Measuring Distance
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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. -
<H1>History of Astronomy by George Forbes</H1>
History of Astronomy by George Forbes History of Astronomy by George Forbes Produced by Jonathan Ingram, Dave Maddock, Charles Franks and the Online Distributed Proofreading Team. [Illustration: SIR ISAAC NEWTON (From the bust by Roubiliac In Trinity College, Cambridge.)] HISTORY OF ASTRONOMY BY GEORGE FORBES, M.A., F.R.S., M. INST. C. E., (FORMERLY PROFESSOR OF NATURAL PHILOSOPHY, ANDERSON'S COLLEGE, GLASGOW) AUTHOR OF "THE TRANSIT OF VENUS," RENDU'S "THEORY OF THE GLACIERS OF SAVOY," ETC., ETC. page 1 / 186 CONTENTS PREFACE BOOK I. THE GEOMETRICAL PERIOD 1. PRIMITIVE ASTRONOMY AND ASTROLOGY 2. ANCIENT ASTRONOMY--CHINESE AND CHALDAEANS 3. ANCIENT GREEK ASTRONOMY 4. THE REIGN OF EPICYCLES--FROM PTOLEMY TO COPERNICUS BOOK II. THE DYNAMICAL PERIOD 5. DISCOVERY OF THE TRUE SOLAR SYSTEM--TYCHO BRAHE--KEPLER 6. GALILEO AND THE TELESCOPE--NOTIONS OF GRAVITY BY HORROCKS, ETC. 7. SIR ISAAC NEWTON--LAW OF UNIVERSAL GRAVITATION page 2 / 186 8. NEWTON'S SUCCESSORS--HALLEY, EULER, LAGRANGE, LAPLACE, ETC. 9. DISCOVERY OF NEW PLANETS--HERSCHEL, PIAZZI, ADAMS, AND LE VERRIER BOOK III. OBSERVATION 10. INSTRUMENTS OF PRECISION--SIZE OF THE SOLAR SYSTEM 11. HISTORY OF THE TELESCOPE--SPECTROSCOPE BOOK IV. THE PHYSICAL PERIOD 12. THE SUN 13. THE MOON AND PLANETS 14. COMETS AND METEORS 15. THE STARS AND NEBULAE page 3 / 186 INDEX PREFACE An attempt has been made in these pages to trace the evolution of intellectual thought in the progress of astronomical discovery, and, by recognising the different points of view of the different ages, to give due credit even to the ancients. No one can expect, in a history of astronomy of limited size, to find a treatise on "practical" or on "theoretical astronomy," nor a complete "descriptive astronomy," and still less a book on "speculative astronomy." Something of each of these is essential, however, for tracing the progress of thought and knowledge which it is the object of this History to describe. -
PHASES Differential Astrometry and Iodine Cell Radial Velocities of The
PHASES Differential Astrometry and Iodine Cell Radial Velocities of the κ Pegasi Triple Star System Matthew W. Muterspaugh1, Benjamin F. Lane1, Maciej Konacki2, Sloane Wiktorowicz2, Bernard F. Burke1, M. M. Colavita3, S. R. Kulkarni4, M. Shao3 [email protected], [email protected], [email protected] ABSTRACT κ Pegasi is a well-known, nearby triple star system. It consists of a “wide” pair with semi-major axis 235 milli-arcseconds, one component of which is a single-line spectroscopic binary (semi-major axis 2.5 milli-arcseconds). Using high-precision differential astrometry and radial velocity observations, the masses for all three components are determined and the relative inclinations between the wide and narrow pairs’ orbits is found to be 43.8±3.0 degrees, just over the threshold for the three body Kozai resonance. The system distance is determined to 34.60 ± 0.21 parsec, and is consistent with trigonometric parallax measurements. Subject headings: stars:individual(κ Pegasi) – binaries:close – binaries:visual – techniques:interferometric – astrometry – stars:distances 1. Introduction ≈ ≈ arXiv:astro-ph/0509406v1 14 Sep 2005 κ Pegasi (10 Pegasi, ADS 15281, HR 8315, HD 206901; V 4.1, K 3.0) is comprised of two components, each with F5 subgiant spectrum, separated by 235 milli-arcseconds (here referred to as A and B; for historical reasons, B is the brighter and more massive—this distinction has been the cause of much confusion). Both components A and B have been 1MIT Kavli Institute for Astrophysics and Space Research, MIT Department of -
PHYS 2410 General Astronomy Homework 1 Due 9/23 Before the Classes
PHYS 2410 General Astronomy Homework 1 Due 9/23 before the classes !!請將答案用筆寫在一張 A4 紙上交給助教!! Multiple Choice (單選題!) 1. If the size of the Sun is represented by a baseball with the Earth is about 15 meters away, how far away, to scale, would the nearest stars to the Sun be? a. About the distance between New York and Boston. b. 100 meters away * c. About the distance across the United States. d. About the distance across 50 football fields. 2. A solar system contains a. primarily planets. b. large amounts of gas and dust but very few stars. c. large amounts of gas, dust, and stars. * d. a single star and planets. e. thousands of superclusters. 3. A galaxy contains a. primarily planets. b. large amounts of gas and dust but very few stars. * c. large amounts of gas, dust, and stars. d. a single star and planets. e. thousands of superclusters. 4. If light takes 8 minutes to reach Earth from the sun and 5.3 hours to reach Pluto, what is the approximate distance from the sun to Pluto? a. 5.3 AU * b. 40 AU c. 40 ly d. 5.3 ly e. 0.6 ly 5. If the nearest star is 4.2 light-years away, then a. the star is 4.2 million AU away. * b. the light we see left the star 4.2 years ago. c. the star must have formed 4.2 billion years ago. d. the star must be very young. e. the star must be very old. 6. If the nearest star is 4.2 light-years away, then a. -
