Software for Aerospace Educationa Bibliography (Second Edition)
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Pub- Lished a Similar Version 1.0 for the First Generation Apple Macintosh (In Monochrome Only)
The History of Flight Simulator In October 2001 the latest version of Flight Simulator was launched by Microsoft - Flight Simulator 2002 (FS2002). Hundreds of enthusiasts and indeed pilots were involved in its development, programming and beta testing. It would appear that millions of copies have already sold worldwide of what can be considered as the “Eighth Generation” of this hugely successful franchise. So if this is the eighth generation, what about the first and consecutive versions and what did they look like? In this first chapter we thought we should give you a complete overview of the history of Flight Simulator since its first release in 1979. From all those years ago many different versions have been released for a variety of oper- ating systems and machines. In fact, Flight Simulator has become a catalyst for one of the biggest aviation genres in the world. Thanks to the inventiveness and dedication of a student called Bruce Artwick. In the mid-70's Bruce Artwick was an electrical engineering student at the University of Illinois. Being a passionate pilot, it was only natural that the principles of flight became the focus of his studies. In his thesis of May 1975, called ‘A versatile computer-generated dynamic flight display’, he presented the flight model of an aircraft displayed on a computer screen. He proved that a 6800 processor (the first available microcomputer at the time) was able to handle both the arith- metic and the graphic display, needed for real-time flight simulation. In short: the first flight simulator was born. The Birth of Flight Simulator In 1978 Bruce Artwick, together with Stu Moment, founded a software company by the name of subLOGIC and started developing graphics programs for the 6800, 6502, 8080 and other processors. -
Galactic Center: an Improved Astrometric Reference Frame for Stellar Orbits Around the Supermassive Black Hole Shoko Sakai,1 Jessica R
Draft version January 28, 2019 Typeset using LATEX twocolumn style in AASTeX62 The Galactic Center: An Improved Astrometric Reference Frame for Stellar Orbits around the Supermassive Black Hole Shoko Sakai,1 Jessica R. Lu,2 Andrea Ghez,1 Siyao Jia,2 Tuan Do,1 Gunther Witzel,1 Abhimat K. Gautam,1 Aurelien Hees,3, 1 E. Becklin,1 K. Matthews,4 and M. W. Hosek Jr.5 1UCLA Department of Physics and Astronomy, Los Angeles, CA 90095-1547, USA 2Astronomy Department, University of California, Berkeley, CA 94720, USA 3SYRTE, Observatoire de Paris, Universit´ePSL, CNRS, Sorbonne Universit´e,LNE, 61 avenue de l’Observatoire 75014 Paris 4Astrophysics, California Institute of Technology, MC 249-17, Pasadena, CA 91125, USA 5Institute for Astronomy, University of Hawaii, Honolulu, HI 96822, USA (Received; Revised; Accepted) Submitted to ApJ ABSTRACT Precision measurements of the stars in short-period orbits around the supermassive black hole at the Galactic Center are now being used to constrain general relativistic effects, such as the gravitational redshift and periapse precession. One of the largest systematic uncertainties in the measured orbits has been errors in the astrometric reference frame, which is derived from seven infrared-bright stars associated with SiO masers that have extremely accurate radio positions, measured in the Sgr A*-rest frame. We have improved the astrometric reference frame within 1400 of the Galactic Center by a factor of 2.5 in position and a factor of 5 in proper motion. In the new reference frame, Sgr A* is localized to within a position of 0.645 mas and proper motion of 0.03 mas yr−1. -
Product Support Bulletin
