William Doberck – Double Star Astronomer
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Astronomie in Theorie Und Praxis 8. Auflage in Zwei Bänden Erik Wischnewski
Astronomie in Theorie und Praxis 8. Auflage in zwei Bänden Erik Wischnewski Inhaltsverzeichnis 1 Beobachtungen mit bloßem Auge 37 Motivation 37 Hilfsmittel 38 Drehbare Sternkarte Bücher und Atlanten Kataloge Planetariumssoftware Elektronischer Almanach Sternkarten 39 2 Atmosphäre der Erde 49 Aufbau 49 Atmosphärische Fenster 51 Warum der Himmel blau ist? 52 Extinktion 52 Extinktionsgleichung Photometrie Refraktion 55 Szintillationsrauschen 56 Angaben zur Beobachtung 57 Durchsicht Himmelshelligkeit Luftunruhe Beispiel einer Notiz Taupunkt 59 Solar-terrestrische Beziehungen 60 Klassifizierung der Flares Korrelation zur Fleckenrelativzahl Luftleuchten 62 Polarlichter 63 Nachtleuchtende Wolken 64 Haloerscheinungen 67 Formen Häufigkeit Beobachtung Photographie Grüner Strahl 69 Zodiakallicht 71 Dämmerung 72 Definition Purpurlicht Gegendämmerung Venusgürtel Erdschattenbogen 3 Optische Teleskope 75 Fernrohrtypen 76 Refraktoren Reflektoren Fokus Optische Fehler 82 Farbfehler Kugelgestaltsfehler Bildfeldwölbung Koma Astigmatismus Verzeichnung Bildverzerrungen Helligkeitsinhomogenität Objektive 86 Linsenobjektive Spiegelobjektive Vergütung Optische Qualitätsprüfung RC-Wert RGB-Chromasietest Okulare 97 Zusatzoptiken 100 Barlow-Linse Shapley-Linse Flattener Spezialokulare Spektroskopie Herschel-Prisma Fabry-Pérot-Interferometer Vergrößerung 103 Welche Vergrößerung ist die Beste? Blickfeld 105 Lichtstärke 106 Kontrast Dämmerungszahl Auflösungsvermögen 108 Strehl-Zahl Luftunruhe (Seeing) 112 Tubusseeing Kuppelseeing Gebäudeseeing Montierungen 113 Nachführfehler -
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. -
Double and Multiple Star Measurements in the Northern Sky with a 10” Newtonian and a Fast CCD Camera in 2006 Through 2009
Vol. 6 No. 3 July 1, 2010 Journal of Double Star Observations Page 180 Double and Multiple Star Measurements in the Northern Sky with a 10” Newtonian and a Fast CCD Camera in 2006 through 2009 Rainer Anton Altenholz/Kiel, Germany e-mail: rainer.anton”at”ki.comcity.de Abstract: Using a 10” Newtonian and a fast CCD camera, recordings of double and multiple stars were made at high frame rates with a notebook computer. From superpositions of “lucky images”, measurements of 139 systems were obtained and compared with literature data. B/w and color images of some noteworthy systems are also presented. mented double stars, as will be described in the next Introduction section. Generally, I used a red filter to cope with By using the technique of “lucky imaging”, seeing chromatic aberration of the Barlow lens, as well as to effects can strongly be reduced, and not only the reso- reduce the atmospheric spectrum. For systems with lution of a given telescope can be pushed to its limits, pronounced color contrast, I also made recordings but also the accuracy of position measurements can be with near-IR, green and blue filters in order to pro- better than this by about one order of magnitude. This duce composite images. This setup was the same as I has already been demonstrated in earlier papers in used with telescopes under the southern sky, and as I this journal [1-3]. Standard deviations of separation have described previously [1-3]. Exposure times varied measurements of less than +/- 0.05 msec were rou- between 0.5 msec and 100 msec, depending on the tinely obtained with telescopes of 40 or 50 cm aper- star brightness, and on the seeing. -
A Calibration of the 85 Peg Binary System
