Object-Role Modeling Fundamentals
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CALCEPH - Fortran 77/90/95 Language Release 3.5.0
CALCEPH - Fortran 77/90/95 language Release 3.5.0 M. Gastineau, J. Laskar, A. Fienga, H. Manche Aug 19, 2021 CONTENTS 1 Introduction 3 2 Installation 5 2.1 Unix-like system (Linux, Mac OS X, BSD, Cygwin, ...)........................5 2.1.1 Quick instructions........................................5 2.1.2 Detailed instructions......................................5 2.2 Windows system.............................................7 2.2.1 Using the Microsoft Visual C++ compiler...........................7 2.2.2 Using the MinGW.......................................9 3 Library interface 11 3.1 A simple example program........................................ 11 3.2 Headers and Libraries.......................................... 11 3.2.1 Compilation on a Unix-like system............................... 12 3.2.2 Compilation on a Windows system............................... 12 3.3 Types................................................... 12 3.4 Constants................................................. 12 4 Multiple file access functions 15 4.1 Thread notes............................................... 15 4.2 Usage................................................... 15 4.3 Functions................................................. 15 4.3.1 calceph_open.......................................... 15 4.3.2 f90calceph_open_array..................................... 16 4.3.3 f90calceph_prefetch....................................... 17 4.3.4 f90calceph_isthreadsafe..................................... 17 4.3.5 f90calceph_compute..................................... -
CALCEPH - Octave/Matlab Language Release 3.5.0
CALCEPH - Octave/Matlab language Release 3.5.0 M. Gastineau, J. Laskar, A. Fienga, H. Manche Aug 19, 2021 CONTENTS 1 Introduction 3 2 Installation 5 2.1 Unix-like system (Linux, Mac OS X, BSD, Cygwin, ...)........................5 2.2 Windows system.............................................6 2.2.1 Using the Microsoft Visual C++ compiler...........................6 2.2.2 Using the MinGW.......................................7 3 Library interface 9 3.1 A simple example program........................................9 3.2 Package..................................................9 3.3 Types................................................... 10 3.4 Constants................................................. 10 4 Multiple file access functions 13 4.1 Thread notes............................................... 13 4.2 Usage................................................... 13 4.3 Functions................................................. 13 4.3.1 CalcephBin.open........................................ 13 4.3.2 CalcephBin.open........................................ 14 4.3.3 CalcephBin.prefetch...................................... 15 4.3.4 CalcephBin.isthreadsafe.................................... 15 4.3.5 CalcephBin.compute...................................... 15 4.3.6 CalcephBin.compute_unit................................... 17 4.3.7 CalcephBin.orient_unit..................................... 18 4.3.8 CalcephBin.rotangmom_unit.................................. 20 4.3.9 CalcephBin.compute_order................................... 21 4.3.10 -
Overview of the Esa Jovian Technology Reference Studies
DOCUMENT OVERVIEW OF THE ESA JOVIAN TECHNOLOGY REFERENCE STUDIES prepared by/préparé par Alessandro Atzei, Arno Wielders, Anamarija Stankov, Peter Falkner reference/réference SCI-AP/2004/TN-085/AA issue/édition 3 revision/révision 0 date of issue/date d’édition 30/03/07 status/état Final Document type/type de document Technical Note SCI-AP a ESTEC Jovian Studies Overview Keplerlaan 1 - 2201 AZ Noordwijk - The Netherlands April_2_04_07 .doc Tel. (31) 71 5656565 - Fax (31) 71 5656040 Overview of the ESA Jovian Technology Reference Studies issue 3 revision 0 - 30/03/07 page 2 of 148 APPROVAL Title Overview of the ESA Jovian Technology Reference Studies issue 3 revision 0 titre issue revision author