DOCSLIB.ORG

Genesis Radiation Environment

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Genesis Radiation Environment https://ntrs.nasa.gov/search.jsp?R=20070014073 2019-08-30T00:44:36+00:00Z 1 Source of Acquisition NASA Marshall Space Flight Center Genesis Radiation Environment Joseph I. Minow* NASA Marshull Space Flight Center, Huntsville, AL 35812 USA Richard L. Altstatt' and William C. Skipworth* Jacobs Engineering, Marshall Space Flight Center Group, Huntsville, AL 35812 USA The Genesis spacecraft launched on 8 August 2001 sampled solar wind environments at L1 from 2001 to 2004. After the Science Capsule door was opened, numerous foils and samples were exposed to the various solar wind environments during periods including slow solar wind from the streamer belts, fast solar wind flows from coronal holes, and coronal mass ejections. The Survey and Examination of Eroded Returned Surfaces (SEERS) program led by NASA's Space Environments and Effects program had initiated access for the space materials community to the remaining Science Capsule hardware after the science samples had been removed for evaluation of materials exposure to the space environment. This presentation will describe the process used to generate a reference radiation Genesis Radiation Environment developed for the SEERS program for use by the materials science community in their analyses of the Genesis hardware. I. Introduction ASA's Space Environments and Effects (SEE) Program initiated the Surveying and Examination of Eroded N Returned Surfaces (SEERS) Initiative in 2003. The goal of the Initiative was to provide leadership in the engineering analysis of returned flight hardware by supporting a comprehensive effort to understand environmental effects due to solar W, ionizing radiation, plasmas, neutral contamination, meteoroids, and other conditions experienced during the mission (not primary science mission objectives). Initial efforts focused on coordinating the access by the materials engineering community to the remaining Genesis and Stardust hardware once the science materials were removed from the sample returned capsules. The Genesis spacecraft sampled solar wind environments at the Sun-Earth L1 point for a period of approximately three years before returning samples of solar wind materials in September 2004 [Wiens et al., 2002; Barraclough et al., 20041 and the Stardust spacecraft returned material from Comet P/Wild 2 and interstellar dust to Earth in January 2006. In support of the SEERS Initiative, the SEE Program funded development of a reference radiation environment for the Genesis spacecraft for use by materials 200 engineers in their evaluation of the space exposed materials. This paper describes the status of this radiation environment development. 11. Genesis Spacecraft and Plasma Data Genesis was launched on 8 August 2001 and inserted into a halo orbit about the Sun-Earth L1 point (Figure 1) on 16 November 2001 with sample collections obtained over an -200 884 day period from 3 December 2001 to 2 April 2004. 300 200 100 0 - 1Ow!OQ-300 Figure 2 shows the spacecraft with the solar arrays, the >G.,, me1 spacecraft bus with the Genesis Ion Monitor (GIM) and Figure 1. Genesis Orbit. Genesis trajectory Electron Monitor (GEM) plasma instruments and support &om Earth to L1 (black) and for 30 November hardware, and the deployed Science Capsule in solar wind 2001 to 1 April 2004 including the period the collection mode. The Science Capsule contains the solar Science Capsule was exposed to the solar wind wind collection materials and was designed to separate from (red). the spacecraft bus after the science mission was complete *AST, Flight Vehicle Space Environments, Spacecraft and Vehicle Systems Department, NASA/MSFC/EV13, Huntsville, AL,Senior Member AIAA 'Radiation Effects Engineer, Jacobs Engineering, MSFC Group, MSFCEV13, Huntsville, AL, *Currentposition: Senior Sohare Engineer, Ameri-Tech International, Inc., Harvest, AL. 1 American Institute of Aeronautics and Astronautics and return to Earth. The GEM and GIM plasma instruments [Barracloughet al., 2003; Neugebauer et al., 20031 were used to support the solar wind collection science by providing a real time monitor of solar wind conditions allowing the sample carriers to selectively collect material from coronal holes (fast >500 Msec solar wind), interstreams (slow <500 Msec solar wind), and coronal mass ejections. GIM is an electrostatic analyzer providing a complete set of ion flux measurements every 2.5 minutes over a 0.1 eV to 14 keV energy range and GEM is an electrostatic analyzer for measuring electron Figure 2. Genesis Spacecraft and Orbit. Artist flux over the range of energies from 0.001 to 1.4 keV. concept of the Genesis spacecraft (courtesy JPL) Both instruments provided angular information on ion showing the Science Capsule (SC), Genesis Ion and electron flux but this data was not available for the Monitor (GIM) and Electron Monitor (GEM) radiation study. The