Alactic Observer Gjohn J
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
VI FORSKER PÅ MARS Kort Om Aktiviteten I Mange Tiår Har Mars Vært Et Yndet Objekt for Forskere Verden Over
VI FORSKER PÅ MARS Kort om aktiviteten I mange tiår har Mars vært et yndet objekt for forskere verden over. Men hvorfor det? Hva er det med den røde planeten som er så interessant? Her forsøker vi å gi en oversikt over hvorfor vi er så opptatt av Mars. Hva har vi oppdaget, og hva er det vi tenker å gjøre? Det finnes en planet i solsystemet vårt som bare er bebodd av roboter -MARS- Læringsmål Elevene skal kunne - gi eksempler på dagsaktuell forskning og drøfte hvordan ny kunnskap genereres gjennom samarbeid og kritisk tilnærming til eksisterende kunnskap - utforske, forstå og lage teknologiske systemer som består av en sender og en mottaker - gjøre rede for energibevaring og energikvalitet og utforske ulike måter å omdanne, transportere og lagre energi på VI FORSKER PÅ MARS side 1 Innhold Kort om aktiviteten ................................................................................................................................ 1 Læringsmål ................................................................................................................................................ 1 Mars gjennom historien ...................................................................................................................... 3 Romkappløp mot Mars ................................................................................................................... 3 2000-tallet gir rovere i fleng ....................................................................................................... 4 Hva nå? ...................................................................................................................................................... -
Endeavour Set to Leave International Space Station Today 24 March 2008
Endeavour Set to Leave International Space Station Today 24 March 2008 who replaced European Space Agency astronaut Léopold Eyharts on the station. Eyharts is returning to Earth aboard Endeavour. The astronauts also performed five spacewalks while on the station. Endeavour is scheduled to land at Kennedy Space Center, Fla., Wednesday. Source: NASA STS-123 Mission Specialist Léopold Eyharts, pictured in the foreground, and Pilot Gregory H. Johnson work at the robotics station in the International Space Station's U.S. laboratory, Destiny. Credit: NASA The crew of space shuttle Endeavour is slated to leave the International Space Station today. The STS-123 and Expedition 16 crews will bid one another farewell, and the hatches between the two spacecraft will close at 5:13 p.m. EDT. Endeavour is scheduled to undock from the International Space Station at 7:56 p.m., ending its 12-day stay at the orbital outpost. STS-123 arrived at the station March 12, delivering the Japanese Logistics Module - Pressurized Section, the first pressurized component of the Japan Aerospace Exploration Agency’s Kibo laboratory, to the station. The crew of Endeavour also delivered the final element of the station’s Mobile Servicing System, the Canadian-built Dextre, also known as the Special Purpose Dextrous Manipulator. In addition, the STS-123 astronauts delivered Expedition 16 Flight Engineer Garrett Reisman, 1 / 2 APA citation: Endeavour Set to Leave International Space Station Today (2008, March 24) retrieved 24 September 2021 from https://phys.org/news/2008-03-endeavour-international-space-station-today.html This document is subject to copyright. -
Generate Viewsheds of Mastcam Images from the Curiosity Rover, Using Arcgis® and Public Datasets