Test Bank for Horizons Exploring the Universe
Test Bank for Horizons Exploring the Universe Enhanced 13th Edition by Seeds IBSN 9781305957374 Full Download: http://downloadlink.org/product/test-bank-for-horizons-exploring-the-universe-enhanced-13th-edition-by-seeds-ibsn-9781305957374/ CHAPTER 2—A USER'S GUIDE TO THE SKY MULTIPLE CHOICE 1. Seen from the northern latitudes (mid-northern hemisphere), the star Polaris a. is never above the horizon during the day. b. always sets directly in the west. c. is always above the northern horizon. d. is never visible during the winter. e. is the brightest star in the sky. ANS: C PTS: 1 2. An observer on Earth's equator would find _______ a. the celestial equator passing at 45 degrees above the northern horizon. b. the celestial equator passing at 45 degrees above the southern horizon. c. that the celestial equator coincides with the horizon. d. the celestial equator passing directly overhead. e. None of the above are true. ANS: D PTS: 1 3. An observer at Earth's geographic north pole would find _______ a. the celestial equator passing at 45 degrees above the northern horizon. b. the celestial equator passing at 45 degrees above the southern horizon. c. that the celestial equator coincides with the horizon. d. the celestial equator passing directly overhead. e. None of the above are true. ANS: C PTS: 1 4. An observer on Earth's geographic north pole would find a. Polaris directly overhead. b. Polaris 40° above the northern horizon. c. that the celestial equator coincides with the horizon. d. that the celestial equator passing directly overhead. -
The Journal of the Association of Lunar and Planetary Observers ?:Ftc Strolling Astronomer
The Journal Of The Association Of Lunar And Planetary Observers ?:ftc Strolling Astronomer 11111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111111 Volume 29, Numbers 7-8 Published August, 1982 Classical Mars chart by G. V. Schiaparelli from Memoria Sesta, Roma, 1899. Note the very dark RIMA TENUIS (thin or fine fissure) dividing the North Polar Cap into two unequal parts along the 150° W - 325° W areographic meridians. Discovered by Schiaparelli during the Martian northern late spring in 1888, RIMA TENUIS was last well observed by M. Maggini in 1918. It unexpectedly appeared again across the North Polar Cap before the Martian northern summer solstice in February, 1980, when it was photographed for the first time by Mars observers in the ALPO. Contributed by Mars Recorder Charles F. Capen. 1111111111111111111111111111111111111111111111::- THE STROLLING ASTRONOMER - Box 3AZ - University Park, New Mexico - 88003 - Residence telephone 522-4213 (Area Code 505) ::- in Las Cruces, New Mexico - Founded In 1947 - IN THIS ISSUE OBSERVING MARS X-REPORTING MARS OBSERVATIONS, by C. F. Capen ................................................... pg. 133 MARS OBSERVING AIDS - BOOKS, KITS, GRAPHS, AND CHARTS, by C. F. Capen ................................................... pg. 138 POSSIBLE LONG TERM CHANGES IN THE EQUATORIAL ZONE OF JUPITER, by Randy Tatum .................................................. pg. 141 SOME EUROPEAN VISUAL OBSERVATIONS OF SATURN IN 1981, by G. Adamoli ................................................... -
Characterizing Exoplanet Habitability
Characterizing Exoplanet Habitability Ravi kumar Kopparapu NASA Goddard Space Flight Center Eric T. Wolf University of Colorado, Boulder Victoria S. Meadows University of Washington Habitability is a measure of an environment’s potential to support life, and a habitable exoplanet supports liquid water on its surface. However, a planet’s success in maintaining liquid water on its surface is the end result of a complex set of interactions between planetary, stellar, planetary system and even Galactic characteristics and processes, operating over the planet’s lifetime. In this chapter, we describe how we can now determine which exoplanets are most likely to be terrestrial, and the research needed to help define the habitable zone under different assumptions and planetary conditions. We then move beyond the habitable zone concept to explore a new framework that looks at far more characteristics and processes, and provide a comprehensive survey of their impacts on a planet’s ability to acquire and maintain habitability over time. We are now entering an exciting era of terrestiral exoplanet atmospheric characterization, where initial observations to characterize planetary composition and constrain atmospheres is already underway, with more powerful observing capabilities planned for the near and far future. Understanding the processes that affect the habitability of a planet will guide us in discovering habitable, and potentially inhabited, planets. There are countless suns and countless earths all rotat- have the capability to characterize the most promising plan- ing around their suns in exactly the same way as the seven ets for signs of habitability and life. We are at an exhilarat- planets of our system. -
