National Aeronautics and Space Administration Thaolar M S M Thaolar I

Total Page:16

File Type:pdf, Size:1020Kb

National Aeronautics and Space Administration Thaolar M S M Thaolar I National Aeronautics and Space Administration S M olar a th i This collection of activities is based on a weekly series of space science problems distributed to thousands of teachers during the 2005- 2012 school years. They were intended for students looking for additional challenges in the math and physical science curriculum in grades 5 through 12. The problems were created to be authentic glimpses of modern science and engineering issues, often involving actual research data. The problems were designed to be ‘one-pagers’ with a Teacher’s Guide and Answer Key as a second page. This compact form was deemed very popular by participating teachers. This book is an expanded edition of the previous Hinode math solar problem book, with many new problems added to the original collection that were created by SpaceMath@NASA since 2009 For more weekly classroom activities about astronomy and space visit the NASA website, http://spacemath.gsfc.nasa.gov Add your email address to our mailing list by contacting Dr. Sten Odenwald at [email protected] Front and back cover credits: Front) Main image: SDO Solar Image of Transit of Venus, June 6, 2012; Small images, top left to right - SOHO/EIT Helium 304A image; Optical image KPNO; 20cm Radio Image, NRAO/VLA Back) Hinode soft x-ray imagery (Hinode/JAXA/NRL) This booklet was created through an education grant NNH06ZDA001N- EPO from NASA's Science Mission Directorate. Space Math http://spacemath.gsfc.nasa.gov Table of Contents ii Grade Page Acknowledgments i Table of Contents ii Mathematics Topic Matrix v How to use this Book ix Alignment with Standards x Teacher Comments xi The Relative Sizes of the Sun and Stars 3-5 1 Monster Sunspots 3-5 2 Solar Surface Details with the Swedish Vacuum Telescope 3-5 3 Close-up of a Sunspot by Hinode 3-5 4 An Extreme Ultraviolet Image of the Sun 3-5 5 Radio Image of the Sun 3-5 6 A Gamma-Ray Image of the Sun 3-5 7 X-Ray Image of the Sun 3-5 8 Hinode Sees Mysterious Solar Micro-flares 3-5 9 X-Ray Image of the Sun 3-5 10 Solar Storm Timeline - Narrative 3-5 11 Solar Storm Timeline - Tabular 3-5 12 Solar flares 3-5 13 Sunspots and Solar Flares 3-5 14 Solar Flares and the Sunspot Cycle 3-5 15 How Common are X-Class Solar Flares? 3-5 16 SPEs and the Sunspot Cycle 3-5 17 Solar Dynamics Observatory: Giga,Tera, Peta and Exabytes 3-5 18 Hinode Satellite Power 3-5 19 Sunspot Size and the Sunspot Cycle 3-5 20 Sunspot Cycles Since 1900 3-5 21 Are you ready for Sunspot Cycle 24? 