Product Support Bulletin Subject: Apex Plus Hardware and Software Compatibility Lists Date: 4/19/89 PSB No: S-007 Page: 1 of 8 Originator: REM The purpose of this bulletin is to provide a current listing of tested hardware and software for the Apex Plus. All testing was performed by Seiko Epson Japan and the results were supplied to Epson America. This is not an all - inclusive list; there are many hardware options and applications that will work correctly that are not listed. Unless otherwise noted, all tests were conducted with the latest release of the Apex Plus MS - DOS operating system software and ROM BIOS. The products tested were certified in one of three ways: OK - Product works with full functionality NG - Product does not work - see compatibility note * Product works with partial functionality - see compatibility note The information provided does not constitute a guarantee or endorsement of any particular product or any specific use or application. Some of the products on the list may have software or hardware requirements which are not met by the Apex Plus personal computer. Therefore, while EPSON believes the information supplied is accurate, EPSON does not assume any responsibility for use of any of the products on the attached list. EPSON MAKES NO REPRESENTATIONS OR WARRANTIES, EITHER EXPRESS OR’ IMPLIED, WITH RESPECT TO THIS LISTING OR THE PRODUCTS REFERENCED IN THE LIST. EPSON SHALL NOT BE LIABLE FOR ANY LOSS, INCONVENIENCE OR DAMAGE, INCLUDING DIRECT, SPECIAL, INCIDENTAL OR CONSEQUENTIAL DAMAGES, RESULTING FROM THE USE OR INABILITY TO USE ANY OF THE PRODUCTS LISTED. -
Variable Star Section Circular
British Astronomical Association VARIABLE STAR SECTION CIRCULAR No 90, December 1996 Contents A Selection of Light Curves ............................................................................. 1 General News ................................................................................................... 2 Recurrent Objects Programme News ............................................................... 3 Chart News ....................................................................................................... 4 Binocular Priority Stars in 1995 ...................................................................... 5 Asteroid-Variable Appulses: a short list to 2000 ........................................... 10 Comments on the VSS Observers Questionnaire .......................................... 12 VSS Meeting: part 1....................................................................................... 14 Photoelectric Minima of Eclipsing Binaries 1995 ......................................... 16 Recent Papers on Variable Stars .................................................................... 17 IBVS............................................................................................................... 18 Eclipsing Binary Predictions .......................................................................... 19 New Chart for CH Cyg................................................................................... 22 ISSN 0267-9272 Office: Burlington House, Piccadilly, London, W1V 9AG A SELECTION OF LIGHT CURVES -
The Nuclear Star Cluster of the Milky Way: Proper Motions and Mass R
Rochester Institute of Technology RIT Scholar Works Articles 3-5-2009 The ucleN ar Star Cluster of the Milky Way: Proper Motions and Mass Rainer Schödel Instituto de Astrofísica de Andalucía David Merritt Rochester Institute of Technology Andreas Eckart Universität zu Köln Follow this and additional works at: http://scholarworks.rit.edu/article Recommended Citation The uclen ar star cluster of the Milky Way: proper motions and mass R. Schödel, D. Merritt nda A. Eckart A&A, 502 1 (2009) 91-111 DOI: https://doi.org/10.1051/0004-6361/200810922 This Article is brought to you for free and open access by RIT Scholar Works. It has been accepted for inclusion in Articles by an authorized administrator of RIT Scholar Works. For more information, please contact [email protected]. Astronomy & Astrophysics manuscript no. proper c ESO 2009 February 23, 2009 The nuclear star cluster of the Milky Way: Proper motions and mass R. Schodel¨ 1, D. Merritt2, and A. Eckart3 1 Instituto de Astrof´ısica de Andaluc´ıa (IAA) - CSIC, Camino Bajo de Huetor´ 50, E-18008 Granada, Spain e-mail: [email protected] 2 Department of Physics and Center for Computational Relativity and Gravitation, Rochester Institute of Technology, Rochester, NY 14623, USA e-mail: [email protected] 3 I.Physikalisches Institut, Universitat¨ zu Koln,¨ Zulpicher¨ Str.77, 50937 Koln,¨ Germany e-mail: [email protected] ABSTRACT Context. Nuclear star clusters (NSCs) are located at the photometric and dynamical centers of the majority of galaxies. They are among the densest star clusters in the Universe. The NSC in the Milky Way is the only object of this class that can be resolved into individual stars. -
