Heber Doust Curtis 1872-1942
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Arxiv:1809.07342V1 [Astro-Ph.SR] 19 Sep 2018
Draft version September 21, 2018 Preprint typeset using LATEX style emulateapj v. 11/10/09 FAR-ULTRAVIOLET ACTIVITY LEVELS OF F, G, K, AND M DWARF EXOPLANET HOST STARS* Kevin France1, Nicole Arulanantham1, Luca Fossati2, Antonino F. Lanza3, R. O. Parke Loyd4, Seth Redfield5, P. Christian Schneider6 Draft version September 21, 2018 ABSTRACT We present a survey of far-ultraviolet (FUV; 1150 { 1450 A)˚ emission line spectra from 71 planet- hosting and 33 non-planet-hosting F, G, K, and M dwarfs with the goals of characterizing their range of FUV activity levels, calibrating the FUV activity level to the 90 { 360 A˚ extreme-ultraviolet (EUV) stellar flux, and investigating the potential for FUV emission lines to probe star-planet interactions (SPIs). We build this emission line sample from a combination of new and archival observations with the Hubble Space Telescope-COS and -STIS instruments, targeting the chromospheric and transition region emission lines of Si III,N V,C II, and Si IV. We find that the exoplanet host stars, on average, display factors of 5 { 10 lower UV activity levels compared with the non-planet hosting sample; this is explained by a combination of observational and astrophysical biases in the selection of stars for radial-velocity planet searches. We demonstrate that UV activity-rotation relation in the full F { M star sample is characterized by a power-law decline (with index α ≈ −1.1), starting at rotation periods & 3.5 days. Using N V or Si IV spectra and a knowledge of the star's bolometric flux, we present a new analytic relationship to estimate the intrinsic stellar EUV irradiance in the 90 { 360 A˚ band with an accuracy of roughly a factor of ≈ 2. -
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. -
Active Galactic Nuclei and Their Neighbours
CCD Photometric Observations of Active Galactic Nuclei and their Neighbours by Traianou Efthalia A dissertation submitted in partial fulfillment of the requirements for the degree of Ptychion (Physics) in Aristotle University of Thessaloniki September 2016 Supervisor: Manolis Plionis, Professor To my loved ones Many thanks to: Manolis Plionis for accepting to be my thesis adviser. ii TABLE OF CONTENTS DEDICATION :::::::::::::::::::::::::::::::::: ii LIST OF FIGURES ::::::::::::::::::::::::::::::: v LIST OF TABLES :::::::::::::::::::::::::::::::: ix LIST OF APPENDICES :::::::::::::::::::::::::::: x ABSTRACT ::::::::::::::::::::::::::::::::::: xi CHAPTER I. Introduction .............................. 1 II. Active Galactic Nuclei ........................ 4 2.1 Early History of AGN’s ..................... 4 2.2 AGN Phenomenology ...................... 7 2.2.1 Seyfert Galaxies ................... 7 2.2.2 Low Ionization Nuclear Emission-Line Regions(LINERS) 10 2.2.3 ULIRGS ........................ 11 2.2.4 Radio Galaxies .................... 12 2.2.5 Quasars or QSO’s ................... 14 2.2.6 Blazars ......................... 15 2.3 The Unification Paradigm .................... 16 2.4 Beyond the Unified Model ................... 18 III. Research Goal and Methodology ................. 21 3.1 Torus ............................... 21 3.2 Ha Balmer Line ......................... 23 3.3 Galaxy-Galaxy Interactions ................... 25 3.4 Our Aim ............................. 27 iii IV. Observations .............................. 29 4.1 The Telescope -
Appendix A: Scientific Notation