3-5 22 Solar Storms: Odds, Fractions and Percentages 3-5 23 Studying Solar Storms with Venn Diagrams 3-5 24 Space Weather Indicators 3-5 25 Sunspot cycles 3-5 26 Solar Irradiance Changes and the Sunspot Cycle 3-5 27 Sunspots and Satellite Re-entry 3-5 28 Satellite Failures and Outages During Cycle 23 3-5 29 Changing Perspectives on the Sun's Diameter 3-5 30 The Sun in Visible Light 3-5 31 SDO Reveals Details on the Surface of the Sun 3-5 32 Getting an Angle on the Sun and Moon 6-8 33 The Last Total Solar Eclipse…Ever! 6-8 34 STEREO Spacecraft give 360o Solar View 6-8 35 Space Math http://spacemath.gsfc.nasa.gov Table of Contents (contd) iii Grade Page General Angles and Radian Measure 6-8 36 The Magnetic Classification of Sunspots 6-8 37 Solar Irradiance Changes and the Sunspot Cycle 6-8 38 How fast does the sun spin? 6-8 39 The Speed of a Coronal Mass Ejection 6-8 40 Measuring the Speed of a Prominence with SDO 6-8 41 Estimating Magnetic Field Speeds on the Sun 6-8 42 Exploring the Solar Wind and Coronal Mass Ejections 6-8 43 STEREO Watches the Sun Kick Up a Storm! 6-8 44 Measuring the Speed of a Solar Tsunami! 6-8 45 Estimating Halo CME Speeds 6-8 46 An Interplanetary Shock Wave 6-8 47 Estimating Halo CME Arrival Times 6-8 48 Histogram of Halo CME Speeds: 1996-2008 6-8 49 Predicting the Direction of Motion of a CME 6-8 50 Fastest Halo CME Speeds by Year and Month 6-8 51 Solar Storms: Sequences and Probabilities I 6-8 52 Are you ready for Sunspot Cycle 24? 6-8 53 Solar Storm Energy and Pie Graphs 6-8 54 Probability of Compound Events 6-8 55 How often do solar storms occur? 6-8 56 Cosmic Rays and the Sunspot Cycle 6-8 57 Active Region Evolution and Energy Release 6-8 58 M-flares as Predictors of X-flares 6-8 59 Find the mystery lines...if you can! 6-8 60 Death Stars 9-12 61 Exploring the Nighttime Launch of STEREO 9-12 62 Do fast CMEs produce intense SPEs? 9-12 63 Seeing Solar Storms in STEREO - II 9-12 64 Seeing Solar Storms in STEREO 9-12 65 Right Triangle Trigonometry 9-12 66 Hinode Studies Loopy Sunspots! 9-12 67 The Most Important Equation in Astronomy! 9-12 68 The Sun in Hydrogen Light 9-12 69 Radio Image of the Sun - I 9-12 70 Radio Image of the Sun - II 9-12 71 Radio Image of the Sun - III 9-12 72 The Solar Spectrum from Gamma to Radio 9-12 73 The Energy of Light - I 9-12 74 The Energy of Light - II 9-12 75 Space Math http://spacemath.gsfc.nasa.gov Table of Contents (contd) iv Grade Page The Flow of Light Energy: Power 9-12 76 CME Kinetic Energy and Mass 9-12 77 Combinations and the Binomial Theorem 9-12 78 Combinations and the Binomial Theorem 9-12 79 Finding Binomial Probabilities using Combinations 9-12 80 Finding Trinomial Probabilities 9-12 81 Normal Distributions 9-12 82 Solar Probe Plus: Working with angular diameter 9-12 83 Solar Probe Plus- Having a hot time near the sun! 9-12 84 Finding Mass in the Cosmos 9-12 85 A Mathematical Model of the Sun 9-12 86 The Law of Sines 9-12 87 The Law of Cosines 9-12 88 Law of Cosines 9-12 89 Functions and their Graphs: Sunspot numbers 9-12 90 Matrix operations 9-12 91 Algebraic Expressions and Models 9-12 92 Polynomial Modeling with Technology 9-12 93 Graphing Simple Rational Functions 9-12 94 Hot Gas and Cold Gas 9-12 95 Using the Doppler Shift to Study Gas 9-12 96 Spectroscopy and Gas Density - Elementary 9-12 97 Density Structure of an Active Region 9-12 98 Plasma Speeds