TECHNICAL Coupling Mars Ground and Orbital Views: Generate REPORTS: METHODS Viewsheds of Mastcam Images From the Curiosity 10.1029/2020EA001247 Rover, Using ArcGIS® and Public Datasets Key Points: 1 2 1 3 4 • Mastcam images from the Curiosity M. Nachon , S. Borges , R. C. Ewing , F. Rivera‐Hernández , N. Stein , and rover are available online but lack a J. K. Van Beek5 public method to be placed back in the Mars orbital context 1Department of Geology and Geophysics, Texas A&M University, College Station, TX, USA, 2Department of Astronomy • This procedure allows users to and Planetary Sciences—College of Engineering, Forestry, and Natural Sciences, Northern Arizona University, Flagstaff, generate Mastcam image viewsheds: 3 4 locate in a map view the Mars AZ, USA, Department of Earth Sciences, Dartmouth College, Hanover, NH, USA, Division of Geological and Planetary 5 terrains visible in Mastcam images Sciences, California Institute of Technology, Pasadena, CA, USA, Malin Space Science Systems, San Diego, CA, USA • This procedure uses ArcGIS® and publicly available Mars datasets Abstract The Mastcam (Mast Camera) instrument onboard the NASA Curiosity rover provides an Supporting Information: exclusive view of Mars: High‐resolution color images from Mastcam allow users to study Gale crater's • Dataset S1 geologic terrains along Curiosity's path. These ground observations complement the spatially broader • Dataset S2 • Dataset S3 views of Gale crater provided by spacecrafts from orbit. However, for a given Mastcam image, it can be • Table S1 challenging to locate the corresponding terrains on the orbital view. No method for locating Mastcam images • Table S2 onto orbital images had been made publicly available. -
No. 40. the System of Lunar Craters, Quadrant Ii Alice P
NO. 40. THE SYSTEM OF LUNAR CRATERS, QUADRANT II by D. W. G. ARTHUR, ALICE P. AGNIERAY, RUTH A. HORVATH ,tl l C.A. WOOD AND C. R. CHAPMAN \_9 (_ /_) March 14, 1964 ABSTRACT The designation, diameter, position, central-peak information, and state of completeness arc listed for each discernible crater in the second lunar quadrant with a diameter exceeding 3.5 km. The catalog contains more than 2,000 items and is illustrated by a map in 11 sections. his Communication is the second part of The However, since we also have suppressed many Greek System of Lunar Craters, which is a catalog in letters used by these authorities, there was need for four parts of all craters recognizable with reasonable some care in the incorporation of new letters to certainty on photographs and having diameters avoid confusion. Accordingly, the Greek letters greater than 3.5 kilometers. Thus it is a continua- added by us are always different from those that tion of Comm. LPL No. 30 of September 1963. The have been suppressed. Observers who wish may use format is the same except for some minor changes the omitted symbols of Blagg and Miiller without to improve clarity and legibility. The information in fear of ambiguity. the text of Comm. LPL No. 30 therefore applies to The photographic coverage of the second quad- this Communication also. rant is by no means uniform in quality, and certain Some of the minor changes mentioned above phases are not well represented. Thus for small cra- have been introduced because of the particular ters in certain longitudes there are no good determi- nature of the second lunar quadrant, most of which nations of the diameters, and our values are little is covered by the dark areas Mare Imbrium and better than rough estimates. -
Special Catalogue Milestones of Lunar Mapping and Photography Four Centuries of Selenography on the Occasion of the 50Th Anniversary of Apollo 11 Moon Landing
Special Catalogue Milestones of Lunar Mapping and Photography Four Centuries of Selenography On the occasion of the 50th anniversary of Apollo 11 moon landing Please note: A specific item in this catalogue may be sold or is on hold if the provided link to our online inventory (by clicking on the blue-highlighted author name) doesn't work! Milestones of Science Books phone +49 (0) 177 – 2 41 0006 www.milestone-books.de [email protected] Member of ILAB and VDA Catalogue 07-2019 Copyright © 2019 Milestones of Science Books. All rights reserved Page 2 of 71 Authors in Chronological Order Author Year No. Author Year No. BIRT, William 1869 7 SCHEINER, Christoph 1614 72 PROCTOR, Richard 1873 66 WILKINS, John 1640 87 