Mars Express Orbiter Radio Science
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Solar-Wind Proton Access Deep Into the Near-Moon Wake M
GEOPHYSICAL RESEARCH LETTERS, VOL. 36, L16103, doi:10.1029/2009GL039444, 2009 Click Here for Full Article Solar-wind proton access deep into the near-Moon wake M. N. Nishino,1 M. Fujimoto,1 K. Maezawa,1 Y. Saito,1 S. Yokota,1 K. Asamura,1 T. Tanaka,1 H. Tsunakawa,2 M. Matsushima,2 F. Takahashi,2 T. Terasawa,2 H. Shibuya,3 and H. Shimizu4 Received 3 June 2009; revised 22 July 2009; accepted 24 July 2009; published 28 August 2009. [1] We study solar wind (SW) entry deep into the near- wake were not known because there were no observation Moon wake using SELENE (KAGUYA) data. It has been data. Recently, a Japanese lunar orbiter SELENE known that SW protons flowing around the Moon access (KAGUYA) performed comprehensive measurements of the central region of the distant lunar wake, while their the plasma and electromagnetic environment around the intrusion deep into the near-Moon wake has never been Moon; in particular, entry of SW protons into the near- expected. We show that SW protons sneak into the deepest Moon wake was found [Nishino et al., 2009]. The SW lunar wake (anti-subsolar region at 100 km altitude), and protons are accelerated by the bipolar electric field around that the entry yields strong asymmetry of the near-Moon the wake boundary and come into the near-Moon wake by wake environment. Particle trajectory calculations their Larmor motion in the direction perpendicular to the demonstrate that these SW protons are once scattered at IMF. This entry mechanism, which we call ‘Type-I entry’, the lunar dayside surface, picked-up by the SW motional lets the SW protons come fairly deep into the wake (solar electric field, and finally sneak into the deepest wake. -
Mission to Jupiter
This book attempts to convey the creativity, Project A History of the Galileo Jupiter: To Mission The Galileo mission to Jupiter explored leadership, and vision that were necessary for the an exciting new frontier, had a major impact mission’s success. It is a book about dedicated people on planetary science, and provided invaluable and their scientific and engineering achievements. lessons for the design of spacecraft. This The Galileo mission faced many significant problems. mission amassed so many scientific firsts and Some of the most brilliant accomplishments and key discoveries that it can truly be called one of “work-arounds” of the Galileo staff occurred the most impressive feats of exploration of the precisely when these challenges arose. Throughout 20th century. In the words of John Casani, the the mission, engineers and scientists found ways to original project manager of the mission, “Galileo keep the spacecraft operational from a distance of was a way of demonstrating . just what U.S. nearly half a billion miles, enabling one of the most technology was capable of doing.” An engineer impressive voyages of scientific discovery. on the Galileo team expressed more personal * * * * * sentiments when she said, “I had never been a Michael Meltzer is an environmental part of something with such great scope . To scientist who has been writing about science know that the whole world was watching and and technology for nearly 30 years. His books hoping with us that this would work. We were and articles have investigated topics that include doing something for all mankind.” designing solar houses, preventing pollution in When Galileo lifted off from Kennedy electroplating shops, catching salmon with sonar and Space Center on 18 October 1989, it began an radar, and developing a sensor for examining Space interplanetary voyage that took it to Venus, to Michael Meltzer Michael Shuttle engines. -
Information Summaries