A&A 392, 529–533 (2002) Astronomy DOI: 10.1051/0004-6361:20020962 & c ESO 2002 Astrophysics A calibration of the 85 Peg binary system J. Fernandes1,P.Morel2, and Y. Lebreton3 1 Observat´orio Astron´omico da Universidade de Coimbra, Santa Clara, 3040 Coimbra, Portugal and Departamento de Matem´atica da Faculdade de Ciˆencias e Tecnologia da Universidade de Coimbra, Portugal 2 D´epartement Cassini, UMR CNRS 6529, Observatoire de la Cˆote d’Azur, BP 4229, 06304 Nice Cedex 4, France 3 GEPI, Observatoire de Paris Meudon, 92195 Meudon, France Received 28 September 2001 / Accepted 11 June 2002 Abstract. We have calibrated the initial abundances, age and mixing-length parameters of the visual binary system 85 Pegasi. We obtain an age t85 Peg = 9 345 500 Myr, masses mA = 0:88 0:01 M and mB = 0:55 0:02 M , an initial helium mass = : : Fe = − : : Λ = : : fraction Yi 0 25 0 01, an initial metallicity [ H ]i 0 185 0 054 and mixing-length parameters A 1 80 0 05 and ΛB = 2:14 0:10. We find that, as already proposed, 85 Peg B is itself a binary. The mass of the unseen companion is mb ≈ 0:11 M . Key words. stars: binaries: visual – stars: evolution – stars: fundamental parameters – stars: individual: 85 Peg 1. Introduction massive than 85 Peg A the brighter one (e.g. Slocum 1915; Hall 1948; Underhill 1963). This was found again by Martin & The calibration of a binary system is based on the adjustment Fe Mignard (1998) on the basis of Hipparcos observations. -
UNSC Science and Technology Command
UNSC Science and Technology Command Earth Survey Catalogue: Official Name/(Common) Star System Distance Coordinates Remarks/Status 18 Scorpii {TCP:p351} 18 Scorpii {Fact} 45.7 LY 16h 15m 37s Diameter: 1,654,100km (1.02R*) {Fact} -08° 22' 06" {Fact} Spectral Class: G2 Va {Fact} Surface Temp.: 5,800K {Fact} 18 Scorpii ?? (Falaknuma) 18 Scorpii {Fact} 45.7 LY 16h 15m 37s UNSC HQ base on world. UNSC {TCP:p351} {Fact} -08° 22' 06" recruitment center in the city of Halkia. {TCP:p355} Constellation: Scorpio 111 Tauri 111 Tauri {Fact} 47.8 LY 05h:24m:25.46s Diameter: 1,654,100km (1.19R*) {Fact} +17° 23' 00.72" {Fact} Spectral Class: F8 V {Fact} Surface Temp.: 6,200K {Fact} Constellation: Taurus 111 Tauri ?? (Victoria) 111 Tauri {Fact} 47.8 LY 05:24:25.4634 UNSC colony. {GoO:p31} {Fact} +17° 23' 00.72" Constellation: Taurus Location of a rebel cell at Camp New Hope in 2531. {GoO:p31} 51 Pegasi {Fact} 51 Pegasi {Fact} 50.1 LY 22h:57m:28s Diameter: 1,668,000km (1.2R*) {Fact} +20° 46' 7.8" {Fact} Spectral Class: G4 (yellow- orange) {Fact} Surface Temp.: Constellation: Pegasus 51 Pegasi-B (Bellerophon) 51 Pegasi 50.1 LY 22h:57m:28s Gas giant planet in the 51 Pegasi {Fact} +20° 46' 7.8" system informally named Bellerophon. Diameter: 196,000km. {Fact} Located on the edge of UNSC territory. {GoO:p15} Its moon, Pegasi Delta, contained a Covenant deuterium/tritium refinery destroyed by covert UNSC forces in 2545. {GoO:p13} Constellation: Pegasus 51 Pegasi-B-1 (Pegasi 51 Pegasi 50.1 LY 22h:57m:28s Moon of the gas giant planet 51 Delta) {GoO:p13} +20° 46' 7.8" Pegasi-B in the 51 Pegasi star Constellation: Pegasus system; a Covenant stronghold on the edge of UNSC territory. -
Macrocosmo Nº33
HA MAIS DE DOIS ANOS DIFUNDINDO A ASTRONOMIA EM LÍNGUA PORTUGUESA K Y . v HE iniacroCOsmo.com SN 1808-0731 Ano III - Edição n° 33 - Agosto de 2006 * t i •■•'• bSÈlÈWW-'^Sif J fé . ’ ' w s » ws» ■ ' v> í- < • , -N V Í ’\ * ' "fc i 1 7 í l ! - 4 'T\ i V ■ }'- ■t i' ' % r ! ■ 7 ji; ■ 'Í t, ■ ,T $ -f . 