in Active Regions 9-12 99 Useful Links 100 Space Math http://spacemath.gsfc.nasa.gov Mathematics Topic Matrix v Topic Problem Numbers 1 2 3 4 5 6 7 8 9 1 1 1 1 1 1 1 1 1 1 2 2 2 2 2 2 2 2 2 2 3 3 0 1 2 3 4 5 6 7 8 9 0 1 2 3 4 5 6 7 8 9 0 1 Inquiry X X Technology, X X X X X X X X X X X rulers Numbers, patterns, X X X X X X X X X X X X percentages Averages X X X X X X X X Time, distance, speed Areas and X X X volumes Scale drawings X X X X X X X X X X X X Geometry X Scientific Notation Unit X Conversions Fractions X Graph or Table X X X X X X X X X X X X X X X X Analysis Solving for X Evaluating Fns Modeling Probability X X Rates/Slopes Logarithmic Fns Polynomials Power Fns Conics Piecewise Fns Trigonometry Integration Differentiation Limits Space Math http://spacemath.gsfc.nasa.gov Mathematics Topic Matrix (cont'd) vi Topic Problem Numbers 3 3 3 3 3 3 3 3 4 4 4 4 4 4 4 4 4 4 5 5 5 5 5 5 5 5 5 5 6 6 6 2 3 4 5 6 7 8 9 0 1 2 3 4 5 6 7 8 9 0 1 2 3 4 5 6 7 8 9 0 1 2 Inquiry X Technology, X X X X X X X X X X rulers Numbers, patterns, X X X X X X X X X X X percentages Averages X X X X X Time, distance, X X X X X X X X X X X X X speed Areas and X volumes Scale drawings X X X X X X X X X X Geometry X X X Scientific X X Notation Unit Conversions Fractions Graph or Table X X X X X X X X X X X X X X Analysis Solving for X Evaluating Fns X X X Modeling Probability X X Rates/Slopes X X X Logarithmic Fns Polynomials X Power Fns Conics Piecewise Fns Trigonometry Integration Differentiation Limits Space Math http://spacemath.gsfc.nasa.gov Mathematics Topic Matrix (cont'd) vii Topic Problem Numbers 6 6 6 6 6 6 6 7 7 7 7 7 7 7 7 7 7 8 8 8 8 8 8 8 8 8 8 9 9 9 9 3 4 5 6 7 8 9 0 1 2 3 4 5 6 7 8 9 0 1 2 3 4 5 6 7 8 9 0 1 2 3 Inquiry X X Technology, rulers Numbers, patterns, X percentages Averages Time, distance X ,speed Areas and volumes X X X X Scale drawings X X X X Geometry X X X X X X X X X Scientific X X X X X X X X X Notation Unit Conversions X Fractions Graph or Table X X X X X X X X X X X Analysis Solving for X Evaluating Fns X X X X X X X X X Modeling X X Probability X X X X Rates/Slopes X Logarithmic Fns X Polynomials X Power Fns Exponential Fns Conics Piecewise Fns Trigonometry X X X X Matrices X Integration Differentiation Limits Space Math http://spacemath.gsfc.nasa.gov Mathematics Topic Matrix (cont'd) viii Topic Problem Numbers 9 9 9 9 9 9 4 5 6 7 8 9 Inquiry X Technology, X X rulers Numbers, patterns, percentages Averages Time, distance X X X ,speed Areas and volumes Scale drawings X X Geometry Scientific X X Notation Unit Conversions Fractions Graph or Table X X X Analysis Solving for X Evaluating Fns X X Modeling Probability Rates/Slopes Logarithmic Fns Polynomials Power Fns Exponential Fns Conics Piecewise Fns Trigonometry Integration Differentiation Limits Space Math http://spacemath.gsfc.nasa.gov How to use this book ix Teachers continue to look for ways to make math meaningful by providing students with problems and examples demonstrating its applications in everyday life.