TIROS 8 12/21/63 Delta-22 TIROS-H (A-53) 17B S National Aeronautics and TIROS 9 1/22/65 Delta-28 TIROS-I (A-54) 17A S Space Administration TIROS Operational 2TIROS 10 7/1/65 Delta-32 OT-1 17B S John F. Kennedy Space Center 2ESSA 1 2/3/66 Delta-36 OT-3 (TOS) 17A S Information Summaries 2 2 ESSA 2 2/28/66 Delta-37 OT-2 (TOS) 17B S 2ESSA 3 10/2/66 2Delta-41 TOS-A 1SLC-2E S PMS 031 (KSC) OSO (Orbiting Solar Observatories) Lunar and Planetary 2ESSA 4 1/26/67 2Delta-45 TOS-B 1SLC-2E S June 1999 OSO 1 3/7/62 Delta-8 OSO-A (S-16) 17A S 2ESSA 5 4/20/67 2Delta-48 TOS-C 1SLC-2E S OSO 2 2/3/65 Delta-29 OSO-B2 (S-17) 17B S Mission Launch Launch Payload Launch 2ESSA 6 11/10/67 2Delta-54 TOS-D 1SLC-2E S OSO 8/25/65 Delta-33 OSO-C 17B U Name Date Vehicle Code Pad Results 2ESSA 7 8/16/68 2Delta-58 TOS-E 1SLC-2E S OSO 3 3/8/67 Delta-46 OSO-E1 17A S 2ESSA 8 12/15/68 2Delta-62 TOS-F 1SLC-2E S OSO 4 10/18/67 Delta-53 OSO-D 17B S PIONEER (Lunar) 2ESSA 9 2/26/69 2Delta-67 TOS-G 17B S OSO 5 1/22/69 Delta-64 OSO-F 17B S Pioneer 1 10/11/58 Thor-Able-1 –– 17A U Major NASA 2 1 OSO 6/PAC 8/9/69 Delta-72 OSO-G/PAC 17A S Pioneer 2 11/8/58 Thor-Able-2 –– 17A U IMPROVED TIROS OPERATIONAL 2 1 OSO 7/TETR 3 9/29/71 Delta-85 OSO-H/TETR-D 17A S Pioneer 3 12/6/58 Juno II AM-11 –– 5 U 3ITOS 1/OSCAR 5 1/23/70 2Delta-76 1TIROS-M/OSCAR 1SLC-2W S 2 OSO 8 6/21/75 Delta-112 OSO-1 17B S Pioneer 4 3/3/59 Juno II AM-14 –– 5 S 3NOAA 1 12/11/70 2Delta-81 ITOS-A 1SLC-2W S Launches Pioneer 11/26/59 Atlas-Able-1 –– 14 U 3ITOS 10/21/71 2Delta-86 ITOS-B 1SLC-2E U OGO (Orbiting Geophysical -
MARS an Overview of the 1985–2006 Mars Orbiter Camera Science
MARS MARS INFORMATICS The International Journal of Mars Science and Exploration Open Access Journals Science An overview of the 1985–2006 Mars Orbiter Camera science investigation Michael C. Malin1, Kenneth S. Edgett1, Bruce A. Cantor1, Michael A. Caplinger1, G. Edward Danielson2, Elsa H. Jensen1, Michael A. Ravine1, Jennifer L. Sandoval1, and Kimberley D. Supulver1 1Malin Space Science Systems, P.O. Box 910148, San Diego, CA, 92191-0148, USA; 2Deceased, 10 December 2005 Citation: Mars 5, 1-60, 2010; doi:10.1555/mars.2010.0001 History: Submitted: August 5, 2009; Reviewed: October 18, 2009; Accepted: November 15, 2009; Published: January 6, 2010 Editor: Jeffrey B. Plescia, Applied Physics Laboratory, Johns Hopkins University Reviewers: Jeffrey B. Plescia, Applied Physics Laboratory, Johns Hopkins University; R. Aileen Yingst, University of Wisconsin Green Bay Open Access: Copyright 2010 Malin Space Science Systems. This is an open-access paper distributed under the terms of a Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Abstract Background: NASA selected the Mars Orbiter Camera (MOC) investigation in 1986 for the Mars Observer mission. The MOC consisted of three elements which shared a common package: a narrow angle camera designed to obtain images with a spatial resolution as high as 1.4 m per pixel from orbit, and two wide angle cameras (one with a red filter, the other blue) for daily global imaging to observe meteorological events, geodesy, and provide context for the narrow angle images. Following the loss of Mars Observer in August 1993, a second MOC was built from flight spare hardware and launched aboard Mars Global Surveyor (MGS) in November 1996. -
The Reference Mission of the NASA Mars Exploration Study Team
NASA Special Publication 6107 Human Exploration of Mars: The Reference Mission of the NASA Mars Exploration Study Team Stephen J. Hoffman, Editor David I. Kaplan, Editor Lyndon B. Johnson Space Center Houston, Texas July 1997 NASA Special Publication 6107 Human Exploration of Mars: The Reference Mission of the NASA Mars Exploration Study Team Stephen J. Hoffman, Editor Science Applications International Corporation Houston, Texas David I. Kaplan, Editor Lyndon B. Johnson Space Center Houston, Texas July 1997 This publication is available from the NASA Center for AeroSpace Information, 800 Elkridge Landing