NASMYTH, James 1874 58, 59, 60, 61 SCHYRLEUS DE RHEITA, Anton 1645 77 NEISON, Edmund 1876 62, 63 HEVELIUS, Johannes 1647 29 LOHRMANN, Wilhelm 1878 42, 43, 44 RICCIOLI, Giambattista 1651 67 SCHMIDT, Johann 1878 75 GALILEI, Galileo 1653 22 WEINEK, Ladislaus 1885 84 KIRCHER, Athanasius 1660 31 PRINZ, Wilhelm 1894 65 CHERUBIN D'ORLEANS, Capuchin 1671 8 ELGER, Thomas Gwyn 1895 15 EIMMART, Georg Christoph 1696 14 FAUTH, Philipp 1895 17 KEILL, John 1718 30 KRIEGER, Johann 1898 33 BIANCHINI, Francesco 1728 6 LOEWY, Maurice 1899 39, 40 DOPPELMAYR, Johann Gabriel 1730 11 FRANZ, Julius Heinrich 1901 21 MAUPERTUIS, Pierre Louis 1741 50 PICKERING, William 1904 64 WOLFF, Christian von 1747 88 FAUTH, Philipp 1907 18 CLAIRAUT, Alexis-Claude 1765 9 GOODACRE, Walter 1910 23 MAYER, Johann Tobias 1770 51 KRIEGER, Johann 1912 34 SAVOY, Gaspare 1770 71 LE MORVAN, Charles 1914 37 EULER, Leonhard 1772 16 WEGENER, Alfred 1921 83 MAYER, Johann Tobias 1775 52 GOODACRE, Walter 1931 24 SCHRÖTER, Johann Hieronymus 1791 76 FAUTH, Philipp 1932 19 GRUITHUISEN, Franz von Paula 1825 25 WILKINS, Hugh Percy 1937 86 LOHRMANN, Wilhelm Gotthelf 1824 41 USSR ACADEMY 1959 1 BEER, Wilhelm 1834 4 ARTHUR, David 1960 3 BEER, Wilhelm 1837 5 HACKMAN, Robert 1960 27 MÄDLER, Johann Heinrich 1837 49 KUIPER Gerard P. -
Thickness of the Martian Crust: Improved Constraints from Geoid-To-Topography Ratios Mark A
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 109, E01009, doi:10.1029/2003JE002153, 2004 Thickness of the Martian crust: Improved constraints from geoid-to-topography ratios Mark A. Wieczorek De´partement de Ge´ophysique Spatiale et Plane´taire, Institut de Physique du Globe de Paris, Saint-Maur, France Maria T. Zuber Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, Massachusetts, USA Received 10 July 2003; revised 1 September 2003; accepted 24 November 2003; published 24 January 2004. [1] The average crustal thickness of the southern highlands of Mars was investigated by calculating geoid-to-topography ratios (GTRs) and interpreting these in terms of an Airy compensation model appropriate for a spherical planet. We show that (1) if GTRs were interpreted in terms of a Cartesian model, the recovered crustal thickness would be underestimated by a few tens of kilometers, and (2) the global geoid and topography signals associated with the loading and flexure of the Tharsis province must be removed before undertaking such a spatial analysis. Assuming a conservative range of crustal densities (2700–3100 kg mÀ3), we constrain the average thickness of the Martian crust to lie between 33 and 81 km (or 57 ± 24 km). When combined with complementary estimates based on crustal thickness modeling, gravity/topography admittance modeling, viscous relaxation considerations, and geochemical mass balance modeling, we find that a crustal thickness between 38 and 62 km (or 50 ± 12 km) is consistent with all studies. Isotopic investigations based on Hf-W and Sm-Nd systematics suggest that Mars underwent a major silicate differentiation event early in its evolution (within the first 30 Ma) that gave rise to an ‘‘enriched’’ crust that has since remained isotopically isolated from the ‘‘depleted’’ mantle. -
Mariner to Mercury, Venus and Mars
NASA Facts National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology Pasadena, CA 91109 Mariner to Mercury, Venus and Mars Between 1962 and late 1973, NASA’s Jet carry a host of scientific instruments. Some of the Propulsion Laboratory designed and built 10 space- instruments, such as cameras, would need to be point- craft named Mariner to explore the inner solar system ed at the target body it was studying. Other instru- -- visiting the planets Venus, Mars and Mercury for ments were non-directional and studied phenomena the first time, and returning to Venus and Mars for such as magnetic fields and charged particles. JPL additional close observations. The final mission in the engineers proposed to make the Mariners “three-axis- series, Mariner 10, flew past Venus before going on to stabilized,” meaning that