Recommended publications
  • Detection and Characterization of Hot Subdwarf Companions of Massive Stars Luqian Wang
    Georgia State University ScholarWorks @ Georgia State University Physics and Astronomy Dissertations Department of Physics and Astronomy 8-13-2019 Detection And Characterization Of Hot Subdwarf Companions Of Massive Stars Luqian Wang Follow this and additional works at: https://scholarworks.gsu.edu/phy_astr_diss Recommended Citation Wang, Luqian, "Detection And Characterization Of Hot Subdwarf Companions Of Massive Stars." Dissertation, Georgia State University, 2019. https://scholarworks.gsu.edu/phy_astr_diss/119 This Dissertation is brought to you for free and open access by the Department of Physics and Astronomy at ScholarWorks @ Georgia State University. It has been accepted for inclusion in Physics and Astronomy Dissertations by an authorized administrator of ScholarWorks @ Georgia State University. For more information, please contact [email protected]. DETECTION AND CHARACTERIZATION OF HOT SUBDWARF COMPANIONS OF MASSIVE STARS by LUQIAN WANG Under the Direction of Douglas R. Gies, PhD ABSTRACT Massive stars are born in close binaries, and in the course of their evolution, the initially more massive star will grow and begin to transfer mass and angular momentum to the gainer star. The mass donor star will be stripped of its outer envelope, and it will end up as a faint, hot subdwarf star. Here I present a search for the subdwarf stars in Be binary systems using the International Ultraviolet Explorer. Through spectroscopic analysis, I detected the subdwarf star in HR 2142 and 60 Cyg. Further analysis led to the discovery of an additional 12 Be and subdwarf candidate systems. I also investigated the EL CVn binary system, which is the prototype of class of eclipsing binaries that consist of an A- or F-type main sequence star and a low mass subdwarf.
    [Show full text]
  • Casiopea 1979 Full Album Download
    casiopea 1979 full album download IsraBox - Music is Life! Casiopea - Best of Casiopea-Alfa Collection (2009) Artist : Casiopea Title : Best of Casiopea-Alfa Collection Year Of Release : 2009 Label : Alfa Records Genre : Jazz, Jazz Fusion Quality : MP3/320 kbps Total Time : 77:28 Total Size : 183 MB(+3%) Casiopea - Jive Jive (2002) [24bit FLAC] Artist : Casiopea Title : Jive Jive Year Of Release : 1983 / 2002 Label : Village Records / Alfa ​– ALR 28052 / Vinyl, LP Genre : Jazz-Rock, Jazz- Funk, Smooth Jazz, Fusion Quality : FLAC (tracks+.cue,log scans) / FLAC (tracks) 24bit-192kHz Total Time : 38:18 Total Size : 245 Mb / 1.48 Gb. Casiopea - Dramatic (1993) Artist : Casiopea Title : Dramatic Year Of Release : 1993 Label : Alfa Records Genre : Jazz, Fusion Quality : FLAC (tracks+.cue, log) Total Time : 51:04 Total Size : 351 MB. Casiopea - Answers (1994) Artist : Casiopea Title : Answers Year Of Release : 1994 Label : Alfa Genre : Smooth Jazz, Jazz-Funk, Fusion Quality : FLAC (image+.cue, log, Artwork) Total Time : 54:13 Total Size : 356 MB. Casiopea - Material (1999) CD Rip. Artist : Casiopea Title : Material Year Of Release : 1999 Label : Pony Canyon[PCCR-00304] Genre : Jazz, Fusion Quality : FLAC (tracks + .cue,log,scans) Total Time : 49:15 Total Size : 323 MB(+3%) Casiopea - Down Upbeat (1984) Artist : Casiopea Title : Down Upbeat Year Of Release : 1984 Label : Alfa Records Genre : jazz, funk, fusion Quality : APE (image+.cue,log,scans) Total Time : 38:26 Total Size : 228 MB. Casiopea - Main Gate (2001) Artist : Casiopea Title : Main
    [Show full text]
  • A Decadal Strategy for Solar and Space Physics
    Space Weather and the Next Solar and Space Physics Decadal Survey Daniel N. Baker, CU-Boulder NRC Staff: Arthur Charo, Study Director Abigail Sheffer, Associate Program Officer Decadal Survey Purpose & OSTP* Recommended Approach “Decadal Survey benefits: • Community-based documents offering consensus of science opportunities to retain US scientific leadership • Provides well-respected source for priorities & scientific motivations to agencies, OMB, OSTP, & Congress” “Most useful approach: • Frame discussion identifying key science questions – Focus on what to do, not what to build – Discuss science breadth & depth (e.g., impact on understanding fundamentals, related fields & interdisciplinary research) • Explain measurements & capabilities