Road, Linthicum Heights, MD 21090-2934 (301) 621-0390. Foreword Mars has long beckoned to humankind interest in this fellow traveler of the solar from its travels high in the night sky. The system, adding impetus for exploration. ancients assumed this rust-red wanderer was Over the past several years studies the god of war and christened it with the have been conducted on various approaches name we still use today. to exploring Earth’s sister planet Mars. Much Early explorers armed with newly has been learned, and each study brings us invented telescopes discovered that this closer to realizing the goal of sending humans planet exhibited seasonal changes in color, to conduct science on the Red Planet and was subjected to dust storms that encircled explore its mysteries. The approach described the globe, and may have even had channels in this publication represents a culmination of that crisscrossed its surface. these efforts but should not be considered the final solution. It is our intent that this Recent explorers, using robotic document serve as a reference from which we surrogates to extend their reach, have can continuously compare and contrast other discovered that Mars is even more complex new innovative approaches to achieve our and fascinating—a planet peppered with long-term goal. -
Variability of Mars' North Polar Water Ice Cap I. Analysis of Mariner 9 and Viking Orbiter Imaging Data
Icarus 144, 382–396 (2000) doi:10.1006/icar.1999.6300, available online at http://www.idealibrary.com on Variability of Mars’ North Polar Water Ice Cap I. Analysis of Mariner 9 and Viking Orbiter Imaging Data Deborah S. Bass Instrumentation and Space Research Division, Southwest Research Institute, P.O. Drawer 28510, San Antonio, Texas 78228-0510 E-mail: [email protected] Kenneth E. Herkenhoff U.S. Geological Survey, 2255 North Gemini Drive, Flagstaff, Arizona 86001 and David A. Paige Department of Earth and Space Sciences, University of California, Los Angeles, 405 Hilgard Avenue, Los Angeles, California 90095-1567 Received May 15, 1998; revised November 17, 1999 1. INTRODUCTION Previous studies interpreted differences in ice coverage between Mariner 9 and Viking Orbiter observations of Mars’ north residual Like Earth, Mars has perennial ice caps and an active wa- polar cap as evidence of interannual variability of ice deposition on ter cycle. The Viking Orbiter determined that the surface of the the cap. However,these investigators did not consider the possibility northern residual cap is water ice (Kieffer et al. 1976, Farmer that there could be significant changes in the ice coverage within et al. 1976). At the south residual polar cap, both Mariner 9 the northern residual cap over the course of the summer season. and Viking Orbiter observed carbon dioxide ice throughout the Our more comprehensive analysis of Mariner 9 and Viking Orbiter summer. Many have related observed atmospheric water vapor imaging data shows that the appearance of the residual cap does not abundances to seasonal exchange between reservoirs such as show large-scale variance on an interannual basis. -
+ New Horizons
Media Contacts NASA Headquarters Policy/Program Management Dwayne Brown New Horizons Nuclear Safety (202) 358-1726 [email protected] The Johns Hopkins University Mission Management Applied Physics Laboratory Spacecraft Operations Michael Buckley (240) 228-7536 or (443) 778-7536 [email protected] Southwest Research Institute Principal Investigator Institution Maria Martinez (210) 522-3305 [email protected] NASA Kennedy Space Center Launch Operations George Diller (321) 867-2468 [email protected] Lockheed Martin Space Systems Launch Vehicle Julie Andrews (321) 853-1567 [email protected] International Launch Services Launch Vehicle Fran Slimmer (571) 633-7462 [email protected] NEW HORIZONS Table of Contents Media Services Information ................................................................................................ 