radiation environments described instruments. here are based only on reconstructed environments derived from the GGion moments (Figure 3) provided by the PI and the public access Genesis data web site (httu://genesis.lanl.gov/dots/index.html). Ion moments derived from the GIM measurements are shown in Figure 3 from the start of instrument operations in August 2001 through the end of April 2004 during the period the Science Capsule was exposed to the solar wind highlighted in yellow. The ion density shown in the top panel of Figure 3 includes both the proton (black symbols) and helium (blue symbols) components of the ion flow which accounts for most of the solar wind mass. The helium density was computed from the He'm ratio reported in the Genesis GIM moments and the proton density. Gaps in the data set occur during periods when the GIM instrument was powered off for station keeping maneuvers and solar proton events. All the moment values were interpolated across these data gaps onto an evenly spaced set of time values (red) The solar wind proton speed and temperatures are shown in the middle two panels. Corresponding helium parameters are not available in the moments so assumptions must be made to incorporate their effects into the reconstructed differential flux models. Observations of differential streaming velocities between solar wind protons and alpha particles have been reported with the alpha velocity exceeding the proton velocity by factors ranging from a few to 50 Ms or more [Yermolaev and Stupin, 1997; Reisenfeld et al., 20011 with the largest differential streaming velocities occurring during periods of high speed solar wind flows and small differential alpha-proton velocity at 1 AU for flows <400 to 500 km/s [Neugebauer et al., 19961. We have adopted a linear fit to alpha-proton differential streaming velocities (Figure 4) observed by instruments on the Helios [Marsch et al., 19821 and WIND [Steinberg et al., 19971 spacecraft to provide a method for deriving mean helium velocities from proton velocity moments available in the Genesis data set. The Marsh et al. [ 19821 values given in Figure 3 are the 0.95 AU alpha-proton streaming values extracted fiom Neugebauer et al. [1996] and assigned to the midpoint of the proton velocity bins. Steinberg et al. [ 19971 in contrast reports average alpha-proton streaming values of 6.Q9.1 MSfor Vp400 WS,2& 17 km/s for 400 kmh IVp -< 500 Ws,and 4 lk 19 km/s for Vp>500 km/s. In order to merge both data sets into the linear fit, we have computed the mean Genesis solar wind velocities V,, ws= 349 km Is and V,500ws = 605 km Is and assigned the corresponding Steinberg et al. [1997] alpha-proton differential streaming speeds of -6 km/s and -4 1 Ws,respectively, to these values with the 400-500 km/s differential streaming value assigned to a proton velocity of 450 kmls. The resulting linear fit for the differential velocity between alpha particles and protons is given by the equation AVHe-p = 0.104Vp -31.66 kmIS which is used in our model to provide the Genesis helium ion flow velocity. 2 American Institute of Aeronautics and Astronautics Lii 2001.5 2002.0 2002.5 2003.0 2003.5 2044.0 2044.5 Time (UT) Figure 3. Genesis Ion Moments and Ion Flux. GIM ion moments (ion density Ni, solar wind ion velocity VS, and proton temperature Tp) are shown in the top three panels with the ion flux derived fiom the moments in the bottom panel. The period the Science Capsule was open is highlighted in yellow. Original GIM records are shown black (protons) and blue (helium) with interpolated values in red. Helium to proton temperature ratios reported in the literature typically range in values from THJTH - 3 to THJTH - 6 depending on the nature of the solar wind flow regime. For example, Reisenfeld et ul. [2001] use data from Feldman et al., [1977] to obtain an average ratio of THJTH - 4.9h1.8 for all solar wind flows, THJTH - 6.2h1.3 for flows >650 km/s, and THJTH - 3.2rt0.9 for flows <350 km/s. Mursch et ul. [1982] report ratios of THJTH - 3.0 for >600 km/s solar wind flows and THJTH - 2.3 for solar wind flows <400 km/s. Yermoluev and Stupin [1997] categorize solar wind data fiom the Prognoz -7 spacecraft into five solar wind flow regimes and report helium to proton temperature ratios of THJTH - 2.7k3.0 for the heliospheric current sheet, THJTH - 423.6 for coronal streamers, THJTH - 4.4h3.0 for coronal holes, THJTH - 3.3h2.6 for shocked solar wind, and THJTH - 3.9h2.8 for coronal mass ejections. For the results presented in this paper, we will adopt the ratio THJTH - 4.0 independent of solar wind velocity. Proton (black) and helium (blue) flux is presented in the bottom panel and is plotted over the interpolated flux values (red) that are based on the solar wind ram flux (-Vsw*Ni). The flux exhibits nearly the same variability as the ion density due to the inverse relationship between solar wind velocity and density [Burluguand Ogilvie, 19701 and the relatively smaller variation in solar wind velocity.