Alessandro Atzei, Arno Wielders, Anamarija Stankov, Peter date 30/03/07 auteur Falkner date approved by date approuvé by date Overview of the ESA Jovian Technology Reference Studies issue 3 revision 0 - 30/03/07 page 3 of 148 T ABLE O F C ONTENTS INTRODUCTION .....................................................................................................................................................7 Technology reference Studies....................................................................................................................7 Purpose of this document...........................................................................................................................7 STUDYING THE JOVIAN SYSTEM ..........................................................................................................................9 -
Scales of the Solar System
Basic Solar System Data The Sun Diameter (103 km) 1400 The Planets (etc.) Distance from Sun (106km) Orbital Period (yrs) Mercury 4.8 58 .24 Venus 13 108 .61 Earth 13 149 1.0 Mars 7 228 1.9 Jupiter 144 778 11.9 Saturn 121 1430 29.5 Uranus 53 2870 84 Neptune 50 4500 165 Pluto 3.0 5900 249 Nearest Star 40 million (4+ light years) Farthest edge of Milky Way 1 million million (100,000 light years) Nearest galaxy 20 million million (2 million light years) Farthest observable objects 50,000 million million (5 billion light years) Major Asteroids Ceres 1.0 (The asteroids generally Pallas .6 occupy orbits between Vesta .5 Mars and Jupiter) Major Moons Distance from Planet (103km) Orbital Period (days) of the Earth The Moon 3.5 385 27 of Mars Phobos .028 9 .3 Deimos .016 24 1.3 of Jupiter Io 3.6 422 1.8 Europa 3.1 671 3.6 Ganymede 5.3 1070 7.2 Callisto 5.0 1880 17 Sinope (farthest) .014 23700 758 of Saturn Tethys 1.0 295 1.9 Dione .8 377 2.7 Rhea 1.5 527 4.5 Titan 5.8 1220 16 Iapetus 1.5 3560 79 Phoebe (farthest) .2 13000 550 of Uranus Miranda .4 130 1.4 Ariel 1.4 191 2.5 Umbriel 1.0 260 4.1 Titania 1.8 436 8.7 Oberon 1.6 583 13 of Neptune Triton 3.8 354 5.9 Nereid .6 5570 360 Relative Scales (with the solar diameter = “1”) The Planets (etc.) Diameter Distance from Sun Mercury .003 41 Venus .009 77 Earth .009 106 Mars .005 163 Jupiter .10 556 Saturn .09 1020 Uranus .04 2050 Neptune .04 3200 Pluto .002 4200 Nearest star 30 million Farthest edge of Milky Way .7 million million Nearest galaxy 14 million million Farthest observable objects 40,000 million -
CALCEPH - Python Language Release 3.5.0
CALCEPH - Python language Release 3.5.0 M. Gastineau, J. Laskar, A. Fienga, H. Manche Aug 19, 2021 CONTENTS 1 Introduction 3 2 Installation 5 2.1 Instructions................................................5 3 Library interface 7 3.1 A simple example program........................................7 3.2 Modules.................................................7 3.3 Types...................................................8 3.4 Constants.................................................8 4 Multiple file access functions 11 4.1 Thread notes............................................... 11 4.2 Usage................................................... 11 4.3 Functions................................................. 11 4.3.1 calcephpy.CalcephBin.open................................... 11 4.3.2 calcephpy.CalcephBin.open................................... 12 4.3.3 calcephpy.CalcephBin.prefetch................................. 13 4.3.4 calcephpy.CalcephBin.isthreadsafe............................... 13 4.3.5 calcephpy.CalcephBin.compute................................. 13 4.3.6 calcephpy.CalcephBin.compute_unit.............................. 15 4.3.7 calcephpy.CalcephBin.orient_unit............................... 17 4.3.8 calcephpy.CalcephBin.rotangmom_unit............................ 18 4.3.9 calcephpy.CalcephBin.compute_order............................. 19 4.3.10 calcephpy.CalcephBin.orient_order............................... 21 4.3.11 calcephpy.CalcephBin.rotangmom_order............................ 23 4.3.12 calcephpy.CalcephBin.getconstant.............................. -