2 Quick Facts .............................................................................................................................. 3 Pluto at a Glance ...................................................................................................................... 5 Why Pluto and the Kuiper Belt? The Science of New Horizons ............................... 7 NASA’s New Frontiers Program ........................................................................................14 The Spacecraft ........................................................................................................................15 Science Payload ...............................................................................................................16 -
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. -
Origin of Fluvial Channels in the Walls of Juventae Chasma: Evidences of Groundwater Sapping? P
47th Lunar and Planetary Science Conference (2016) 1878.pdf ORIGIN OF FLUVIAL CHANNELS IN THE WALLS OF JUVENTAE CHASMA: EVIDENCES OF GROUNDWATER SAPPING? P. Singh1, R. Sarkar1, I. Ganesh1 and A. Porwal1, 1Geology and Mineral Resources Group, CSRE, Indian Institute of Technology, Bombay, India ([email protected]) Introduction: Juventae Chasma is a deep box- Type IV: This type includes channels emanating from canyon located to the north of Valles Marineris. The gullies between the spurs on the chasma wall (Fig. 1d). main geological units of the chasma are chaotic terrain, They are mainly found in the southern wall of the four mounds of interior layered deposits (ILDs) and an chasma. These channels have shorter lengths ranging outflow channel. The presence of the outflow channel from 1-6 km and at places converge into a single chan- indicates that water played an important role in the nel. geological and geomorphological evolution of the Age determination: We estimated the ages of the chasma. In this paper, we report ground-water sapping geological units containing Type 1 and Type III chan- features from the wall of Juventae Chasma. We also delineate and characterize fluvial channels originating nels using crater size-frequency distributions. The re- from the chasma wall. This study was carried out using sults indicate that Type 1 channels are younger than panchromatic data from the CTX and digital terrain 790+- 200 Ma and Type III channels are younger than models from the HRSC onboard the MRO and MEX 620+-300 Ma. Type II and IV were left out because of respectively. -
DSCOVR Magnetometer Observations Adam Szabo, Andriy Koval NASA Goddard Space Flight Center
DSCOVR Magnetometer Observations Adam Szabo, Andriy Koval NASA Goddard Space Flight Center 1 Locations of the Instruments Faraday Cup EPIC Omni Antenna Star Tracker Thruster Modules Digital Sun Sensor Electron Spectrometer +Z +X Magnetometer +Y 2 Goddard Fluxgate Magnetometer The Fluxgate Magnetometer measures the interplanetary vector magnetic field It is located at the tip of a 4.0 m boom to minimize the effect of spacecraft fields Requirement Value Method Performance Magnetometer Range 0.1-100 nT Test 0.004-65,500 nT Accuracy +/- 1 nT Measured +/- 0.2 nT Cadence 1 min Measured 50 vector/sec 3 Pre-flight Calibration • Determined the magnetometer zero levels, scale factors, and magnetometer orthogonalization matrix. • Determined the spacecraft generated magnetic fields – Subsystem level magnetic tests. Reaction wheels, major source of dynamic field, were shielded – Spacecraft unpowered magnetic test in the GSFC 40’ magnetic facility In-Flight Boom Deployment • Nominal deployment on 2/15/15, seen as 4.4 rotations in the magnetometer components Mostly spacecraft Boom deployment Interplanetary magnetic field induced fields 5 Alfven Waves in the Solar Wind • The solar wind contains magnetic field rotations that preserve the magnitude of the field, so called Alfven waves. • Alfven waves are ubiquitous and are possible to identify with automated routines. • Systematic deviations from a constant field magnitude during these waves are an indication of spacecraft induced offsets. • Minimizing the deviations with slowly changing offsets allows in-flight calibrations. 