Appendix A: Scientific Notation Since in astronomy we often have to deal with large numbers, writing a lot of zeros is not only cumbersome, but also inefficient and difficult to count. Scientists use the system of scientific notation, where the number of zeros is short handed to a superscript. For example, 10 has one zero and is written as 101 in scientific notation. Similarly, 100 is 102, 100 is 103. So we have: 103 equals a thousand, 106 equals a million, 109 is called a billion (U.S. usage), and 1012 a trillion. Now the U.S. federal government budget is in the trillions of dollars, ordinary people really cannot grasp the magnitude of the number. In the metric system, the prefix kilo- stands for 1,000, e.g., a kilogram. For a million, the prefix mega- is used, e.g. megaton (1,000,000 or 106 ton). A billion hertz (a unit of frequency) is gigahertz, although I have not heard of the use of a giga-meter. More rarely still is the use of tera (1012). For small numbers, the practice is similar. 0.1 is 10À1, 0.01 is 10À2, and 0.001 is 10À3. The prefix of milli- refers to 10À3, e.g. as in millimeter, whereas a micro- second is 10À6 ¼ 0.000001 s. It is now trendy to talk about nano-technology, which refers to solid-state device with sizes on the scale of 10À9 m, or about 10 times the size of an atom. With this kind of shorthand convenience, one can really go overboard. -
A New Form of Estimating Stellar Parameters Using an Optimization Approach
A&A 532, A20 (2011) Astronomy DOI: 10.1051/0004-6361/200811182 & c ESO 2011 Astrophysics Modeling nearby FGK Population I stars: A new form of estimating stellar parameters using an optimization approach J. M. Fernandes1,A.I.F.Vaz2, and L. N. Vicente3 1 CFC, Department of Mathematics and Astronomical Observatory, University of Coimbra, Portugal e-mail: [email protected] 2 Department of Production and Systems, University of Minho, Portugal e-mail: [email protected] 3 CMUC, Department of Mathematics, University of Coimbra, Portugal e-mail: [email protected] Received 17 October 2008 / Accepted 27 May 2011 ABSTRACT Context. Modeling a single star with theoretical stellar evolutionary tracks is a nontrivial problem because of a large number of unknowns compared to the number of observations. A current way of estimating stellar age and mass consists of using interpolations in grids of stellar models and/or isochrones, assuming ad hoc values for the mixing length parameter and the metal-to-helium enrichment, which is normally scaled to the solar values. Aims. We present a new method to model the FGK main-sequence of Population I stars. This method is capable of simultaneously estimating a set of stellar parameters, namely the mass, the age, the helium and metal abundances, the mixing length parameter, and the overshooting. Methods. The proposed method is based on the application of a global optimization algorithm (PSwarm) to solve an optimization problem that in turn consists of finding the values of the stellar parameters that lead to the best possible fit of the given observations. -
How Supernovae Became the Basis of Observational Cosmology
Journal of Astronomical History and Heritage, 19(2), 203–215 (2016). HOW SUPERNOVAE BECAME THE BASIS OF OBSERVATIONAL COSMOLOGY Maria Victorovna Pruzhinskaya Laboratoire de Physique Corpusculaire, Université Clermont Auvergne, Université Blaise Pascal, CNRS/IN2P3, Clermont-Ferrand, France; and Sternberg Astronomical Institute of Lomonosov Moscow State University, 119991, Moscow, Universitetsky prospect 13, Russia. Email: [email protected] and Sergey Mikhailovich Lisakov Laboratoire Lagrange, UMR7293, Université Nice Sophia-Antipolis, Observatoire de la Côte d’Azur, Boulevard de l'Observatoire, CS 34229, Nice, France. Email: [email protected] Abstract: This paper is dedicated to the discovery of one of the most important relationships in supernova cosmology—the relation between the peak luminosity of Type Ia supernovae and their luminosity decline rate after maximum light. The history of this relationship is quite long and interesting. The relationship was independently discovered by the American statistician and astronomer Bert Woodard Rust and the Soviet