3 j i A 'A ! : 1 l 4/ í o dia que o ceu explodiu! t \ Constelação de Andrômeda - Parte II Desnudando a princesa acorrentada £ Dicas Digitais: Softwares e afins, ATM, cursos online e publicações eletrônicas revista macroCOSMO .com Ano III - Edição n° 33 - Agosto de I2006 Editorial Além da órbita de Marte está o cinturão de asteróides, uma região povoada com Redação o material que restou da formação do Sistema Solar. Longe de serem chamados como simples pedras espaciais, os asteróides são objetos rochosos e/ou metálicos, [email protected] sem atmosfera, que estão em órbita do Sol, mas são pequenos demais para serem considerados como planetas. Até agora já foram descobertos mais de 70 Diretor Editor Chefe mil asteróides, a maior parte situados no cinturão de asteróides entre as órbitas Hemerson Brandão de Marte e Júpiter. [email protected] Além desse cinturão podemos encontrar pequenos grupos de asteróides isolados chamados de Troianos que compartilham a mesma órbita de Júpiter. Existem Editora Científica também aqueles que possuem órbitas livres, como é o caso de Hidalgo, Apolo e Walkiria Schulz Ícaro. [email protected] Quando um desses asteróides cruza a nossa órbita temos as crateras de impacto. A maior cratera visível de nosso planeta é a Meteor Crater, com cerca de 1 km de Diagramadores diâmetro e 600 metros de profundidade. -
Hydrogen Subordinate Line Emission at the Epoch of Cosmological Recombination M
Astronomy Reports, Vol. 47, No. 9, 2003, pp. 709–716. Translated from Astronomicheski˘ı Zhurnal, Vol. 80, No. 9, 2003, pp. 771–779. Original Russian Text Copyright c 2003 by Burgin. Hydrogen Subordinate Line Emission at the Epoch of Cosmological Recombination M. S. Burgin Astro Space Center, Lebedev Physical Institute, Russian Academy of Sciences, Profsoyuznaya ul. 84/32, Moscow, 117997 Russia Received December 10, 2002; in final form, March 14, 2003 Abstract—The balance equations for the quasi-stationary recombination of hydrogen plasma in a black- body radiation field are solved. The deviations of the excited level populations from equilibrium are computed and the rates of uncompensated line transitions determined. The expressions obtained are stable for computations of arbitrarily small deviations from equilibrium. The average number of photons emitted in hydrogen lines per irreversible recombination is computed for plasma parameters corresponding to the epoch of cosmological recombination. c 2003 MAIK “Nauka/Interperiodica”. 1. INTRODUCTION of this decay is responsible for the appreciable differ- When the cosmological expansion of the Universe ence between the actual degree of ionization and the lowered the temperature sufficiently, the initially ion- value correspondingto the Saha –Boltzmann equi- ized hydrogen recombined. According to [1, 2], an librium. A detailed analysis of processes affectingthe appreciable fraction of the photons emitted at that recombination rate and computations of the temporal time in subordinate lines survive to the present, lead- behavior of the degree of ionization for various sce- ingto the appearance of spectral lines in the cosmic narios for the cosmological expansion are presented background (relict) radiation. Measurements of the in [5, 6]. -
Venus and Mercury Are Back
FORT WORTH ASTRONOMICAL SOCIETY (est. 1949) NOVEMBER 2011 Venus and Mercury Are Back In This Issue November Club Calendar ... 2 Night Sky Chart ... 3 Cloudy Night Library ... 4 The Gray Cubicle You Want To Work In ... 6 Clues From Ancient Light ... 7 This Month’s Constellation - Pisces ... 8 Image courtesy of science.nasa.gov PRIME FOCUS - FORT WORTH ASTRONOMICAL SOCIETY NOVEMBER 2011 November 2011 Sun Mon Tue Wed Thu Fri Sat 1 2 3 4 5 1st Quarter Moon 11:38pm 6 7 8 9 10 11 12 Day Light Saving Asteroid 2005 Neptune is Full Moon Veterans Day ends at 2am YU55 passes only stationary 2:16pm 202,000mi from Earth 13 14 15 16 17 18 19 Leonid meteor Last Quarter shower peaks Moon 9:09am FWAS Monthly Meeting 20 21 22 23 24 25 26 Thanksgiving Day New Moon 12:10am Mercury is stationary 27 28 29 30 2 PRIME FOCUS - FORT WORTH ASTRONOMICAL SOCIETY NOVEMBER 2011 November Night Sky November 15, 2011 @ 10:00pm CST Sky chart coutesy of Chris Peat and http://www.heavens-above.com/ Planet Viewing This Month Mercury is in the western evening sky and remains about 20 from Venus for the first half of the month. Venus sits low in the southwestern evening twilight. Mars is mostly out of the picture but can be spotted in Leo early in the morning. Jupiter has just passed opposition and still traverses the sky all evening, setting near dawn. Although the angle of ecliptic favors the Northern Hemisphere, Saturn can be seen in the pre-dawn sky, in Virgo. -
