: 10.1051/0004-6361:20077168 & c ESO 2007 Astrophysics The Mira variable S Orionis: relationships between the photosphere, molecular layer, dust shell, and SiO maser shell at 4 epochs,,,† M. Wittkowski1,D.A.Boboltz2, K. Ohnaka3,T.Driebe3, and M. Scholz4,5 1 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany e-mail: [email protected] 2 United States Naval Observatory, 3450 Massachusetts Avenue, NW, Washington, DC 20392-5420, USA e-mail: [email protected] 3 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany 4 Institut für Theoretische Astrophysik der Univ. Heidelberg, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany 5 Institute of Astronomy, School of Physics, University of Sydney, Sydney NSW 2006, Australia Received 25 January 2007 / Accepted 18 April 2007 ABSTRACT Aims. We present the first multi-epoch study that includes concurrent mid-infrared and radio interferometry of an oxygen-rich Mira star. Methods. We obtained mid-infrared interferometry of S Ori with VLTI/MIDI at four epochs in December 2004, February/March 2005, November 2005, and December 2005. We concurrently observed v = 1, J = 1−0 (43.1 GHz), and v = 2, J = 1−0 (42.8 GHz) SiO maser emission toward S Ori with the VLBA in January, February, and November 2005. The MIDI data are analyzed using self-excited dynamic model atmospheres including molecular layers, complemented by a radiative transfer model of the circumstellar dust shell. The VLBA data are reduced to the spatial structure and kinematics of the maser spots. -
Max-Planck-Institut Für Astronomie 26.02.09 11:43
Max-Planck-Institut für Astronomie 26.02.09 11:43 Planeten- und Sternentstehung/ Planet and Star Formation (2007) Refereed Papers Adelman-McCarthy, J. K., M. A. Agüeros, S. S. Allam, K. S. J. Anderson, S. F. Anderson, J. Annis, N. A. Bahcall, C. A. L. Bailer-Jones, I. K. Baldry, J. C. Barentine, T. C. Beers, V. Belokurov, A. Berlind, M. Bernardi, M. R. Blanton, J. J. Bochanski, W. N. Boroski, D. M. Bramich, H. J. Brewington, J. Brinchmann, J. Brinkmann, R. J. Brunner, T. Budavári, L. N. Carey, S. Carliles, M. A. Carr, F. J. Castander, A. J. Connolly, R. J. Cool, C. E. Cunha, I. Csabai, J. J. Dalcanton, M. Doi, D. J. Eisenstein, M. L. Evans, N. W. Evans, X. Fan, D. P. Finkbeiner, S. D. Friedman, J. A. Frieman, M. Fukugita, B. Gillespie, G. Gilmore, K. Glazebrook, J. Gray, E. K. Grebel, J. E. Gunn, E. de Haas, P. B. Hall, M. Harvanek, S. L. Hawley, J. Hayes, T. M. Heckman, J. S. Hendry, G. S. Hennessy, R. B. Hindsley, C. M. Hirata, C. J. Hogan, D. W. Hogg, J. A. Holtzman, S.-i. Ichikawa, T. Ichikawa, Z. Ivezic, S. Jester, D. E. Johnston, A. M. Jorgensen, M. Juric, G. Kauffmann, S. M. Kent, S. J. Kleinman, G. R. Knapp, A. Y. Kniazev, R. G. Kron, J. Krzesinski, N. Kuropatkin, D. Q. Lamb, H. Lampeitl, B. C. Lee, R. F. Leger, M. Lima, H. Lin, D. C. Long, J. Loveday, R. H. Lupton, R. Mandelbaum, B. Margon, D. Martínez-Delgado, T. Matsubara, P. M. McGehee, T. -
Episodic Accretion in Young Stars
Episodic Accretion in Young Stars Marc Audard University of Geneva Peter´ Abrah´ am´ Konkoly Observatory Michael M. Dunham Yale University Joel D. Green University of Texas at Austin Nicolas Grosso Observatoire Astronomique de Strasbourg Kenji Hamaguchi National Aeronautics and Space Administration and University of Maryland, Baltimore County Joel H. Kastner Rochester Institute of Technology Agnes´ Kosp´ al´ European Space Agency Giuseppe Lodato Universit`aDegli Studi di Milano Marina M. Romanova Cornell University Stephen L. Skinner University of Colorado at Boulder Eduard I. Vorobyov University of Vienna and Southern Federal University Zhaohuan Zhu Princeton University In the last twenty years, the topic of episodic accretion has gained significant interest in the star formation community. It is now viewed as a common, though still poorly understood, phenomenon in low-mass star formation. The FU Orionis objects (FUors) are long-studied arXiv:1401.3368v1 [astro-ph.SR] 14 Jan 2014 examples of this phenomenon. FUors are believed to undergo accretion outbursts during which −7 −4 −1 the accretion rate rapidly increases from typically 10 to a few 10 M⊙ yr , and remains elevated over several decades or more. EXors, a loosely defined class of pre-main sequence stars, exhibit shorter and repetitive outbursts, associated with lower accretion rates. The relationship between the two classes, and their connection to the standard pre-main sequence evolutionary sequence, is an open question: do they represent two distinct classes, are they triggered by the same physical mechanism, and do they occur in the same evolutionary phases? Over the past couple of decades, many theoretical and numerical models have been developed to explain the origin of FUor and EXor outbursts. -
The Astronomical Zoo: Discovery and Classification
Theme 6: The Astronomical Zoo: discovery and classification 6.1 Discovery As discussed earlier, astronomy is atypical among the exact sciences in that discovery normally precedes understanding, sometimes by many years. Astronomical discovery is usually driven by availability of technology rather than by theoretical predictions or speculation. Figure 6.1, redrawn from Martin Harwit’s Cosmic Discovery (MIT Press, 1984), show how the rate of disco- very of “astronomical phenomena” (i.e. classes of object, rather than properties such as dis- tance) has increased over time (the line is a rough fit to an exponential), and 50 the age of the necessary technology at the time the discovery was made. (I 40 have not attempted to update Harwit’s data, because the decision as to what 30 constitutes a new phenomenon is sub- 20 jective to some degree; he puts in seve- ral items that I would not have regar- 10 ded as significant, omits some I would total numberof classes have listed, and doesn’t always assign 0 the same date as I would.) 1550 1600 1650 1700 1750 1800 1850 1900 1950 date Note that the pace of discoveries accel- erates in the 20th century, and the time Impact of new technology lag between the availability of the ne- 15 cessary technology and the actual dis- covery decreases. This is likely due to 10 the greater number of working astro- <1954 nomers: if the technology to make the 5 discovery exists, someone will make it. 1954-74 However, Harwit also makes the point 0 that the discoveries made in the period Numberof discoveries <5 5-10 10-25 25-50 >50 1954−74 were generally (~85%) made Age of required technology (years) by people who were not initially trained in astronomy (mostly physi- Figure 6.1: astronomical discoveries.