Meeting Abstracts
228th AAS San Diego, CA – June, 2016 Meeting Abstracts Session Table of Contents 100 – Welcome Address by AAS President Photoionized Plasmas, Tim Kallman (NASA 301 – The Polarization of the Cosmic Meg Urry GSFC) Microwave Background: Current Status and 101 – Kavli Foundation Lecture: Observation 201 – Extrasolar Planets: Atmospheres Future Prospects of Gravitational Waves, Gabriela Gonzalez 202 – Evolution of Galaxies 302 – Bridging Laboratory & Astrophysics: (LIGO) 203 – Bridging Laboratory & Astrophysics: Atomic Physics in X-rays 102 – The NASA K2 Mission Molecules in the mm II 303 – The Limits of Scientific Cosmology: 103 – Galaxies Big and Small 204 – The Limits of Scientific Cosmology: Town Hall 104 – Bridging Laboratory & Astrophysics: Setting the Stage 304 – Star Formation in a Range of Dust & Ices in the mm and X-rays 205 – Small Telescope Research Environments 105 – College Astronomy Education: Communities of Practice: Research Areas 305 – Plenary Talk: From the First Stars and Research, Resources, and Getting Involved Suitable for Small Telescopes Galaxies to the Epoch of Reionization: 20 106 – Small Telescope Research 206 – Plenary Talk: APOGEE: The New View Years of Computational Progress, Michael Communities of Practice: Pro-Am of the Milky Way -- Large Scale Galactic Norman (UC San Diego) Communities of Practice Structure, Jo Bovy (University of Toronto) 308 – Star Formation, Associations, and 107 – Plenary Talk: From Space Archeology 208 – Classification and Properties of Young Stellar Objects in the Milky Way to Serving -
Legacy Image
NASA SP17069 NASA Thesaurus Astronomy Vocabulary Scientific and Technical Information Division 1988 National Aeronautics and Space Administration Washington, M= . ' NASA SP-7069 NASA Thesaurus Astronomy Vocabulary A subset of the NASA Thesaurus prepared for the international Astronomical Union Conference July 27-31,1988 This publication was prepared by the NASA Scientific and Technical Information Facility operated for the National Aeronautics and Space Administration by RMS Associates. INTRODUCTION The NASA Thesaurus Astronomy Vocabulary consists of terms used by NASA indexers as descriptors for astronomy-related documents. The terms are presented in a hierarchical format derived from the 1988 edition of the NASA Thesaurus Volume 1 -Hierarchical Listing. Main (postable) terms and non- postable cross references are listed in alphabetical order. READING THE HIERARCHY Each main term is followed by a display of its context within a hierarchy. USE references, UF (used for) references, and SN (scope notes) appear immediately below the main term, followed by GS (generic structure), the hierarchical display of term relationships. The hierarchy is headed by the broadest term within that hierarchy. Terms that are broader in meaning than the main term are listed . above the main term; terms narrower in meaning are listed below the main term. The term itself is in boldface for easy identification. Finally, a list of related terms (RT) from other hierarchies is provided. Within a hierarchy, the number of dots to the left of a term indicates its hierarchical level - the more dots, the lower the level (i.e., the narrower the meaning of the term). For example, the term "ELLIPTICAL GALAXIES" which is preceded by two dots is narrower in meaning than "GALAXIES"; this in turn is narrower than "CELESTIAL BODIES". -
Star Name Database