Stephen M. Cabrinety Collection in the History of Microcomputing, Ca
http://oac.cdlib.org/findaid/ark:/13030/kt529018f2 No online items Guide to the Stephen M. Cabrinety Collection in the History of Microcomputing, ca. 1975-1995 Processed by Stephan Potchatek; machine-readable finding aid created by Steven Mandeville-Gamble Department of Special Collections Green Library Stanford University Libraries Stanford, CA 94305-6004 Phone: (650) 725-1022 Email: [email protected] URL: http://library.stanford.edu/spc © 2001 The Board of Trustees of Stanford University. All rights reserved. Special Collections M0997 1 Guide to the Stephen M. Cabrinety Collection in the History of Microcomputing, ca. 1975-1995 Collection number: M0997 Department of Special Collections and University Archives Stanford University Libraries Stanford, California Contact Information Department of Special Collections Green Library Stanford University Libraries Stanford, CA 94305-6004 Phone: (650) 725-1022 Email: [email protected] URL: http://library.stanford.edu/spc Processed by: Stephan Potchatek Date Completed: 2000 Encoded by: Steven Mandeville-Gamble © 2001 The Board of Trustees of Stanford University. All rights reserved. Descriptive Summary Title: Stephen M. Cabrinety Collection in the History of Microcomputing, Date (inclusive): ca. 1975-1995 Collection number: Special Collections M0997 Creator: Cabrinety, Stephen M. Extent: 815.5 linear ft. Repository: Stanford University. Libraries. Dept. of Special Collections and University Archives. Language: English. Access Access restricted; this collection is stored off-site in commercial storage from which material is not routinely paged. Access to the collection will remain restricted until such time as the collection can be moved to Stanford-owned facilities. Any exemption from this rule requires the written permission of the Head of Special Collections. -
Radial Velocities of K–M Dwarfs and Local Stellar Kinematics?
A&A 596, A116 (2016) Astronomy DOI: 10.1051/0004-6361/201527850 & c ESO 2016 Astrophysics Radial velocities of K–M dwarfs and local stellar kinematics? J. Sperauskas1, S. Bartašiut¯ e˙1, R. P. Boyle2, V. Deveikis1, S. Raudeliunas¯ 1, and A. R. Upgren3 1 Vilnius University Observatory, Ciurlionioˇ 29, 03100 Vilnius, Lithuania e-mail: [email protected] 2 Vatican Observatory Research Group, Steward Observatory, University of Arizona, Tucson, Arizona 85721, USA 3 Wesleyan and Yale Universities, Middletown and New Haven, Connecticut 06457, USA Received 27 November 2015 / Accepted 18 July 2016 ABSTRACT Aims. The goal of this paper is to present complete radial-velocity data for the spectroscopically selected McCormick sample of nearby K–M dwarfs and, based on these and supplementary data, to determine the space-velocity distributions of late-type stars in the solar neighborhood. Methods. We analyzed nearly 3300 measurements of radial velocities for 1049 K–M dwarfs, that we obtained during the past decade with a CORAVEL-type instrument, with a primary emphasis on detecting and eliminating from kinematic calculations the spec- troscopic binaries and binary candidates. Combining radial-velocity data with Hipparcos/Tycho-2 astrometry we calculated the space-velocity components and parameters of the galactic orbits in a three-component model potential for the stars in the sample, that we use for kinematical analysis and for the identification of possible candidate members of nearby stellar kinematic groups. Results. We present the catalog of our observations of radial velocities for 959 stars which are not suspected of velocity variability, along with the catalog of U; V; W velocities and Galactic orbital parameters for a total of 1088 K–M stars which are used in the present kinematic analysis. -
Information Technology Breeds New Age Terrorism