to answer questions • Discuss complementarity of initiatives, relative phasing, domestic & international context” *From “The Role of NRC Decadal Surveys in Prioritizing Federal Funding for Science & Technology,” Jon Morse, Office of Science & Technology Policy (OSTP), NRC Workshop on Decadal Surveys, November 14-16, 2006 2 Context The Sun to the Earth—and Beyond: A Decadal Research Strategy in Solar and Space Physics Summary Report (2002) Compendium of 5 Study Panel Reports (2003) First NRC Decadal Survey in Solar and Space Physics Community-led Integrated plan for the field Prioritized recommendations Sponsors: NASA, NSF, NOAA, DoD (AFOSR and ONR) 3 Decadal Survey Purpose & OSTP* Recommended Approach “Decadal Survey benefits: • Community-based documents offering consensus of science opportunities
    [Show full text]
  • Solar Activity Affecting Space Weather
    March 7, 2006, STP11, Rio de Janeiro, Brazil Solar Activity Affecting Space Weather Kazunari Shibata Kwasan and Hida Observatories Kyoto University, Japan contents • Introduction • Flares • Coronal Mass Ejections(CME) • Solar Wind • Future Projects Japanese newspaper reporting the big flare of Oct 28, 2003 and its impact on the Earth big flare (third largest flare in record) on Oct 28, 2003 X17 X-ray Intensity time A big flare on Oct 28, 2003 (third largest X-ray intensity in record) EUV Visible light SOHO/EIT SOHO/LASCO • Flare occurred at UT11:00 on Oct 28 Magnetic Storm on the Earth Around UT 6:00- Aurora observed in Japan on Oct 29, 2003 at around UT 14:00 on Oct 29, 2003 During CAWSES campaign observations (Shinohara) Xray X17 X6.2 Proton 10MeV 100MeV Vsw 44h 30h Bt Bz Dst Flares What is a flare ? Hα chromosphere 10,000 K Discovered in Mid 19C Near sunspots=> energy source is magnetic energy size~(1-10)x 104 km Total energy 1029 -1032erg (~ 105ー108 hydrogen bombs ) (Hida Observatory) Prominence eruption (biggest: June 4, 1946) Electro- magnetic Radio waves emitted from a flare (Svestka Visible 1976) UV 1hour time Solar corona observed in soft X-rays (Yohkoh) Soft X-ray telescope (1keV) Coronal plasma 2MK-10MK X-ray view of a flare Magnetic reconneciton Hα X-ray MHD simulation of a solar flare based on reconnection model including heat conduction and chromospheric evaporation (Yokoyama-Shibata 1998, 2001) A solar flare Observed with Yohkoh soft X-ray telescope (Tsuneta) Relation between filament (prominence) eruption and flare A flare
    [Show full text]
  • Optical and Radio Solar Observation for Space Weather
    2 Solar and Solar wind 2-1 Optical and Radio Solar Observation for Space Weather AKIOKA Maki, KONDO Tetsuro, SAGAWA Eiichi, KUBO Yuuki, and IWAI Hironori Researches on solar observation technique and data utilization are important issues of space weather forecasting program. Hiraiso Solar Observatory is a facility for R & D for solar observation and routine solar observation for CRL's space environment information service. High definition H alpha solar telescope is an optical telescope with very narrow pass-band filter for high resolution full-disk imaging and doppler mapping of upper atmos- phere dynamics. Hiraiso RAdio-Spectrograph (HiRAS) provides information on coronal shock wave and particle acceleration in the soar atmosphere. These information are impor- tant for daily space weather forecasting and alert. In this article, high definition H alpha solar telescope and radio spectrograph system are briefly introduced. Keywords Space weather forecast, Solar observation, Solar activity 1 Introduction X-ray and ultraviolet radiation resulting from solar activities and solar flares cause distur- 1.1 The Sun as the Origin of Space bances in the ionosphere and the upper atmos- Environment Disturbances phere, which in turn cause communication dis- The space environment disturbance phe- ruptions and affect the density structure of the nomena studied in space weather forecasting Earth's atmosphere. CME induce geomagnet- at CRL include a wide range of phenomena ic storms and ionospheric disturbances upon such as solar energetic particle (SEP) events, reaching the Earth's magnetosphere, and are geomagnetic storms, ionospheric disturbances, believed to be responsible for particle acceler- and radiation belt activity. All of these space environment disturbance events are believed to have solar origins.