Moons of the Solar System
MOONS OF OUR SOLAR SYSTEM last updated October 7, 2019 Since there are over 200 known moons in our solar system, all have been given names or designations. The problem of naming is compounded when space pictures are analyzed and new moons are discovered (or on rare occasions when spacecraft images of small, distant moons are found to be imaging flaws, and a moon is removed from the list). This is a list of the planets' known moons, with their names or other designations. If a planet has more than one moon, they are listed from the moon closest to the planet to the moon farthest from the planet. Since the naming systems overlap, many moons have more than one designation; in each case, the first identification listed is the official one. MERCURY and VENUS have no known moons. EARTH has one known moon. It has no official name. MARS has two known moons: Phobos and Deimos. ASTEROIDS (Small moons have now been found around several asteroids. In addition, a growing number of asteroids are now known to be binary, meaning two asteroids of about the same size orbiting each other. Whether there is a fundamental difference in these situations is uncertain.) JUPITER has 79 known moons. Names such as “S/2003 J2" are provisional. Metis (XVI), Adrastea (XV), Amalthea (V), Thebe (XIV), Io (I), Europa (II), Ganymede (III), Callisto (IV), Themisto (XVIII), Leda (XIII), Himalia (Hestia or VI), S/2018 J1, S/2017 J4, Lysithea (Demeter or X), Elara (Hera or VII), Dia (S/2000 J11), Carpo (XLVI), S/2003 J12, Valetudo (S/2016 J2), Euporie (XXXIV), S/2003 J3, S/2011 -
A Capture Model for Irregular Moons Based on a Restricted 2+2 Body Problem and Its Statistical Analysis
TESIS DOCTORAL Título A capture model for irregular moons based on a restricted 2+2 body problem and its statistical analysis Autor/es Wafaa Kanaan Director/es Víctor Lanchares Barrasa Facultad Facultad de Ciencia y Tecnología Titulación Departamento Matemáticas y Computación Curso Académico A capture model for irregular moons based on a restricted 2+2 body problem and its statistical analysis, tesis doctoral de Wafaa Kanaan, dirigida por Víctor Lanchares Barrasa (publicada por la Universidad de La Rioja), se difunde bajo una Licencia Creative Commons Reconocimiento-NoComercial-SinObraDerivada 3.0 Unported. Permisos que vayan más allá de lo cubierto por esta licencia pueden solicitarse a los titulares del copyright. © El autor © Universidad de La Rioja, Servicio de Publicaciones, 2017 publicaciones.unirioja.es E-mail: [email protected] FACULTY OF SCIENCE AND TECHNOLOGY DEPARTMENT OF MATHEMATICS AND COMPUTATION PHD THESIS: A CAPTURE MODEL FOR IRREGULAR MOONS BASED ON A RESTRICTED 2+2 BODY PROBLEM AND ITS STATISTICAL ANALYSIS A Thesis submitted by Wafaa Kanaan for the degree of Doctor of Philosophy in the University of La Rioja Supervised by: Víctor Lanchares To the soul of my brother Aeman. Who has always been my hero and now is the brightest star in my sky, showing me the right path to follow. iv Acknowledgements I would like to express my gratitude to everybody that, in one way or another, has contributed with valuable help and comments that finally ended in this report. First of all, I would like to thank my advisor, Victor Lanchares, for guiding and supporting me. From him I learned many things and with him I shared very hard times during these years of thesis. -
CLARK PLANETARIUM SOLAR SYSTEM FACT SHEET Data Provided by NASA/JPL and Other Official Sources
