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A&A 619, A61 (2018) Astronomy https://doi.org/10.1051/0004-6361/201833747 & c ESO 2018 Astrophysics Dramatic change in the boundary layer in the symbiotic recurrent nova T Coronae Borealis G. J. M. Luna1,2,3 , K. Mukai4,5, J. L. Sokoloski6, T. Nelson7, P. Kuin8, A. Segreto9, G. Cusumano9, M. Jaque Arancibia10,11, and N. E. Nuñez11 1 CONICET-Universidad de Buenos Aires, Instituto de Astronomía y Física del Espacio (IAFE), Av. Inte. Güiraldes 2620, C1428ZAA Buenos Aires, Argentina e-mail: [email protected] 2 Universidad de Buenos Aires, Facultad de Ciencias Exactas y Naturales, Buenos Aires, Argentina 3 Universidad Nacional Arturo Jauretche, Av. Calchaquí 6200, F. Varela, Buenos Aires, Argentina 4 CRESST and X-ray Astrophysics Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA 5 Department of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, MD 21250, USA 6 Columbia Astrophysics Lab 550 W 120th St., 1027 Pupin Hall, MC 5247 Columbia University, New York, NY 10027, USA 7 Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260, USA 8 University College London, Mullard Space Science Laboratory, Holmbury St. Mary, Dorking RH5 6NT, UK 9 INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, Via U. La Malfa 153, 90146 Palermo, Italy 10 Departamento de Física y Astronomía, Universidad de La Serena, Av. Cisternas 1200, La Serena, Chile 11 Instituto de Ciencias Astronómicas, de la Tierra y del Espacio (ICATE-CONICET), Av. España Sur 1512, J5402DSP San Juan, Argentina Received 29 June 2018 / Accepted 23 August 2018 ABSTRACT A sudden increase in the rate at which material reaches the most internal part of an accretion disk, i.e., the boundary layer, can change its structure dramatically. -
Extensional Tectonics in Tempe Terra 8 May 2006
Extensional tectonics in Tempe Terra 8 May 2006 Tectonic processes (extensional stresses, in this case) have led to the development of these grabens. After the tectonic activity, other processes reshaped the landscape. In the scene, the results of weathering and mass transport can be seen. Due to erosion, the surface has been smoothed, giving formerly sharp edges a rounded appearance. Such terrain is called "fretted terrain" and is characteristic for the transition of highland to lowland. The valleys and grabens are 5 to 10 kilometres wide and up to 1500 metres deep. Along the graben flanks, the layering of the bedrock is exposed. The lineations on the valley floors are attributed to a slow viscous movement of material, Extensional tectonics in Tempe Terra. presumably in connection with ice. These lineations and indications of possible ice underneath the surface lead scientists to assume that the structures are rock glaciers or similar phenomena These images, taken by the High Resolution known from alpine regions on Earth. Stereo Camera (HRSC) on board ESA's Mars Express spacecraft, show the tectonic 'grabens' in The stereo and colour capabilities, and the high- Tempe Terra, a geologically complex region that is resolution coverage of extended areas, provided by part of the old Martian highlands. the HRSC camera allow for improved study of the complex geologic evolution of the Red Planet. The The HRSC obtained these images during orbit Mars Express HRSC camera gives scientists the 1180 on 19 December 2004 with a ground opportunity to better understand the tectonics of resolution of approximately 16.5 metres per pixel. -
136, June 2008
British Astronomical Association VARIABLE STAR SECTION CIRCULAR No 136, June 2008 Contents Group Photograph, AAVSO/BAAVSS meeting ........................ inside front cover From the Director ............................................................................................... 1 Eclipsing Binary News ....................................................................................... 4 Experiments in the use of a DSLR camera for V photometry ............................ 5 Joint Meeting of the AAVSO and the BAAVSS ................................................. 8 Coordinated HST and Ground Campaigns on CVs ............................... 