Star Name Database Patrick J. Gleason April 29, 2019 Copyright © 2019 Atlanta Bible Fellowship All rights reserved. Except for brief passages quoted in a review, no part of this book may be reproduced by any mechanical, photographic, or electronic process, nor may it be stored in any information retrieval system, transmitted or otherwise copied for public or private use, without the written permission of the publisher. Requests for permission or further information should be addressed to S & R Technology Group, Suite 250, PMB 96, 15310 Amberly Drive, Tampa, Florida 33647. Star Names April 29, 2019 Patrick J. Gleason Atlanta Bible Fellowship Table of Contents 1.0 The Initiative ................................................................................................... 1 1.1 The Method ......................................................................................................... 2 2.0 Key Fields ........................................................................................................ 3 3.0 Data Fields ....................................................................................................... 7 3.1 Common_Name (Column A) ............................................................................. 7 3.2 Full_Name (Column B) ...................................................................................... 7 3.3 Language (Column C) ........................................................................................ 8 3.4 Translation (Column D).................................................................................... -
November 2020 BRAS Newsletter
A Mars efter Lowell's Glober ca. 1905-1909”, from Percival Lowell’s maps; National Maritime Museum, Greenwich, London (see Page 6) Monthly Meeting November 9th at 7:00 PM, via Jitsi (Monthly meetings are on 2nd Mondays at Highland Road Park Observatory, temporarily during quarantine at meet.jit.si/BRASMeets). GUEST SPEAKER: Chuck Allen from the Astronomical League will speak about The Cosmic Distance Ladder, which explores the historical advancement of distance determinations in astronomy. What's In This Issue? President’s Message Member Meeting Minutes Business Meeting Minutes Outreach Report Asteroid and Comet News Light Pollution Committee Report Globe at Night Member’s Corner – John Nagle ALPO 2020 Conference Astro-Photos by BRAS Members - MARS Messages from the HRPO REMOTE DISCUSSION Solar Viewing Edge of Night Natural Sky Conference Recent Entries in the BRAS Forum Observing Notes: Pisces – The Fishes Like this newsletter? See PAST ISSUES online back to 2009 Visit us on Facebook – Baton Rouge Astronomical Society BRAS YouTube Channel Baton Rouge Astronomical Society Newsletter, Night Visions Page 2 of 24 November 2020 President’s Message Welcome to the home stretch for 2020. The nights are starting earlier and earlier as the weather becomes more and more comfortable and all of our old favorites of the fall and winter skies really start finding their places right where they belong. October was a busy month for us, with several big functions at the Observatory, including two oppositions and two more all night celebrations. By comparison, November is looking fairly calm, the big focus there is going to be our third annual Natural Sky Conference on the 13th, which I’m encouraging people who care about the state of light pollution in our city and the surrounding area to get involved in. -
Chapter 2 Narrow Angle Astrometry
Binary Star Systems and Extrasolar Planets Matthew Ward Muterspaugh Submitted to the Department of Physics in partial fulfillment of the requirements for the degree of Doctor of Philosophy at the MASSACHUSETTS INSTITUTE OF TECHNOLOGY i%pk?-i& ;?0051 July 2005 @Matthew Ward Muterspaugh, 2005. All rights reserved. --wtatalbtd~~ -*ispa*reeardb -PtrWclypapsrond , -w-cdmw whole ahpar Author . ./pw.5 r. .....,. ........... ................... 7' Department of Physics July 6, 2005 Certified by . :-...... .I..........-. r" Y .-. ..............................- '7L. Bernard F. Burke Professor Emeritus Thesis Supervisor - Accepted by ..............)<. ... ,.+..,4. .. i /' ..-ib ..- 8 , 2 homas Greytak Associate Department Head for Education I ARCHIVES I I MAR 1 7 2006 1 I Binary Star Systems and Extrasolar Planets by Matthew Ward Muterspaugh Submitted to the Department of Physics on July 6, 2005, in partial fulfillment of the requirements for the degree of Doctor of Philosophy Abstract For ten years, planets around stars similar to the Sun have been discovered, confirmed, and their properties studied. Planets have been found in a variety of environments previously thought impossible. The results have revolutionized the way in which scientists underst and planet and star formation and evolution, and provide context for the roles of the Earth and our own solar system. Over half of star systems contain more than one stellar component. Despite this, binary stars have often been avoided by programs searching for planets. Discovery of giant planets in compact binary systems would indirectly probe the timescales of planet formation, an important quantity in determining by which processes planets form. A new observing method has been developed to perform very high precision differ- ential astronrletry on bright binary stars with separations in the range of = 0.1 - 1.0 arcseconds.