Curriculum Vitae Date: 4/03/2013 Initials
Curriculum Vitae Date: 4/03/2013 Initials: Gordon Arthur Hunter WALKER Born: 30 January 1936 Married: Sigrid Helene Fischer, April 1962 Children: Nicholas and Eric Languages: English, French, and German. POST-SECONDARY EDUCATION University of Edinburgh Hon.B.Sc. Natural Philosophy 1958 University of Cambridge (Caius) Ph.D. Astrophysics 1962 PROFESSIONAL EMPLOYMENT Radcliffe Observatory, Pretoria Research Assistant 1960-61 DAO, Victoria NRC Fellow 1962-63 DAO, Victoria Scientific Officer 3 1963-69 University of Texas Visiting Lecturer 1965 (Spring) University of Victoria Visiting Lecturer 1966 (Spring) UBC Associate Professor April 1, 1969 Director, Institute 1972-78 Astronomy and Space Science Professor July 1, 1974-97 Professor Emeritus July 1 1997 { HIA/NRC Guest-worker 1998 { UVic Adjunct Professor April 23 2004 { INTERNATIONAL PROJECTS Scientific Advisory Committee of the CFHT 1972-79 Project Scientist for `Starlab' an Australian, Canadian, NASA, space telescope proposal until Canada withdrew in 1984 CFHT Board of Directors 1986-91 Canadian Project Scientist (1989-90): EUVITA - far ultraviolet astronomical satellite experiment joint with USSR, Switzerland, USA. Canadian Project Scientist (1990{97): Gemini - twin 8 metre optical telescopes (1 in Hawaii, 1 in Chile) joint with USA, U.K., Chile, Australia, Argentina, Brazil. Gemini Scientific Advisory Committee 1991{97 Gemini Board of Directors 1991{97 1 MOST Science team (1997{2009): a Canadian satellite launched in 2003 for ultra-precise photom- etry of bright stars, with collaboration from Austria. Gemini/NSF Visiting Committee 2004 AURA Source Selection Board for future Gemini Instrumentation 2004 TMT - chair HROS Review Panel 2005 chair Gemini Source Selection Board for HRNIRS 2005 chair Gemini Source Selection Board for PRVS 2006 member SPIRou Preliminary Design Revue Committee 2012 - a high resolution visible/infrared spectropolarimeter proposed for CFHT RESEARCH CAREER My fascination with astronomy began at age 7 when my father explained that stars were very distant suns. -
Numbers 1 to 100
Numbers 1 to 100 PDF generated using the open source mwlib toolkit. See http://code.pediapress.com/ for more information. PDF generated at: Tue, 30 Nov 2010 02:36:24 UTC Contents Articles −1 (number) 1 0 (number) 3 1 (number) 12 2 (number) 17 3 (number) 23 4 (number) 32 5 (number) 42 6 (number) 50 7 (number) 58 8 (number) 73 9 (number) 77 10 (number) 82 11 (number) 88 12 (number) 94 13 (number) 102 14 (number) 107 15 (number) 111 16 (number) 114 17 (number) 118 18 (number) 124 19 (number) 127 20 (number) 132 21 (number) 136 22 (number) 140 23 (number) 144 24 (number) 148 25 (number) 152 26 (number) 155 27 (number) 158 28 (number) 162 29 (number) 165 30 (number) 168 31 (number) 172 32 (number) 175 33 (number) 179 34 (number) 182 35 (number) 185 36 (number) 188 37 (number) 191 38 (number) 193 39 (number) 196 40 (number) 199 41 (number) 204 42 (number) 207 43 (number) 214 44 (number) 217 45 (number) 220 46 (number) 222 47 (number) 225 48 (number) 229 49 (number) 232 50 (number) 235 51 (number) 238 52 (number) 241 53 (number) 243 54 (number) 246 55 (number) 248 56 (number) 251 57 (number) 255 58 (number) 258 59 (number) 260 60 (number) 263 61 (number) 267 62 (number) 270 63 (number) 272 64 (number) 274 66 (number) 277 67 (number) 280 68 (number) 282 69 (number) 284 70 (number) 286 71 (number) 289 72 (number) 292 73 (number) 296 74 (number) 298 75 (number) 301 77 (number) 302 78 (number) 305 79 (number) 307 80 (number) 309 81 (number) 311 82 (number) 313 83 (number) 315 84 (number) 318 85 (number) 320 86 (number) 323 87 (number) 326 88 (number) -