unlike other space probes encounter Mercury, after which it returned to Mercury they would not spin. for a total of three flybys. The next-to-last, Mariner Each of the Mariner projects was designed to have 9, became the first ever to orbit another planet when two spacecraft launched on separate rockets, in case it rached Mars for about a year of mapping and mea- of difficulties with the nearly untried launch vehicles. surement. Mariner 1, Mariner 3, and Mariner 8 were in fact lost The Mariners were all relatively small robotic during launch, but their backups were successful. No explorers, each launched on an Atlas rocket with Mariners were lost in later flight to their destination either an Agena or Centaur upper-stage booster, and planets or before completing their scientific missions. -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
Weiler2006.Pdf (5.444Mb)
Study of the Gas and Dust Activity of Recent Comets vorgelegt von Diplom-Physiker Michael Weiler aus Andernach Von der Fakult¨at II - Mathematik und Naturwissenschaften der Technischen Universit¨at Berlin zur Erlangung des akademischen Grades Doktor der Naturwissenschaften Dr. rer. nat. genehmigte Dissertation Promotionsausschuss: Vorsitzender: Prof. Dr.-Ing. Hans Joachim Eichler Berichter/Gutachter: Prof. Dr. rer. nat. Heike Rauer Berichter/Gutachter: Prof. Dr. rer. nat. Erwin Sedlmayr Tag der wissenschaftlichen Aussprache: 18.12.2006 Berlin 2007 D 83 1 Contents 0 Zusammenfassung 6 1 Introduction 7 1.1 Historical Development of Comet Science in Brief . ...... 7 1.2 Short Overview of the Present Picture of Comets . ..... 7 1.2.1 TheCometaryNucleus ........................ 8 1.2.2 TheDustComaandTail........................ 9 1.2.3 TheNeutralComa ........................... 10 1.2.4 ThePlasmaEnvironment . 10 1.2.5 Dynamical Classification of Comets . 11 1.2.6 CometarySourceRegions . 12 1.2.7 Classification according to the Coma Composition . 13 1.2.8 Correlations between Taxonomy, Source Regions, and Formation RegionsofComets ........................... 14 1.3 The Formation Chemistry of C2 and C3 ................... 15 1.4 Goalsofthiswork................................ 16 2 Optical Comet Observations 19 2.1 OpticalEmissionsfromComets . 19 2.1.1 GasEmissions.............................. 19 2.1.2 Light Scattering by Dust Particles . 20 2.1.3 OpticalObservationsoftheNucleus. 21 2.2 Overview of Observational Techniques . 22 2.2.1 Long-SlitSpectroscopy . 22 2.2.2 Imaging ................................. 23 2.3 ObservationalDatasetofthisWork . 23 2.3.1 Observations of Comet 67P/Churyumov-Gerasimenko . 24 2.3.2 Observations of Comet 9P/Tempel 1 . 27 2.3.3 Observations of Comets C/2002 T7 LINEAR and C/2001 Q4 NEAT 28 2.3.4 Reference Observations of Comet C/1995 O1 Hale-Bopp . -
Space Shuttle Endeavour Will Rocket Into History
Space Shuttle Endeavour Will Rocket Into History 4/29/2011 http://www.pbs.org/newshour/extra/features/science/jan-june11/endeavour_04-29.html Estimated Time: One 45-minute class period with possible extension Student Worksheet (reading comprehension and discussion questions without answers) PROCEDURE 1. WARM UP Use initiating questions to introduce the topic and find out how much your students know. 2. MAIN ACTIVITY Have students read NewsHour Extra's feature story and answer the reading comprehension and discussion questions on the student handout. 3. DISCUSSION Use discussion questions to encourage students to think about how the issues outlined in the story affect their lives and express and debate different opinions INITIATING QUESTIONS 1. How do astronauts reach space? 2. How does a space shuttle work? How is it different from prior space vehicles? 3. Which U.S. government agency oversees space travel? READING COMPREHENSION QUESTIONS 1. Who will pilot the Endeavour on this mission and how is he related to a recent news event? The shuttle will be piloted by astronaut Mark Kelly, whose wife, Congresswoman Gabrielle Giffords (D-Ariz.), was shot in the head in January by a lone gunman at a community event. Giffords, who is recovering from her brain injury at a Houston rehabilitation center, will be in attendance at the launch. 2. What is the Endeavour transporting into space? Endeavour’s final mission will transport three tiny satellites to be mounted on the International Space Station for a brief time to see how they hold up in the harsh conditions of space. Endeavor will also bring a historic artifact into space: a three-inch wooden ball called a “parrel” that was used by sailors to raise sails up masts. -