CLARK PLANETARIUM SOLAR SYSTEM FACT SHEET Data provided by NASA/JPL and other official sources. This handout ©Jan 2020 by Clark Planetarium (www.clarkplanetarium.org). May be freely copied by professional educators for classroom use only. The known satellites of the Solar System shown here next to their planets with their sizes (mean diameter in km) in parenthesis. The planets and satellites (with diameters above 950 km) are depicted in relative size (with Earth = 0.500 inches). Moons are listed in order of increasing average distance from planet (closest first). Distances from planet to moon are not listed. Mercury Jupiter Saturn Uranus Neptune Pluto • 1- Metis (44) • 26- S/2017 J 3 (2) • 54- S/2017 J 5 (2) • 1- S/2009 S1 (0.6) • 33- Erriapo (10) • 1- Cordelia (40.2) (Dwarf Planet) (no natural satellites) • 2- Adrastea (16) • 27- Orthosie (2) • 55- S/2017 J 8 (1) • 2- Pan (26) • 34- Siarnaq (40) • 2- Ophelia (42.8) • Charon (1212) • 3- Bianca (51.4) Venus • 3- Amalthea (168) • 28- Euanthe (3) • 56- S/2003 J 4 (2) • 3- Daphnis (7) • 35- Skoll (6) • Nix (50) • 4- Thebe (98) • 29- Thyone (4) • 57- Erinome (3.2) • 4- Atlas (32) • 36- Tarvos (15) • 4- Cressida (79.6) • Hydra (65) • 5- Desdemona (64) • 30- S/2003 J 16 (2) • 58- S/2017 J 2 (2) • 5- Prometheus (100.2) • 37- Tarqeq (7) • Kerberos (19.5) • 5- Io (3,643.2) • 6- Pandora (83.8) • 38- Greip (6) • 6- Juliet (93.6) • 1- Naiad (58) • 31- Mneme (2) • 59- S/2010 J 1 (2) • Styx (19) • 7- Epimetheus (119) • 39- Hyrrokkin (8) • 7- Portia (135.2) • 2- Thalassa (80) • 6- Europa (3,121.6) • -
Cladistical Analysis of the Jovian and Saturnian Satellite Systems
Draft version October 2, 2018 Typeset using LATEX modern style in AASTeX61 CLADISTICAL ANALYSIS OF THE JOVIAN AND SATURNIAN SATELLITE SYSTEMS Timothy. R. Holt,1, 2 Adrian. J. Brown,3 David Nesvorny,´ 4 Jonathan Horner,1 and Brad Carter1 1University of Southern Queensland, Computational Engineering and Science Research Centre, Queensland, Australia 2Swinburne University of Technology, Center for Astrophysics and Supercomputing, Victoria, Australia. 3Plancius Research LLC, Severna Park, MD. USA. 4Southwest Research Institute, Department of Space Studies, Boulder, CO. USA. (Received June 8th, 2017; Revised April 9th, 2018; Accepted April 10th, 2018; Published MM DD, 2018) Submitted to The Astrophysical Journal ABSTRACT Jupiter and Saturn each have complex systems of satellites and rings. These satel- lites can be classified into dynamical groups, implying similar formation scenarios. Re- cently, a larger number of additional irregular satellites have been discovered around both gas giants that have yet to be classified. The aim of this paper is to examine the relationships between the satellites and rings of the gas giants, using an analytical technique called cladistics. Cladistics is traditionally used to examine relationships between living organisms, the `tree of life'. In this work, we perform the first cladis- tical study of objects in a planetary science context. Our method uses the orbital, physical and compositional characteristics of satellites to classify the objects in the Jovian and Saturnian systems. We find that the major relationships between the arXiv:1706.01423v2 [astro-ph.EP] 30 Apr 2018 satellites in the two systems, such as families, as presented in previous studies, are broadly preserved. In addition, based on our analysis of the Jovian system, we iden- tify a new retrograde irregular family, the Iocaste family, and suggest that the Phoebe family of the Saturnian system can be further divided into two subfamilies. -
Phase II Proposal Instructions 25.0
Phase II Proposal Instructions 25.0 HST Cycle 25 Phase II Proposal Instructions Operations and Data Management Division 3700 San Martin Drive Baltimore, Maryland 21218 [email protected] Operated by the Association of Universities for Research in Astronomy, Inc., for the National Aeronautics and Space Administration Revision History Release Version Type Editors Date Cycle 25 GO June 2017 HST Instrument Team Members and S. Rose See Significant Changes Since the Previous Cycle Cycle 24 GO June 2016 HST Instrument Team Members and S. Rose Cycle 23 GO June 2015 HST Instrument Team Members and S. Rose Cycle 22 GO June 2014 J. Younger and S. Rose 21.0 GO May 2013 J. Younger and S. Rose 20.0 GO June 2012 J. Younger and S. Rose This version is issued in coordination with the APT release and should be fully compliant with Cycle 25.2 APT. This is the General Observer version. If you would like some hints on how to read and use this document, see: Some Pointers in PDF and APT JavaHelp How to get help 1. Visit STScI’s Web site: http://www.stsci.edu/hst where you will find resources for observing with HST and working with HST data. 2. Contact your Program Coordinator (PC) or Contact Scientist (CS) you have been assigned. These individuals were identified in the notification letter from STScI. 3. Send e-mail to [email protected], or call 1-800-544-8125. From outside the United States, call 1-410-338-1082. Table of Contents HST Cycle 25 Phase II Proposal Instructions Part I: Phase II Proposal Writing ................................ -