Rochester Institute of Technology RIT Scholar Works Theses 2002 Information technology breeds new age terrorism Amita Aziz Follow this and additional works at: https://scholarworks.rit.edu/theses Recommended Citation Aziz, Amita, "Information technology breeds new age terrorism" (2002). Thesis. Rochester Institute of Technology. Accessed from This Thesis is brought to you for free and open access by RIT Scholar Works. It has been accepted for inclusion in Theses by an authorized administrator of RIT Scholar Works. For more information, please contact [email protected]. Information Technology Breeds New age Terrorism By Amita Aziz Thesis submitted in partial fulfillment of the requirements for the degree of Master of Science in Information Technology Rochester Institute of Technology B. Thomas Golisano College of Computing and Information Sciences September 2002 Thesis Reproduction Permission Form Rochester Institute of Technology B. Thomas Golisano College Of Computing and Information Sciences Master of Science in Information Technology Information Technology Breeds New Age Terrorism I, Amita Aziz, hereby grant permission to the Wallace Library of the Rochester Institute of Technology to reproduce my thesis in whole or in part. Any reproduction must not be for commercial use or profit. Date: g-(301°.1 Signature of Author: _ Rochester Institute of Technology B. Thomas Golisano College of Computing and Information Sciences Master of Science in Information Technology Thesis Approval Form Student Name: Amita Aziz Project Title: Information Technology Breeds New Age Terrorism Thesis Committee Name Signature Date Prof. Rayno Niemi Chair 0 Erof.~:;':":"':''''':'::':~--=:..;;;;l,"",,-=,,-=------------Rudy Pugliese '('''':'{_~l ,l20 2..-- Committee Member ··Prof. Alec Berenbaum ~ .:.....:....:~...::==-=~~=.:::.:~-------------.....,i'----j.'-'1;:16;2?V . -
THE 100 Myr STAR FORMATION HISTORY of NGC 5471 from CLUSTER and RESOLVED STELLAR PHOTOMETRY
The Astronomical Journal, 141:126 (16pp), 2011 April doi:10.1088/0004-6256/141/4/126 C 2011. The American Astronomical Society. All rights reserved. Printed in the U.S.A. THE 100 Myr STAR FORMATION HISTORY OF NGC 5471 FROM CLUSTER AND RESOLVED STELLAR PHOTOMETRY Ruben´ Garc´ıa-Benito1,2, Enrique Perez´ 3, Angeles´ I. D´ıaz2,Jesus´ Ma´ız Apellaniz´ 3,4, and Miguel Cervino˜ 3 1 Kavli Institute of Astronomy and Astrophysics, Peking University, 100871 Beijing, China; [email protected] 2 Departamento de F´ısica Teorica´ (C-XI), Facultad de Ciencias, Universidad Autonoma´ de Madrid, Ctra. Colmenar Viejo km 15.600, E-28049 Madrid, Spain; [email protected] 3 Instituto de Astrof´ısica de Andaluc´ıa, CSIC, Aptdo. Correos 3004, E-18080 Granada, Spain; [email protected], jmaiz@iaa, [email protected] Received 2010 August 23; accepted 2011 February 1; published 2011 March 8 ABSTRACT We show that star formation in the giant H ii region NGC 5471 has been ongoing during the past 100 Myr. Using Hubble Space Telescope/Wide-Field Planetary Camera 2 F547M and F675W, ground-based JHKs , and GALEX FUV and NUV images, we have conducted a photometric study of the star formation history (SFH) in the massive giant extragalactic H ii region NGC 5471 in M101. We perform a photometric study of the color–magnitude diagram (CMD) of the resolved stars and an integrated analysis of the main individual star-forming clusters and of NGC 5471 as a whole. The integrated UV–optical–NIR photometry for the whole region provides two different reference ages, 8 Myr and 60 Myr, revealing a complex SFH, clearly confirmed by the CMD-resolved stellar photometry analysis. -
Gaia Proper Motions and Orbits of the Ultra-Faint Milky Way Satellites