Load more

Recommended publications
  • Planetary Science Division Status Report
    Planetary Science Division Status Report Jim Green NASA, Planetary Science Division January 26, 2017 Astronomy and Astrophysics Advisory CommiBee Outline • Planetary Science ObjecFves • Missions and Events Overview • Flight Programs: – Discovery – New FronFers – Mars Programs – Outer Planets • Planetary Defense AcFviFes • R&A Overview • Educaon and Outreach AcFviFes • PSD Budget Overview New Horizons exploresPlanetary Science Pluto and the Kuiper Belt Ascertain the content, origin, and evoluFon of the Solar System and the potenFal for life elsewhere! 01/08/2016 As the highest resolution images continue to beam back from New Horizons, the mission is onto exploring Kuiper Belt Objects with the Long Range Reconnaissance Imager (LORRI) camera from unique viewing angles not visible from Earth. New Horizons is also beginning maneuvers to be able to swing close by a Kuiper Belt Object in the next year. Giant IcebergsObjecve 1.5.1 (water blocks) floatingObjecve 1.5.2 in glaciers of Objecve 1.5.3 Objecve 1.5.4 Objecve 1.5.5 hydrogen, mDemonstrate ethane, and other frozenDemonstrate progress gasses on the Demonstrate Sublimation pitsDemonstrate from the surface ofDemonstrate progress Pluto, potentially surface of Pluto.progress in in exploring and progress in showing a geologicallyprogress in improving active surface.in idenFfying and advancing the observing the objects exploring and understanding of the characterizing objects The Newunderstanding of Horizons missionin the Solar System to and the finding locaons origin and evoluFon in the Solar System explorationhow the chemical of Pluto wereunderstand how they voted the where life could of life on Earth to that pose threats to and physical formed and evolve have existed or guide the search for Earth or offer People’sprocesses in the Choice for Breakthrough of thecould exist today life elsewhere resources for human Year forSolar System 2015 by Science Magazine as exploraon operate, interact well as theand evolve top story of 2015 by Discover Magazine.
    [Show full text]
  • The Mars 2001 Odyssey and the "Autogen" Process
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by DigitalCommons@USU AUTOGEN: The Mars 2001 Odyssey and the "Autogen" Process By Roy Gladden June 6, 2002 Jet Propulsion Laboratory / California Institute of Technology Pasadena, California Abstract In many deep space and interplanetary missions, it is widely recognized that the scheduling of many commands to operate a spacecraft can follow very regular patterns. In these instances, it is greatly desired to convert the knowledge of how commands are scheduled into algorithms in order to automate the development of command sequences. In doing so, it is possible to dramatically reduce the number of people and work-hours that are required to develop a sequence. The development of the "autogen" process for the Mars 2001 Odyssey spacecraft is one implementation of this concept. It combines robust scheduling algorithms with software that is compatible with pre- existing "uplink" software, and literally reduced the duration of some sequence generation processes from weeks to minutes. This paper outlines the "autogen" tools and processes and describes how they have been implemented for the various phases of the Mars 2001 Odyssey mission. What is autogen? manually building the commands for lengthy and well- understood command sequences, efforts were made to The term "autogen" is applied in two different ways. develop software that would automatically schedule the First, "autogen," in its broadest sense, identifies a commands given certain input data. By taking the process that may be used to automatically generate knowledge for how commands were to be scheduled sequences for a spacecraft and, second, it is a Solaris and writing algorithms to replicate that knowledge, it script that has been used to facilitate this process.