Molds Aboard the International Space Station
Mold Species in Dust from the International Space Station Identified and Quantified by Mold Specific Quantitative PCR Stephen J. Vesper a*, Wing Wongb C. Mike Kuoc, Duane L. Piersond a National Exposure Research Laboratory (NERL), United States (US) Environmental Protection Agency, Cincinnati, OH; b Enterprise Advisory Services Inc., Houston, TX c WYLE Laboratories Inc., Houston, TX d Johnson Space Center, National Aeronautics and Space Administration, Houston, TX *Corresponding Author: Stephen Vesper, US EPA, 26 West M.L. King Ave., M.L. 314, Cincinnati, Ohio 45268. Phone: 513-569-7367; email: [email protected] Abstract Dust was collected over a period of several weeks in 2007 from HEPA filters in the U.S. Laboratory Module of the International Space Station (ISS). The dust was returned on the Space Shuttle Atlantis, mixed, sieved, and the DNA was extracted. Using a DNA- based method called mold specific quantitative PCR (MSQPCR), 39 molds were measured in the dust. Potential opportunistic pathogens Aspergillus flavus and A. niger and potential moderate toxin producers Penicillium chrysogenum and P. brevicompactum were noteworthy. No cells of the potential opportunistic pathogens A. fumigatus, A. terreus, Fusarium solani or Candida albicans were detected. Keywords: International Space Station, mold specific quantitative PCR, Aspergillus 1 1. Introduction Since human space exploration began, microbes have traveled with us and are ubiquitous throughout the spacecraft. Previous studies have demonstrated that bacteria, including potential pathogens, were commonly isolated in the air, water, and on surfaces aboard the Mir Space Station [12] and the International Space Station (ISS) [1,6]. Biofilms were found in the water distribution lines on the Space Shuttle Discovery [5]. -
Orbiter Processing Facility
National Aeronautics and Space Administration Space Shuttle: Orbiter Processing From Landing To Launch he work of preparing a space shuttle for the same facilities. Inside is a description of an flight takes place primarily at the Launch orbiter processing flow; in this case, Discovery. Complex 39 Area. TThe process actually begins at the end of each acts Shuttle Landing Facility flight, with a landing at the center or, after landing At the end of its mission, the Space Shuttle f at an alternate site, the return of the orbiter atop a Discovery lands at the Shuttle Landing Facility on shuttle carrier aircraft. Kennedy’s Shuttle Landing one of two runway headings – Runway 15 extends Facility is the primary landing site. from the northwest to the southeast, and Runway There are now three orbiters in the shuttle 33 extends from the southeast to the northwest fleet: Discovery, Atlantis and Endeavour. Chal- – based on wind currents. lenger was destroyed in an accident in January After touchdown and wheelstop, the orbiter 1986. Columbia was lost during approach to land- convoy is deployed to the runway. The convoy ing in February 2003. consists of about 25 specially designed vehicles or Each orbiter is processed independently using units and a team of about 150 trained personnel, NASA some of whom assist the crew in disembarking from the orbiter. the orbiter and a “white room” is mated to the orbiter hatch. The The others quickly begin the processes necessary to “safe” the hatch is opened and a physician performs a brief preliminary orbiter and prepare it for towing to the Orbiter Processing Fa- medical examination of the crew members before they leave the cility.