8 Eclipsing Binaries - Observational Challenges .................................................. 9 Peer to Peer Astronomy Education .................................................................. 10 AAVSO Acronyms De-mystified in Fifteen Minutes ...................................... 11 New Results on SW Sextantis Stars and Proposed Observing Campaign ........ 12 A Week in the Life of a Remote Observer ........................................................ 13 Finding Eclipsing Binaries in NSVS Data ......................................................... 13 British Variable Star Associations 1848-1908 .................................................. 14 “Chasing Rainbows” (The European Amateur Spectroscopy Scene) .............. 15 Long Term Monitoring and the Carbon Miras ................................................. 18 Cataclysmic Variables from Large Surveys: A Silent Revolution -
Martian Crater Morphology
ANALYSIS OF THE DEPTH-DIAMETER RELATIONSHIP OF MARTIAN CRATERS A Capstone Experience Thesis Presented by Jared Howenstine Completion Date: May 2006 Approved By: Professor M. Darby Dyar, Astronomy Professor Christopher Condit, Geology Professor Judith Young, Astronomy Abstract Title: Analysis of the Depth-Diameter Relationship of Martian Craters Author: Jared Howenstine, Astronomy Approved By: Judith Young, Astronomy Approved By: M. Darby Dyar, Astronomy Approved By: Christopher Condit, Geology CE Type: Departmental Honors Project Using a gridded version of maritan topography with the computer program Gridview, this project studied the depth-diameter relationship of martian impact craters. The work encompasses 361 profiles of impacts with diameters larger than 15 kilometers and is a continuation of work that was started at the Lunar and Planetary Institute in Houston, Texas under the guidance of Dr. Walter S. Keifer. Using the most ‘pristine,’ or deepest craters in the data a depth-diameter relationship was determined: d = 0.610D 0.327 , where d is the depth of the crater and D is the diameter of the crater, both in kilometers. This relationship can then be used to estimate the theoretical depth of any impact radius, and therefore can be used to estimate the pristine shape of the crater. With a depth-diameter ratio for a particular crater, the measured depth can then be compared to this theoretical value and an estimate of the amount of material within the crater, or fill, can then be calculated. The data includes 140 named impact craters, 3 basins, and 218 other impacts. The named data encompasses all named impact structures of greater than 100 kilometers in diameter. -
First Science with the Keck Interferometer Nuller R
The Astrophysical Journal, 677:1253Y1267, 2008 April 20 # 2008. The American Astronomical Society. All rights reserved. Printed in U.S.A. MILLIARCSECOND N-BAND OBSERVATIONS OF THE NOVA RS OPHIUCHI: FIRST SCIENCE WITH THE KECK INTERFEROMETER NULLER R. K. Barry,1,2 W. C. Danchi,1 W. A. Traub,3 J. L. Sokoloski,4 J. P. Wisniewski,1 E. Serabyn,3 M. J. Kuchner,1 R. Akeson,5 E. Appleby,6 J. Bell,6 A. Booth,3 H. Brandenburg,5 M. Colavita,3 S. Crawford,3 M. Creech-Eakman,3 W. Dahl,6 C. Felizardo,5 J. Garcia,3 J. Gathright,6 M. A. Greenhouse,1 J. Herstein,5 E. Hovland,3 M. Hrynevych,6 C. Koresko,3 R. Ligon,3 B. Mennesson,3 R. Millan-Gabet,5 D. Morrison,6 D. Palmer,3 T. Panteleeva,6 S. Ragland,6 M. Shao,3 R. Smythe,3 K. Summers,6 M. Swain,3 K. Tsubota,6 C. Tyau,6 E. Wetherell,6 P. Wizinowich,6 J. Woillez,6 and G. Vasisht3 Received 2007 August 9; accepted 2008 January 9 ABSTRACT We report observations of the nova RS Ophiuchi (RS Oph) using the Keck Interferometer Nuller (KIN), approxi- mately 3.8 days following the most recent outburst that occurred on 2006 February 12. These observations represent the first scientific results from the KIN, which operates in N band from 8 to 12.5 m in a nulling mode. The nulling technique is the sparse aperture equivalent of the conventional coronagraphic technique used in filled aperture tele- scopes. In this mode the stellar light itself is suppressed by a destructive fringe, effectively enhancing the contrast of the circumstellar material located near the star. -