The Astrophysical Journal, 863:89 (15pp), 2018 August 10 https://doi.org/10.3847/1538-4357/aacdfb © 2018. The American Astronomical Society. All rights reserved. Gaia Proper Motions and Orbits of the Ultra-faint Milky Way Satellites Joshua D. Simon Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USA; [email protected] Received 2018 April 30; accepted 2018 May 31; published 2018 August 13 Abstract The second data release from the Gaia mission (DR2) provides a comprehensive and unprecedented picture of the motions of astronomical sources in the plane of the sky, extending from the solar neighborhood to the outer reaches of the Milky Way. I present proper-motion measurements based on Gaia DR2 for 17 ultra-faint dwarf galaxies within 100kpc of the Milky Way. I compile the spectroscopically confirmed member stars in each dwarf bright enough for Gaia astrometry from the literature, producing member samples ranging from two stars in TriangulumII to 68 stars in BoötesI. From the spectroscopic member catalogs, I estimate the proper motion of each system. I find good agreement with the proper motions derived by the Gaia collaboration for BoötesI and LeoI. The tangential velocities for 14 of the 17 dwarfs are determined to better than 50kms−1, more than doubling the sample of such measurements for Milky Way satellite galaxies. The orbital pericenters are well constrained, with a mean value of 38kpc. Only one satellite, TucanaIII, is on an orbit passing within 15kpc of the Galactic center, suggesting that the remaining ultra-faint dwarfs are unlikely to have experienced severe tidal stripping. -
Dust Around Main-Sequence and Supergiant Stars
Dust around Main-Sequence and Supergiant Stars A Thesis submitted for the Degree of Doctor of Philosophy of the University of London by Roger James Sylvester UCL Department of Physics & Astronomy University College London University of London 1995 ProQuest Number: 10044337 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 10044337 Published by ProQuest LLC(2016). 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 A bstract This thesis is a study of the properties of the dust around two rather different types of star. The first part is concerned with the mid-infrared emission from a sample of 16 M-type supergiants. As weU as silicate emission features, seven of the stars showed the UIR (unidentified infrared) emission bands, associated with carbonaceous material. According to standard theory, aU the carbon in the outflows from these oxygen-rich stars should be bound up in CO molecules, preventing the formation of carbonaceous dust. The results were interpreted in terms of a non-equilibrium chemical model, which invoked chromospheric UV photons to dissociate CO, allowing carbonaceous material to form, and to excite the observed UIR-band emission. -
A Surprise in the Updated List of Stellar Perturbers of Long Period Comets
Astronomy & Astrophysics manuscript no. main c ESO 2020 April 28, 2020 A surprise in the updated list of stellar perturbers of long period comets motion. Rita Wysoczanska´ ⋆ and Piotr A. Dybczynski´ ⋆⋆ and Magdalena Polinska´ ⋆⋆⋆ Astronomical Observatory Institute, Faculty of Physics, A. Mickiewicz University, Słoneczna 36, Poznan,´ Poland April 28, 2020 ABSTRACT Context. The second Gaia data release (Gaia DR2) provided us with the precise five-parameter astrometry for 1.3 billion of sources. As stars passing close to the Solar System are thought to be responsible for influencing the dynamical history of long period comets, we update and extend the list of stars that could potentially perturb motion of these comets. Aims. We aim to announce a publicly available database containing an up to date list of stars and stellar systems potentially perturbing long period comets motion. We add new objects and revise previously published lists. Special emphasis was placed on stellar systems. Discussion on masses estimation is included. Methods. Using the astrometry, preferably from Gaia DR2, augmented with data from other sources, we calculate spatial positions and velocities for each star. To filter studied objects on the basis of their minimal heliocentric distances we numerically integrate motion of stars under the Galactic potential and their mutual interactions. Results. We announce the updated list of stellar perturbers of cometary motion, including masses of perturbers along with the publicly available database interface. These data are ready to be used with the observed long period comets orbits to study an individual influence of a whole sample of perturbers, or specific stars, on a dynamical past or future of a specific comet.