astronomer Yury Pavlovich Pskovskii in the 1970s. Using a limited sample of Type I supernovae they were able to show that the brighter the supernova is, the slower its luminosity declines after maximum. Only with the appearance of CCD cameras could Mark Phillips re-inspect this relationship on a new level of accuracy using a better sample of supernovae. His investigations confirmed the idea proposed earlier by Rust and Pskovskii. Keywords: supernovae, Pskovskii, Rust 1 INTRODUCTION However, from the moment that Albert Einstein (1879–1955; Whittaker, 1955) introduced into the In 1998–1999 astronomers discovered the accel- equations of the General Theory of Relativity a erating expansion of the Universe through the cosmological constant until the discovery of the observations of very far standard candles (for accelerating expansion of the Universe, nearly a review see Lipunov and Chernin, 2012). -
MAS Mentoring Project Overview 2020
Macarthur Astronomical Society Student Projects in Astronomy A Guide of Teachers and Mentors 2020 (c) Macarthur Astronomical Society, 2020 DRAFT The following Project Overviews are based on those suggested by Dr Rahmi Jackson of Broughton Anglican College. The Focus Questions and Issues section should be used by teachers and mentors to guide students in formulating their own questions about the topic. References to the NSW 7-10 Science Syllabus have been included. Note that only those sections relevant are included. For example, subsections a and d may be used, but subsections b and c are omitted as they do not relate to this topic. A generic risk assessment is provided, but schools should ensure that it aligns with school- based policies. MAS Student Projects in Astronomy page 1 Project overviews Semester 1, 2020: Project Stage Technical difficulty 4 5 6 1 The Moons of Jupiter X X X Moderate to high (extension) NOT available Semester 1 2 Astrophotography X X X Moderate to high 3 Light pollution X X Moderate 4 Variable stars X X Moderate to high 5 Spectroscopy X X High 6 A changing lunarscape X X Low to moderate Recommended project 7 Magnitude of stars X X Moderate to high Recommended for technically able students 8 A survey of southern skies X X Low to moderate 9 Double Stars X X Moderate to high 10 The Phases of the Moon X X Low to moderate Recommended project 11 Observing the Sun X X Moderate MAS Student Projects in Astronomy page 2 Project overviews Semester 2, 2020: Project Stage Technical difficulty 4 5 6 1 The Moons of Jupiter -
The Chemical Composition of Solar-Type Stars and Its Impact on the Presence of Planets
The chemical composition of solar-type stars and its impact on the presence of planets Patrick Baumann Munchen¨ 2013 The chemical composition of solar-type stars and its impact on the presence of planets Patrick Baumann Dissertation der Fakultat¨ fur¨ Physik der Ludwig-Maximilians-Universitat¨ Munchen¨ durchgefuhrt¨ am Max-Planck-Institut fur¨ Astrophysik vorgelegt von Patrick Baumann aus Munchen¨ Munchen,¨ den 31. Januar 2013 Erstgutacher: Prof. Dr. Achim Weiss Zweitgutachter: Prof. Dr. Joachim Puls Tag der mündlichen Prüfung: 8. April 2013 Zusammenfassung Wir untersuchen eine mogliche¨ Verbindung zwischen den relativen Elementhaufig-¨ keiten in Sternatmospharen¨ und der Anwesenheit von Planeten um den jeweili- gen Stern. Um zuverlassige¨ Ergebnisse zu erhalten, untersuchen wir ausschließlich sonnenahnliche¨ Sterne und fuhren¨ unsere spektroskopischen Analysen zur Bestim- mung der grundlegenden Parameter und der chemischen Zusammensetzung streng differenziell und relativ zu den solaren Werten durch. Insgesamt untersuchen wir 200 Sterne unter Zuhilfenahme von Spektren mit herausragender Qualitat,¨ die an den modernsten Teleskopen gewonnen wurden, die uns zur Verfugung¨ stehen. Mithilfe der Daten fur¨ 117 sonnenahnliche¨ Sterne untersuchen wir eine mogliche¨ Verbindung zwischen der Oberflachenh¨ aufigkeit¨ von Lithium in einem Stern, seinem Alter und der Wahrscheinlichkeit, dass sich ein oder mehrere Sterne in einer Um- laufbahn um das Objekt befinden. Fur¨ jeden Stern erhalten wir sehr exakte grundle- gende Parameter unter Benutzung einer sorgfaltig¨ zusammengestellten Liste von Fe i- und Fe ii-absorptionslinien, modernen Modellatmospharen¨ und Routinen zum Erstellen von Modellspektren. Die Massen und das Alter der Objekte werden mithilfe von Isochronen bestimmt, was zu sehr soliden relativen Werten fuhrt.