Biological Damage of Uv Radiation in Environments Of
BIOLOGICAL DAMAGE OF UV RADIATION IN ENVIRONMENTS OF F-TYPE STARS by SATOKO SATO Presented to the Faculty of the Graduate School of The University of Texas at Arlington in Partial Fulfillment of the Requirements for the Degree of DOCTOR OF PHILOSOPHY THE UNIVERSITY OF TEXAS AT ARLINGTON May 2014 Copyright c by Satoko Sato 2014 All Rights Reserved I dedicate this to my daughter Akari Y. Sato. Acknowledgements First of all, I would like to thank my supervising professor Dr. Manfred Cuntz. His advice on my research and academic life has always been invaluable. I would have given up the Ph.D. bound program without his encouragement and generous support as the supervising professor during a few difficult times in my life. I would like to thank Dr. Wei Chen, Dr. Yue Deng, Dr. Zdzislaw E. Musielak, and Dr. Sangwook Park for their interest in my research and for their time to serve in my committee. Next, I would like to acknowledge my research collaborators at University of Guanajuato, Cecilia M. Guerra Olvera, Dr. Dennis Jack, and Dr. Klaus-Peter Schr¨oder,for providing me the data of F-type evolutionary tracks and UV spectra. I would also like to express my deep gratitude to my parents, Hideki and Kumiko Yakushigawa, for their enormous support in many ways in my entire life, and to my sister, Tomoko Yakushigawa, for her constant encouragement to me. I am grateful to my husband, Makito Sato, and my daughter, Akari Y. Sato. Their presence always gives me strength. I am thankful to my parents-in-law, Hisao and Tsuguho Sato, and my grand-parents-in-law, Kanji and Ayako Momoi, for their financial support and prayers. -
Theory of Stellar Atmospheres
© Copyright, Princeton University Press. No part of this book may be distributed, posted, or reproduced in any form by digital or mechanical means without prior written permission of the publisher. EXTENDED BIBLIOGRAPHY References [1] D. Abbott. The terminal velocities of stellar winds from early{type stars. Astrophys. J., 225, 893, 1978. [2] D. Abbott. The theory of radiatively driven stellar winds. I. A physical interpretation. Astrophys. J., 242, 1183, 1980. [3] D. Abbott. The theory of radiatively driven stellar winds. II. The line acceleration. Astrophys. J., 259, 282, 1982. [4] D. Abbott. The theory of radiation driven stellar winds and the Wolf{ Rayet phenomenon. In de Loore and Willis [938], page 185. Astrophys. J., 259, 282, 1982. [5] D. Abbott. Current problems of line formation in early{type stars. In Beckman and Crivellari [358], page 279. [6] D. Abbott and P. Conti. Wolf{Rayet stars. Ann. Rev. Astr. Astrophys., 25, 113, 1987. [7] D. Abbott and D. Hummer. Photospheres of hot stars. I. Wind blan- keted model atmospheres. Astrophys. J., 294, 286, 1985. [8] D. Abbott and L. Lucy. Multiline transfer and the dynamics of stellar winds. Astrophys. J., 288, 679, 1985. [9] D. Abbott, C. Telesco, and S. Wolff. 2 to 20 micron observations of mass loss from early{type stars. Astrophys. J., 279, 225, 1984. [10] C. Abia, B. Rebolo, J. Beckman, and L. Crivellari. Abundances of light metals and N I in a sample of disc stars. Astr. Astrophys., 206, 100, 1988. [11] M. Abramowitz and I. Stegun. Handbook of Mathematical Functions. (Washington, DC: U.S. Government Printing Office), 1972.