    [Show full text]
  • Coordinate Systems for Solar Image Data
    A&A 449, 791–803 (2006) Astronomy DOI: 10.1051/0004-6361:20054262 & c ESO 2006 Astrophysics Coordinate systems for solar image data W. T. Thompson L-3 Communications GSI, NASA Goddard Space Flight Center, Code 612.1, Greenbelt, MD 20771, USA e-mail: [email protected] Received 27 September 2005 / Accepted 11 December 2005 ABSTRACT A set of formal systems for describing the coordinates of solar image data is proposed. These systems build on current practice in applying coordinates to solar image data. Both heliographic and heliocentric coordinates are discussed. A distinction is also drawn between heliocentric and helioprojective coordinates, where the latter takes the observer’s exact geometry into account. The extension of these coordinate systems to observations made from non-terrestial viewpoints is discussed, such as from the upcoming STEREO mission. A formal system for incorporation of these coordinates into FITS files, based on the FITS World Coordinate System, is described, together with examples. Key words. standards – Sun: general – techniques: image processing – astronomical data bases: miscellaneous – methods: data analysis 1. Introduction longitude and latitude – only need to worry about two spatial dimensions. The same can be said for normal cartography of Solar research is becoming increasingly more sophisticated. a planet such as Earth. However, to properly treat the complete Advances in solar instrumentation have led to increases in spa- range of solar phenomena, from the interior out into the corona, tial resolution, and will continue to do so. Future space mis- a complete three-dimensional coordinate system is required. sions will view the Sun from different perspectives than the Unfortunately, not all the information necessary to determine current view from ground-based observatories, or satellites in the full three-dimensional position of a solar feature is usually Earth orbit.
    [Show full text]
  • CESRA Workshop 2019: the Sun and the Inner Heliosphere Programme
    CESRA Workshop 2019: The Sun and the Inner Heliosphere July 8-12, 2019, Albert Einstein Science Park, Telegrafenberg Potsdam, Germany Programme and abstracts Last update: 2019 Jul 04 CESRA, the Community of European Solar Radio Astronomers, organizes triennial workshops on investigations of the solar atmosphere using radio and other observations. Although special emphasis is given to radio diagnostics, the workshop topics are of interest to a large community of solar physicists. The format of the workshop will combine plenary sessions and working group sessions, with invited review talks, oral contributions, and posters. The CESRA 2019 workshop will place an emphasis on linking the Sun with the heliosphere, motivated by the launch of Parker Solar Probe in 2018 and the upcoming launch of Solar Orbiter in 2020. It will provide the community with a forum for discussing the first relevant science results and future science opportunities, as well as on opportunity for evaluating how to maximize science return by combining space-borne observations with the wealth of data provided by new and future ground-based radio instruments, such as ALMA, E-OVSA, EVLA, LOFAR, MUSER, MWA, and SKA, and by the large number of well-established radio observatories. Scientific Organising Committee: Eduard Kontar, Miroslav Barta, Richard Fallows, Jasmina Magdalenic, Alexander Nindos, Alexander Warmuth Local Organising Committee: Gottfried Mann, Alexander Warmuth, Doris Lehmann, Jürgen Rendtel, Christian Vocks Acknowledgements The CESRA workshop has received generous support from the Leibniz Institute for Astrophysics Potsdam (AIP), which provides the conference venue at Telegrafenberg. Financial support for travel and organisation has been provided by the Deutsche Forschungsgemeinschaft (DFG) (GZ: MA 1376/22-1).