¨ Bei jungen Sternen, fur¨ die die Isochronenmethode recht unzuverlssig¨ ist, vergleichen wir verschiedene alternative Methoden. -
Nucleosynthesis in the Stellar Systems Omega Centauri And
CSIRO PUBLISHING Publications of the Astronomical Society of Australia, 2011, 28, 28–37 www.publish.csiro.au/journals/pasa Nucleosynthesis in the Stellar Systems v Centauri and M22 G. S. Da CostaA,C and A. F.MarinoB A Research School of Astronomy & Astrophysics, Australian National University, Mt Stromlo Observatory, via Cotter Rd, Weston, ACT 2611, Australia B Dipartimento di Astronomia, Universita` di Padova, vicolo dell’Osservatorio 2, I-35122 Padova, Italy C Corresponding author. Email: [email protected] Received 2010 August 3, accepted 2010 September 7 Abstract: The stellar system v Centauri (v Cen) is well known for the large range in elemental abundances among its member stars. Recent work has indicated that the globular cluster M22 (NGC 6656) also possesses an internal abundance range, albeit substantially smaller than that in v Cen. Here we compare, as a function of [Fe/H], element-to-iron ratios in the two systems for a number of different elements using data from abundance analyses of red giant branch stars. It appears that the nucleosynthetic enrichment processes were very similar in these two systems despite the substantial difference in total mass. Keywords: globular clusters: general — globular clusters: individual (M22, v Cen) — stars: abundances 1 Introduction tidally disrupted by the Milky Way (e.g., Freeman 1993). The stellar system v Centauri (v Cen) has been known for Bekki & Freeman (2003), for example, have shown that a long time to be different from most other Galactic this is dynamically plausible. The different evolutionary globular clusters because its member stars exhibit a wide environment may then have allowed additional chemical range in the abundance of heavier elements such as iron processes that do not occur in ‘regular’ globular clusters (e. -
Astrophysics in 2006 3
ASTROPHYSICS IN 2006 Virginia Trimble1, Markus J. Aschwanden2, and Carl J. Hansen3 1 Department of Physics and Astronomy, University of California, Irvine, CA 92697-4575, Las Cumbres Observatory, Santa Barbara, CA: ([email protected]) 2 Lockheed Martin Advanced Technology Center, Solar and Astrophysics Laboratory, Organization ADBS, Building 252, 3251 Hanover Street, Palo Alto, CA 94304: ([email protected]) 3 JILA, Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder CO 80309: ([email protected]) Received ... : accepted ... Abstract. The fastest pulsar and the slowest nova; the oldest galaxies and the youngest stars; the weirdest life forms and the commonest dwarfs; the highest energy particles and the lowest energy photons. These were some of the extremes of Astrophysics 2006. We attempt also to bring you updates on things of which there is currently only one (habitable planets, the Sun, and the universe) and others of which there are always many, like meteors and molecules, black holes and binaries. Keywords: cosmology: general, galaxies: general, ISM: general, stars: general, Sun: gen- eral, planets and satellites: general, astrobiology CONTENTS 1. Introduction 6 1.1 Up 6 1.2 Down 9 1.3 Around 10 2. Solar Physics 12 2.1 The solar interior 12 2.1.1 From neutrinos to neutralinos 12 2.1.2 Global helioseismology 12 2.1.3 Local helioseismology 12 2.1.4 Tachocline structure 13 arXiv:0705.1730v1 [astro-ph] 11 May 2007 2.1.5 Dynamo models 14 2.2 Photosphere 15 2.2.1 Solar radius and rotation 15 2.2.2 Distribution of magnetic fields 15 2.2.3 Magnetic flux emergence rate 15 2.2.4 Photospheric motion of magnetic fields 16 2.2.5 Faculae production 16 2.2.6 The photospheric boundary of magnetic fields 17 2.2.7 Flare prediction from photospheric fields 17 c 2008 Springer Science + Business Media. -