    [Show full text]
  • Stardust Sample Return
    National Aeronautics and Space Administration Stardust Sample Return Press Kit January 2006 www.nasa.gov Contacts Merrilee Fellows Policy/Program Management (818) 393-0754 NASA Headquarters, Washington DC Agle Stardust Mission (818) 393-9011 Jet Propulsion Laboratory, Pasadena, Calif. Vince Stricherz Science Investigation (206) 543-2580 University of Washington, Seattle, Wash. Contents General Release ............................................................................................................... 3 Media Services Information ……………………….................…………….................……. 5 Quick Facts …………………………………………..................………....…........…....….. 6 Mission Overview …………………………………….................……….....……............…… 7 Recovery Timeline ................................................................................................ 18 Spacecraft ………………………………………………..................…..……...........……… 20 Science Objectives …………………………………..................……………...…..........….. 28 Why Stardust?..................…………………………..................………….....………............... 31 Other Comet Missions .......................................................................................... 33 NASA's Discovery Program .................................................................................. 36 Program/Project Management …………………………........................…..…..………...... 40 1 2 GENERAL RELEASE: NASA PREPARES FOR RETURN OF INTERSTELLAR CARGO NASA’s Stardust mission is nearing Earth after a 2.88 billion mile round-trip journey
    [Show full text]
  • The Messenger Sept. 8Th GENESIS SUNDAY
    WHAT’S INSIDE: Stewardship and Finance……...pg. 2 Congregational News…………... pg. 3 Celebrating Lohmen……………..pg. 4 Adult Education…………………...pg. 5 Faith Through the Generations….pgs. 6-7 Community Events…………..pgs. 8-9 WPC Food Pantry………………..pg. 10 The Messenger Prayer Ministry & Groups…….pg. 11 Environmental Stewardship...pg. 12 VOLUME 89, ISSUE 8 Confirmation Class……………...pg. 12 AUGUST 2019 Sept. 8th GENESIS SUNDAY Bring the whole family and invite a friend for a day full of food, games, live music, and lots of wild surprises! 2 CONGREGATIONAL NEWS The Pastor Nominating Committee Report (PNC) Nine members of the congregation were nominated and elected to serve on the Pastor Nominating Committee (PNC). They are: Andrew Finkner, Michael Gregg, Steve Hughes, Jim Kinkennon, Sandi Larson, Deb Schorr, Alisha Stokes, Allen Wachter and Joyce Douglas, Moderator. These members represent the whole congregation and have the responsibility for nominating an individual to present to the congregation to serve as our Head of Staff. In the future months, the PNC will journey through the search process seeking to hear the call of Christ. The first step will be to review the documentation from our group meetings held last Fall which represents the needs of Westminster and then complete the Ministry Information Form. The PNC has received reading materials already and will begin meeting together in early August. The PNC plans to keep the congregation informed on the status of this search. Our journey begins……… Joyce Douglas, Moderator LOOKING AHEAD Sun. August 4th—Celebrating Lohmen, our sister church in Germany (after worship, meet in chancel) Tues., Aug.
    [Show full text]
  • Titan and Enceladus $1 B Mission
    JPL D-37401 B January 30, 2007 Titan and Enceladus $1B Mission Feasibility Study Report Prepared for NASA’s Planetary Science Division Prepared By: Kim Reh Contributing Authors: John Elliott Tom Spilker Ed Jorgensen John Spencer (Southwest Research Institute) Ralph Lorenz (The Johns Hopkins University, Applied Physics Laboratory) KSC GSFC ARC Approved By: _________________________________ Kim Reh Dr. Ralph Lorenz Jet Propulsion Laboratory The Johns Hopkins University, Applied Study Manager Physics Laboratory Titan Science Lead _________________________________ Dr. John Spencer Southwest Research Institute Enceladus Science Lead Pre-decisional — For Planning and Discussion Purposes Only Titan and Enceladus Feasibility Study Report Table of Contents JPL D-37401 B The following members of an Expert Advisory and Review Board contributed to ensuring the consistency and quality of the study results through a comprehensive review and advisory process and concur with the results herein. Name Title/Organization Concurrence Chief Engineer/JPL Planetary Flight Projects Gentry Lee Office Duncan MacPherson JPL Review Fellow Glen Fountain NH Project Manager/JHU-APL John Niehoff Sr. Research Engineer/SAIC Bob Pappalardo Planetary Scientist/JPL Torrence Johnson Chief Scientist/JPL i Pre-decisional — For Planning and Discussion Purposes Only Titan and Enceladus Feasibility Study Report Table of Contents JPL D-37401 B This page intentionally left blank ii Pre-decisional — For Planning and Discussion Purposes Only Titan and Enceladus Feasibility Study Report Table of Contents JPL D-37401 B Table of Contents 1. EXECUTIVE SUMMARY.................................................................................................. 1-1 1.1 Study Objectives and Guidelines............................................................................ 1-1 1.2 Relation to Cassini-Huygens, New Horizons and Juno.......................................... 1-1 1.3 Technical Approach...............................................................................................