Jupiter's Outer Satellites and Trojans
12 Jupiter's Outer Satellites and Trojans David C. J ewitt Institute for Astronomy, University of Hawaii Scott Sheppard Institute for Astronomy, University of Hawaii Carolyn Porco Southwest Research Institute 12.1 INTRODUCTION Jupiter's irregular satellites possess large, eccentric and highly inclined orbits. They are conventionally considered separately from the temporarily captured satellites and the Trojans (the latter co-orbiting the Sun, leading and trail ing Jupiter by 60°). However, there is reason to believe that objects in these three groups share many similarities, both in terms of their physical properties and their origins. Ac cordingly, in this review we jointly discuss the irregular and temporary satellites and the Trojans. In the modern view of the solar system, different pop ulations of small bodies can be traced back to their ori gin in the protoplanetary disk of the Sun. Most planetesi mals that formed near the orbits of the giant planets were promptly ejected from the planetary region. A small frac Figure 12.1. Interrelations among the populations considered tion of those ejected (perhaps 10%) remain bound to the in this chapter. Solid arrows denote established dynamical path ways. At the present epoch, in which sources of energy dissipa Sun in the rv105 AU scale Oort Cloud which provides a tion are essentially absent, no known pathways (dashed lines) continuing source of the long-period comets. Planetesimals exist between the temporary and permanent satellite and Trojan growing beyond Neptune were relatively undisturbed and populations. Numbers in parentheses indicate the approximate their descendants survive today in the Kuiper Belt. The dynamical lifetimes of the different populations. -
Fractal Properties of the Gas Giants and Their Satellites Within the Solar System
To Physics Journal Vol 2 (2019) ISSN: 2581-7396 http://www.purkh.com/index.php/tophy Fractal properties of the Gas giants and their satellites within the Solar system Rosen Iliev1, Boyko Ranguelov2 1Institute for Space Research and Technology, Bulgarian Academy of Sciences, Sofia, Bulgaria 2Department of Applied Geophysics, University of Mining and Geology “St. Ivan Rilski”, Sofia, Bulgaria Email addresses: [email protected], [email protected] Abstract This study reveals the fractal structure of gas giants and their moons. For this purpose, fractal analysis of Jupiter, Saturn, Uranus, Neptune and 182 moons was performed based on their radius (size). The results obtained reveal the fractal geometry of the planet / moon systems within the outer Solar system (SS). The resulting fractal dimensions (D) range from -0.57 to -1.43, decreasing with distance from the Sun. This requires a thorough analysis. Keywords: Solar system, Jupiter, Saturn, Uranus, Neptune, moons, fractal Introduction The theory of fractals has been largely developed in the last few decades. The results obtained are frequently used for explanation of the self-similarity and the self-organization of different elements related to the Earth and Planetary science. Thanks to the high achievements of scientific and technical thought in the last half century, mankind has been able to explore the space that has not been available until then. In the course of various space missions, massive data on the geology, topography and physics of the celestial bodies in the solar system has been gathered through space probes and powerful telescopes and satellites. There was a need to develop methods and approaches to analyze and interpret new data.