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. -
Exoplanet Community Report
JPL Publication 09‐3 Exoplanet Community Report Edited by: P. R. Lawson, W. A. Traub and S. C. Unwin National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology Pasadena, California March 2009 The work described in this publication was performed at a number of organizations, including the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). Publication was provided by the Jet Propulsion Laboratory. Compiling and publication support was provided by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not constitute or imply its endorsement by the United States Government, or the Jet Propulsion Laboratory, California Institute of Technology. © 2009. All rights reserved. The exoplanet community’s top priority is that a line of probeclass missions for exoplanets be established, leading to a flagship mission at the earliest opportunity. iii Contents 1 EXECUTIVE SUMMARY.................................................................................................................. 1 1.1 INTRODUCTION...............................................................................................................................................1 1.2 EXOPLANET FORUM 2008: THE PROCESS OF CONSENSUS BEGINS.....................................................2 -
High-Resolution N-Band Observations of the Nova RS Ophiuchi with the Keck Interferometer Nuller
High-Resolution N-Band Observations of the Nova RS Ophiuchi with the Keck Interferometer Nuller ABSTRACT We report new observations of the nova RS Ophiuchi (RS Oph) using the Keck Interferometer Nulling Instrument, approximately 3.8 days following the most recent outburst that occurred on 2006 February 12. The Keck Interferome- ter Nuller (KIN) operates in K-band from 8 to 12.5 pm in a nulling mode, which means that the central broad-band interference fringe is a dark fringe - with an angular width of 25 mas at mid band - rather than the bright fringe used ill a con- ventional optical interferometer. In this mode the stellar light itself is suppressed by the destructive fringe, effectively enhancing the contrast of the circumstellar material located near the star. By subsequently shifting the neighboring bright fringe onto the center of the source brightness distribution and integrating, a second spatial regime dominated by light from the central portion of the source is almost simultaneously sampled. The nulling technique is the sparse aperture equivalent of the conventional corongraphic technique used in filled aperture tele- scopes. By fitting the unique KIK inner and outer spatial regime data, we have obtained an angular size of the mid-infrared continuum of 6.2, 4.0. or 5.4 mas for a disk profile, gaussian profile (fwhm), and shell profile respectively. The data show evidence of enhanced neutral atomic hydrogen emission located in the inner spatial regime relative to the outer regime. There is also evidence of a 9.7 micron silicate feature seen outside of this region. -
Glossary of Lunar Terminology
Glossary of Lunar Terminology albedo A measure of the reflectivity of the Moon's gabbro A coarse crystalline rock, often found in the visible surface. The Moon's albedo averages 0.07, which lunar highlands, containing plagioclase and pyroxene. means that its surface reflects, on average, 7% of the Anorthositic gabbros contain 65-78% calcium feldspar. light falling on it. gardening The process by which the Moon's surface is anorthosite A coarse-grained rock, largely composed of mixed with deeper layers, mainly as a result of meteor calcium feldspar, common on the Moon. itic bombardment. basalt A type of fine-grained volcanic rock containing ghost crater (ruined crater) The faint outline that remains the minerals pyroxene and plagioclase (calcium of a lunar crater that has been largely erased by some feldspar). Mare basalts are rich in iron and titanium, later action, usually lava flooding. while highland basalts are high in aluminum. glacis A gently sloping bank; an old term for the outer breccia A rock composed of a matrix oflarger, angular slope of a crater's walls. stony fragments and a finer, binding component. graben A sunken area between faults. caldera A type of volcanic crater formed primarily by a highlands The Moon's lighter-colored regions, which sinking of its floor rather than by the ejection of lava. are higher than their surroundings and thus not central peak A mountainous landform at or near the covered by dark lavas. Most highland features are the center of certain lunar craters, possibly formed by an rims or central peaks of impact sites. -