    [Show full text]
  • Genesis Sample Return
    NATIONAL AERONAUTICS AND SPACE ADMINISTRATION Genesis Sample Return Press Kit September 2004 Media Contacts Donald Savage Policy/program management 202/358-1727 Headquarters, [email protected] Washington, D.C. DC Agle Genesis mission 818/393-9011 Jet Propulsion Laboratory, [email protected] Pasadena, Calif. Robert Tindol Principal investigator 626/395-3631 California Institute of Technology [email protected] Pasadena, Calif. Contents General Release ……................……………………………….........................………..……....… 3 Media Services Information …………………………….........................................………..…….... 5 Quick Facts…………………………………………………….......................................………....…. 6 Mysteries of the Solar Nebula ........………...…………………………......................................……7 Solar Studies Past and Present ...................................................................................... 8 NASA's Discovery Program .......................................................................................... 10 Mission Overview….………...…………...…………………………....................................…….... 12 Mid-Air Retrievals........................................................................................................... 14 Sample Return Missions ................................................................................................ 15 Spacecraft ………………………………………………………………......................................…. 26 Science Objectives ………………………………………………………....................................…. 33 The Solar Corona and
    [Show full text]
  • NASA Sets Sights on Asteroid Exploration : Nature News & Comment
    NASA sets sights on asteroid exploration Agency plans to launch a mission to visit the Trojan asteroids in 2021, and one to the metallic asteroid Psyche in 2023. Alexandra Witze 04 January 2017 NASA/JPL-Caltech An artist’s conception of the Psyche spacecraft, which will explore a metallic asteroid. NASA will send two spacecraft to explore asteroids in the hopes of revealing new information about the Solar System’s origins. Psyche will journey to what could be the metallic heart of a failed planet and Lucy will investigate the Trojan asteroids near Jupiter. The missions, announced on 4 January, are part of NASA’s Discovery Program for planetary exploration. They were shortlisted by NASA in September 2015 and have survived a final cut that eliminated two proposed missions to Venus — which has not seen a US planetary mission since Magellan launched in 1989. “What can I say? It’s deeply disappointing,” says Robert Grimm, a planetary scientist at the Southwest Research Institute in Boulder, Colorado, and chairman of a group that analyses Venus issues for NASA. “We want to make sure NASA continues to support high-level Venus activities.” Scheduled to launch in October 2021 and arrive at its first major target in 2027, Lucy will explore six of Jupiter’s Trojan asteroids, which are trapped in orbits ahead of and behind the giant planet. Named after the famous hominid fossil, the spacecraft will investigate the origins of the giant planets by looking at the fragments left over from their formation. “These small bodies really are the fossils of planet formation,” said Lucy principal investigator Hal Levison of the Southwest Research Institute, at a media teleconference.
    [Show full text]
  • Dawn Mission to Vesta and Ceres Symbiosis Between Terrestrial Observations and Robotic Exploration
    Earth Moon Planet (2007) 101:65–91 DOI 10.1007/s11038-007-9151-9 Dawn Mission to Vesta and Ceres Symbiosis between Terrestrial Observations and Robotic Exploration C. T. Russell Æ F. Capaccioni Æ A. Coradini Æ M. C. De Sanctis Æ W. C. Feldman Æ R. Jaumann Æ H. U. Keller Æ T. B. McCord Æ L. A. McFadden Æ S. Mottola Æ C. M. Pieters Æ T. H. Prettyman Æ C. A. Raymond Æ M. V. Sykes Æ D. E. Smith Æ M. T. Zuber Received: 21 August 2007 / Accepted: 22 August 2007 / Published online: 14 September 2007 Ó Springer Science+Business Media B.V. 2007 Abstract The initial exploration of any planetary object requires a careful mission design guided by our knowledge of that object as gained by terrestrial observers. This process is very evident in the development of the Dawn mission to the minor planets 1 Ceres and 4 Vesta. This mission was designed to verify the basaltic nature of Vesta inferred both from its reflectance spectrum and from the composition of the howardite, eucrite and diogenite meteorites believed to have originated on Vesta. Hubble Space Telescope observations have determined Vesta’s size and shape, which, together with masses inferred from gravitational perturbations, have provided estimates of its density. These investigations have enabled the Dawn team to choose the appropriate instrumentation and to design its orbital operations at Vesta. Until recently Ceres has remained more of an enigma. Adaptive-optics and HST observations now have provided data from which we can begin C. T. Russell (&) IGPP & ESS, UCLA, Los Angeles, CA 90095-1567, USA e-mail: [email protected] F.