| University Microfilms, a XEROX Company , Ann Arbor, Michigan I
THE UPPER CENTAURUS ASSOCIATION Item Type text; Dissertation-Reproduction (electronic) Authors Glaspey, John Warren, 1944- Publisher The University of Arizona. Rights Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author. Download date 06/10/2021 14:40:24 Link to Item http://hdl.handle.net/10150/287700 71-21,990 GLASPEY, John Warren, 1944- THE UPPER CENTAURUS ASSOCIATION. The University of Arizona, Ph.D., 1971 Astronomy | University Microfilms, A XEROX Company , Ann Arbor, Michigan i THIS DISSERTATION HAS BEEN MICROFILMED EXACTLY AS RECEIVED THE UPPER CENTAURUS ASSOCIATION by John Warren Glaspey A Dissertation Submitted to the Faculty of the DEPARTMENT OF ASTRONOMY In Partial Fulfillment of the Requirements For the Degree of DOCTOR OF PHILOSOPHY In the Graduate College THE UNIVERSITY OF ARIZONA 19 7 1 THE UNIVERSITY OF ARIZONA GRADUATE COLLEGE I hereby recommend that this dissertation prepared under my direction by John. Warren Glaspev entitled The Upper Centaurus Association be accepted as fulfilling the dissertation requirement of the degree of Doctor of Philosophy (0 Date 7 After inspection of the final copy of the dissertation, the follov/ing members of the Final Examination Committee concur in its approval and recommend its acceptance:* f~el /Qj / 7 7 t \All^VUA^J/( , (.A ftwh I 0 i 0 , ^ —- _ja 7/ [<D ifl/ This approval and acceptance is contingent on the candidate's adequate performance and defense of this dissertation at the final oral examination. -
Pulsating Components in Binary and Multiple Stellar Systems---A
Research in Astron. & Astrophys. Vol.15 (2015) No.?, 000–000 (Last modified: — December 6, 2014; 10:26 ) Research in Astronomy and Astrophysics Pulsating Components in Binary and Multiple Stellar Systems — A Catalog of Oscillating Binaries ∗ A.-Y. Zhou National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China; [email protected] Abstract We present an up-to-date catalog of pulsating binaries, i.e. the binary and multiple stellar systems containing pulsating components, along with a statistics on them. Compared to the earlier compilation by Soydugan et al.(2006a) of 25 δ Scuti-type ‘oscillating Algol-type eclipsing binaries’ (oEA), the recent col- lection of 74 oEA by Liakos et al.(2012), and the collection of Cepheids in binaries by Szabados (2003a), the numbers and types of pulsating variables in binaries are now extended. The total numbers of pulsating binary/multiple stellar systems have increased to be 515 as of 2014 October 26, among which 262+ are oscillating eclipsing binaries and the oEA containing δ Scuti componentsare updated to be 96. The catalog is intended to be a collection of various pulsating binary stars across the Hertzsprung-Russell diagram. We reviewed the open questions, advances and prospects connecting pulsation/oscillation and binarity. The observational implication of binary systems with pulsating components, to stellar evolution theories is also addressed. In addition, we have searched the Simbad database for candidate pulsating binaries. As a result, 322 candidates were extracted. Furthermore, a brief statistics on Algol-type eclipsing binaries (EA) based on the existing catalogs is given. We got 5315 EA, of which there are 904 EA with spectral types A and F.