    [Show full text]
  • Culmination of a Constellation
    Culmination of a Constellation Over any night, stars and constellations in the sky will appear to move from east to west due to the Earth’s rotation on its axis. A constellation will culminate (reach its highest point in the sky for your location) when it centres on the meridian - an imaginary line that runs across the sky from north to south and also passes through the zenith (the point high in the sky directly above your head). For example: When to Observe Constellations The taBle shows the approximate time (AEST) constellations will culminate around the middle (15th day) of each month. Constellations will culminate 2 hours earlier for each successive month. Note: add an hour to the given time when daylight saving time is in effect. The time “12” is midnight. Sunrise/sunset times are rounded off to the nearest half an hour. Sun- Jan Feb Mar Apr May Jun Jul Aug Sep Oct Nov Dec Rise 5am 5:30 6am 6am 7am 7am 7am 6:30 6am 5am 4:30 4:30 Set 7pm 6:30 6pm 5:30 5pm 5pm 5pm 5:30 6pm 6pm 6:30 7pm And 5am 3am 1am 11pm 9pm Aqr 5am 3am 1am 11pm 9pm Aql 4am 2am 12 10pm 8pm Ara 4am 2am 12 10pm 8pm Ari 5am 3am 1am 11pm 9pm Aur 10pm 8pm 4am 2am 12 Boo 3am 1am 11pm 9pm 7pm Cnc 1am 11pm 9pm 7pm 3am CVn 3am 1am 11pm 9pm 7pm CMa 11pm 9pm 7pm 3am 1am Cap 5am 3am 1am 11pm 9pm 7pm Car 2am 12 10pm 8pm 6pm Cen 4am 2am 12 10pm 8pm 6pm Cet 4am 2am 12 10pm 8pm Cha 3am 1am 11pm 9pm 7pm Col 10pm 8pm 4am 2am 12 Com 3am 1am 11pm 9pm 7pm CrA 3am 1am 11pm 9pm 7pm CrB 4am 2am 12 10pm 8pm Crv 3am 1am 11pm 9pm 7pm Cru 3am 1am 11pm 9pm 7pm Cyg 5am 3am 1am 11pm 9pm 7pm Del
    [Show full text]
  • Subgiants As Probes of Galactic Chemical Evolution
    Astronomy & Astrophysics manuscript no. Thoren September 9, 2018 (DOI: will be inserted by hand later) Subgiants as probes of galactic chemical evolution ⋆, ⋆⋆, ⋆⋆⋆ Patrik Thor´en, Bengt Edvardsson and Bengt Gustafsson Department of Astronomy and Space Physics, Uppsala Astronomical Observatory, Box 515, S-751 20 Uppsala, Sweden Received 12 March 2004 / Accepted 28 May 2004 Abstract. Chemical abundances for 23 candidate subgiant stars have been derived with the aim at exploring their usefulness for studies of galactic chemical evolution. High-resolution spectra from ESO CAT-CES and NOT- SOFIN covered 16 different spectral regions in the visible part of the spectrum. Some 200 different atomic and molecular spectral lines have been used for abundance analysis of ∼ 30 elemental species. The wings of strong, pressure-broadened metal lines were used for determination of stellar surface gravities, which have been compared with gravities derived from Hipparcos parallaxes and isochronic masses. Stellar space velocities have been derived from Hipparcos and Simbad data, and ages and masses were derived with recent isochrones. Only 12 of the stars turned out to be subgiants, i.e. on the “horizontal” part of the evolutionary track between the dwarf- and the giant stages. The abundances derived for the subgiants correspond closely to those of dwarf stars. With the possible exceptions of lithium and carbon we find that subgiant stars show no “chemical” traces of post-main-sequence evolution and that they are therefore very useful targets for studies of galactic chemical evolution. Key words. stars:abundances – stars:evolution – galaxy:abundances – galaxy:evolution 1. Introduction The volume is limited by the low luminosities of the dwarfs used in the surveys, and by the limited view in cer- Abundance patterns in stellar populations have proven to tain directions through the galactic disk.