    [Show full text]
  • SIMBIO-SYS: Scientific Cameras and Spectrometer for the Bepicolombo
    Space Sci Rev (2020) 216:75 https://doi.org/10.1007/s11214-020-00704-8 SIMBIO-SYS: Scientific Cameras and Spectrometer for the BepiColombo Mission G. Cremonese1 · F. Capaccioni2 · M.T. Capria2 · A. Doressoundiram3 · P. Palumbo4 · M. Vincendon5 · M. Massironi6 · S. Debei7 · M. Zusi2 · F. Altieri2 · M. Amoroso8 · G. Aroldi9 · M. Baroni9 · A. Barucci3 · G. Bellucci2 · J. Benkhoff10 · S. Besse11 · C. Bettanini7 · M. Blecka12 · D. Borrelli9 · J.R. Brucato13 · C. Carli2 · V. Carlier5 · P. Cerroni2 · A. Cicchetti2 · L. Colangeli10 · M. Dami9 · V. Da Deppo14 · V. Della Corte2 · M.C. De Sanctis2 · S. Erard3 · F. Esposito 15 · D. Fantinel1 · L. Ferranti16 · F. Ferri7 · I. Ficai Veltroni9 · G. Filacchione2 · E. Flamini17 · G. Forlani18 · S. Fornasier3 · O. Forni19 · M. Fulchignoni20 · V. Galluzzi2 · K. Gwinner21 · W. Ip 22 · L. Jorda23 · Y. Langevin 5 · L. Lara24 · F. Leblanc 25 · C. Leyrat3 · Y. Li 26 · S. Marchi27 · L. Marinangeli28 · F. Marzari29 · E. Mazzotta Epifani30 · M. Mendillo31 · V. Mennella15 · R. Mugnuolo32 · K. Muinonen33,34 · G. Naletto29 · R. Noschese2 · E. Palomba2 · R. Paolinetti9 · D. Perna30 · G. Piccioni2 · R. Politi2 · F. Poulet 5 · R. Ragazzoni1 · C. Re1 · M. Rossi9 · A. Rotundi35 · G. Salemi36 · M. Sgavetti37 · E. Simioni1 · N. Thomas38 · L. Tommasi9 · A. Turella9 · T. Van Hoolst39 · L. Wilson40 · F. Zambon 2 · A. Aboudan7 · O. Barraud3 · N. Bott3 · P. Borin 1 · G. Colombatti7 · M. El Yazidi7 · S. Ferrari7 · J. Flahaut41 · L. Giacomini2 · L. Guzzetta2 · A. Lucchetti1 · E. Martellato4 · M. Pajola1 · A. Slemer14 · G. Tognon7 · D. Turrini2 Received: 12 December 2019 / Accepted: 6 June 2020 / Published online: 17 June 2020 © The Author(s) 2020 Abstract The SIMBIO-SYS (Spectrometer and Imaging for MPO BepiColombo Integrated Observatory SYStem) is a complex instrument suite part of the scientific payload of the Mer- cury Planetary Orbiter for the BepiColombo mission, the last of the cornerstone missions of the European Space Agency (ESA) Horizon + science program.