Appendix I Lunar and Martian Nomenclature
APPENDIX I LUNAR AND MARTIAN NOMENCLATURE LUNAR AND MARTIAN NOMENCLATURE A large number of names of craters and other features on the Moon and Mars, were accepted by the IAU General Assemblies X (Moscow, 1958), XI (Berkeley, 1961), XII (Hamburg, 1964), XIV (Brighton, 1970), and XV (Sydney, 1973). The names were suggested by the appropriate IAU Commissions (16 and 17). In particular the Lunar names accepted at the XIVth and XVth General Assemblies were recommended by the 'Working Group on Lunar Nomenclature' under the Chairmanship of Dr D. H. Menzel. The Martian names were suggested by the 'Working Group on Martian Nomenclature' under the Chairmanship of Dr G. de Vaucouleurs. At the XVth General Assembly a new 'Working Group on Planetary System Nomenclature' was formed (Chairman: Dr P. M. Millman) comprising various Task Groups, one for each particular subject. For further references see: [AU Trans. X, 259-263, 1960; XIB, 236-238, 1962; Xlffi, 203-204, 1966; xnffi, 99-105, 1968; XIVB, 63, 129, 139, 1971; Space Sci. Rev. 12, 136-186, 1971. Because at the recent General Assemblies some small changes, or corrections, were made, the complete list of Lunar and Martian Topographic Features is published here. Table 1 Lunar Craters Abbe 58S,174E Balboa 19N,83W Abbot 6N,55E Baldet 54S, 151W Abel 34S,85E Balmer 20S,70E Abul Wafa 2N,ll7E Banachiewicz 5N,80E Adams 32S,69E Banting 26N,16E Aitken 17S,173E Barbier 248, 158E AI-Biruni 18N,93E Barnard 30S,86E Alden 24S, lllE Barringer 29S,151W Aldrin I.4N,22.1E Bartels 24N,90W Alekhin 68S,131W Becquerei -
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, -
N95- 27078 13 Discussion on Selected Symbiotic Stars
N95- 27078 13 DISCUSSION ON SELECTED SYMBIOTIC STARS R. Viotti and M. Hack I. INTRODUCTION made of its variations" (Mayall, 1969). This pessimistic remark should be consid- Because of its large variety of aspects, the ered as a note of caution for those involved in symbiotic phenomenon is not very suitable for the interpretation of the observations. In the a statistical treatment. It is also not clear following, we shall discuss a number of indi- whether symbiotic stars really represent a vidual symbiotic stars for which the amount of homogeneous group of astrophysical objects or observational data is large enough to draw a a collection of objects of different natures but rather complete picture of their general behav- showing similar phenomena. However, as al- ior and to make consistent models. We shall ready discussed in the introduction to the sym- especially illustrate the necessary steps toward biotic stars, in this monograph we are espe- an empirical model and take the discussion of cially interested in the symbiotic phenomenon, the individual objects as a useful occasion to i.e., in those physical processes occurring in describe different techniques of diagnosis. the atmosphere of each individual object and in their time dependence. Such a research can be I1. Z ANDROMEDAE AND THE DIAGNOS- performed through the detailed analysis of TICS OF THE SYMBIOTIC STARS individual objects. This study should be done for a time long enough to cover all the different II.A. INTRODUCTION phases of their activity, in all the spectral ranges. Since the typical time scale of the symbiotic phenomena is up to several years and Z And has been considered as the prototype decades, this represents a problem since, for of the symbiotic stars, from its light history and instance, making astronomy outside the visual the spectral variation during outburst.