    [Show full text]
  • 20171030-SORS-2018-1.7.Pdf
    SMITHSONIAN OPPORTUNITIES FOR RESEARCH AND STUDY 2018 Office of Fellowships and Internships Smithsonian Institution Washington, DC The Smithsonian Opportunities for Research and Study Guide Can be Found Online at http://www.smithsonianofi.com/sors-introduction/ Version 1.7 (Updated October 30, 2017) Copyright © 2017 by Smithsonian Institution Table of Contents Table of Contents..................................................................................................................................................................................... 1 How to Use This Book ........................................................................................................................................................................... 1 Anacostia Community Museum (ACM) .......................................................................................................................................... 3 Archives of American Art (AAA) ........................................................................................................................................................ 5 Asian Pacific American Center (APAC) ........................................................................................................................................... 7 Center for Folklife and Cultural Heritage (CFCH) ...................................................................................................................... 8 Cooper-Hewitt, National Design Museum (CHNDM) ..........................................................................................................
    [Show full text]
  • Mission Operations and Communication Services
    Space Communications and Navigation (SCaN) Overview Astrophysics Explorers SMEX Preproposal Conference Jerry Mason May 2, 2019 Agenda • Space Communications and Navigation (SCaN) overview • AO Considerations and Requirements • Spectrum Access & Licensing • SCaN’s Mission Commitment Offices • Points of contact •2 SCaN is Responsible for all NASA Space Communications • Responsible for Agency-wide operations, management, and development of all NASA space communications capabilities and enabling technology. • Expand SCaN capabilities to enable and enhance robotic and human exploration. • Manage spectrum and represent NASA on national and international spectrum management programs. • Develop space communication standards as well as Positioning, Navigation, and Timing (PNT) policy. • Represent and negotiate on behalf of NASA on all matters related to space telecommunications in coordination with the appropriate offices and flight mission directorates. •3 Supporting Over 100 Missions • SCaN supports over 100 space missions with the three networks. – Which includes every US government launch and early orbit flight • Earth Science – Earth observation missions – Global observation of climate, Land, Sea state and Atmospheric conditions. – Aura, Aqua, Landsat, Ice Cloud and Land Elevation Satellite (ICESAT-2), Orbiting Carbon Observatory (OCO- 2) • Heliophysics – Solar observation-Understanding the Sun and its effect on Space and Earth. – Parker Solar Probe, Solar Dynamics Observer (SDO), Solar Terrestrial Relations Observatory (STEREO) • Astrophysics – Studying the Universe and its origins. – Hubble Space Telescope, Chandra X-ray Observatory, James E. Webb Space Telescope (JWST), WFIRST • Planetary – Exploring our solar system’s content and composition – Voyagers-1/2, Mars Atmosphere and Volatile Evolution (MAVEN), InSight, Lunar Reconnaissance Orbiter (LRO) • Human Space Flight – Human tended Exploration missions, Commercial Space transportation and Space Communications.
    [Show full text]
  • Proposed Changes to Sacramento Peak Observatory Operations: Historic Properties Assessment of Effects
    TECHNICAL REPORT Proposed Changes to Sacramento Peak Observatory Operations: Historic Properties Assessment of Effects Prepared for National Science Foundation October 2017 CH2M HILL, Inc. 6600 Peachtree Dunwoody Rd 400 Embassy Row, Suite 600 Atlanta, Georgia 30328 Contents Section Page Acronyms and Abbreviations ............................................................................................................... v 1 Introduction ......................................................................................................................... 1-1 1.1 Definition of Proposed Undertaking ................................................................................ 1-1 1.2 Proposed Alternatives Background ................................................................................. 1-1 1.3 Proposed Alternatives Description .................................................................................. 1-1 1.4 Area of Potential Effects .................................................................................................. 1-3 1.5 Methodology .................................................................................................................... 1-3 1.5.1 Determinations of Eligibility ............................................................................... 1-3 1.5.2 Finding of Effect .................................................................................................. 1-9 2 Identified Historic Properties ...............................................................................................
    [Show full text]