    [Show full text]
  • Issue 102, May 2005
    3636THTH LLUNARUNAR ANDAND PPLANETARYLANETARY SSCIENCECIENCE CCONFERENCEONFERENCE The 36th Lunar and Planetary Science Conference (LPSC) marked another incredible record-breaking year, with 1460 participants from 24 countries attending the conference held at the South Shore Harbour Resort and Conference Center in League City, Texas, on March 14–18, 2005. This year’s attendance statistics (see inset) reflect a continuing excitement about the future of planetary science. The marked increase in the number of attendees had the potential for presenting a logistical nightmare for conference organizers and staff, but the introduction of overflow seating accommodations for some of the more popular sessions met with tremendous success. LPSC has long been recognized among the international science Attendance from Non-U.S. Countries community as the most important planetary conference in the world, and this year’s meeting substantiated the merit of that Algeria: 1 Australia: 10 reputation. Hundreds of planetary scientists attended both oral and Austria: 3 poster sessions focusing on such diverse topics as the Moon, Mars, Belgium: 1 Mercury, and Venus; outer planets and satellites; meteorites; Canada: 24 comets, asteroids, and other small bodies; impacts; interplanetary Croatia: 1 dust particles and presolar grains; origins of planetary systems; Czech Republic: 2 planetary formation and early evolution; and astrobiology. Sunday Denmark: 5 night’s registration and reception were held at the Center for Finland: 4 France: 53 Advanced Space Studies, which houses the Lunar and Planetary Germany: 48 Institute. Also featured on Sunday night was an open house for the Hungary: 7 display of education and public outreach activities and programs. India: 2 Italy: 9 Highlights of the conference program, established by the program Japan: 75 committee under the guidance of co-chairs Dr.
    [Show full text]
  • Strategic Investment in Laboratory Analysis of Planetary Materials As Ground Truth for Solar System Exploration
    Stra Strategic Investment in Laboratory Analysis of Planetary Materials as Ground Truth for Solar System Exploration Rhonda Stroud (Naval Research Laboratory, [email protected], 202-404-4143) Jessica Barnes (University of Arizona) Larry Nittler (Carnegie Institution for Science) Juliane Gross (Rutgers University) Jemma Davidson (Arizona State University) Catherine Corrigan (Smithsonian Museum of Natural History) Hope Ishii (University of Hawaii) Jamie Elsila Cook (NASA Goddard Space Flight Center) Justin Filiberto (Lunar and Planetary Institute) Samuel Lawrence (NASA Johnson Space Center) Michael Zolensky (NASA Johnson Space Center) Devin Schrader (Arizona State University) Barbara Cohen (NASA Goddard Space Flight Center) Kevin McKeegan (University of California, Los Angeles) and CAPTEM. Introduction: Laboratory analysis of planetary materials provides a wealth of information critical to solving fundamental questions in planetary science that cannot be replicated through remote or in situ analyses alone. Our ground-based collections include samples of the Moon, Mars, the Solar corona, and dozens of asteroids and comets. This vastly exceeds the number of targets of past, and future fly-by, orbiter, or lander missions in the next decade. Similarly, the combined analytical power of the laboratory instrumentation available now vastly exceeds that of the weight and power-constrained spacecraft and rover instrumentation that has already and can be flown this decade. If we are able to put new human footprints on the Moon and Mars within the next few years, as it is now hoped, those astronauts will go propelled in part by the information gleaned by thousands of researchers who have already held the Moon and Mars in their hands.
    [Show full text]
  • THE HUMAN NATURE of ANGELS in GENESIS Kristian Edosomwan
    THE HUMAN NATURE OF ANGELS IN GENESIS Kristian Edosomwan Edosomwan 2 Introduction Genesis often portrays angels in very human ways. The angels described in Genesis 6:1-4 can both copulate and procreate with human women, giving them undeniably human characteristics. In Genesis 18 and 19, angels accept human hospitality and eat human food. And the angel in Genesis 32 uses a human form to wrestle with Jacob on even footing. As these three narratives show, and this paper will argue, angels in Genesis demonstrate an apparently human nature through their interactions with human beings. Genesis 6:1-41 Gen 6:1-4 gives us a window to view how ancient Israelites saw angels. Within the narrative the “sons of God” see the “daughters of men” and choose to marry them and have children (Gen 6:1-2). The “sons of God” are angels while the “daughters of men” are human women. This story has traditionally been looked at as a story of angels transgressing the boundary between heaven and earth and mingling illicitly with human women, such as in 1 Enoch and Jubilees. A common interpretation is that “sons of God” does not refer to angels and instead refers to minor deities under Yahweh. Early Israelite angelology can be seen as an adaptation of the polytheistic system of other Ancient Near Eastern nations.2 The term “sons of gods” was used to signify minor deities on the divine council in Canaanite mythology, but these deities became the angels of Hebrew angelology.3 The angels referenced in Gen 6:1-4 could be deities that the 1 For the sake of my argument I have ignored Gen 6:3, which is a break in the text and seems unrelated to the rest of Gen 6:1-4.
    [Show full text]