6 In-Flight Magnetometer Calibrations Z Magnetometer Zero Offsets X • X axis Roll and Z axis Slew data is Y consistent with ground calibration estimates X • Independent zero offset determination by rolls, slews and using solar wind Alfvenicity give consistent values Z • Time variation is consistent with yearly orbital change. -
The Terraforming Timeline. A. J. Berliner1 and C. P. Mckay2
Planetary Science Vision 2050 Workshop 2017 (LPI Contrib. No. 1989) 8031.pdf The Terraforming Timeline. A. J. Berliner1 and C. P. McKay2, 1University of California Berkeley, Berkeley, CA 94704, [email protected], 2Space Sciences Division, NASA Ames Research Center, Mountain View, CA 94075. Introduction: Terraforming, the transformation of particularly the winter South Polar Cap, and any CO2 a planet so as to resemble the earth so that it can sup- that is absorbed into the cold ground in the polar re- port widespread life, has been described as a grand gions. Once the warming starts all this releasable CO2 challenge of both space sciences and synthetic biology will go into the atmosphere. Thus, it is important to [1,2]. We propose the following abstract on a Martian know the total before warming starts. Current esti- Terraforming timeline as a guide to shaping planetary mates of the releasable CO2 on Mars today range from science research over the coming century. a little more than the present thin atmosphere to values Terraforming Mars can be divided into two phases. sufficient to create a pressure on Mars equal to the sea The first phase is warming the planet from the present level pressure on Earth. Nitrogen is a fundamental re- average surface temperature of -60ºC to a value close quirement for life and necessary constituent of a to Earth’s average temperature to +15ºC, and re- breathable atmosphere. The recent discovery by the creating a thick CO2 atmosphere [3,4,5,6] This warm- Curiosity Rover of nitrate in the soil on Mars (~0.03% ing phase is relatively easy and quick, and could take by mass) is therefore encouraging for terraforming [7]. -
An Approach to Magnetic Cleanliness for the Psyche Mission M
An Approach to Magnetic Cleanliness for the Psyche Mission M. de Soria-Santacruz J. Ream K. Ascrizzi ([email protected]), ([email protected]), ([email protected]) M. Soriano R. Oran University of Michigan Ann Arbor ([email protected]), ([email protected]), 500 S State St O. Quintero B. P. Weiss Ann Arbor, MI 48109 ([email protected]), ([email protected]) F. Wong Department of Earth, Atmospheric, ([email protected]), and Planetary Sciences S. Hart Massachusetts Institute of Technology ([email protected]), 77 Massachusetts Avenue M. Kokorowski Cambridge, MA 02139 ([email protected]) B. Bone ([email protected]), B. Solish ([email protected]), D. Trofimov ([email protected]), E. Bradford ([email protected]), C. Raymond ([email protected]), P. Narvaez ([email protected]) Jet Propulsion Laboratory, California Institute of Technology 4800 Oak Grove Drive Pasadena, CA 91109 C. Keys C. Russell L. Elkins-Tanton ([email protected]), ([email protected]), ([email protected]) P. Lord University of California Los Angeles Arizona State University ([email protected]) 405 Hilgard Avenue PO Box 871404 Maxar Technologies Inc. Los Angeles, CA 90095 Tempe, AZ 85287 3825 Fabian Avenue Palo Alto, CA 94303 Abstract— Psyche is a Discovery mission that will visit the fields. Limiting and characterizing spacecraft-generated asteroid (16) Psyche to determine if it is the metallic core of a magnetic fields is therefore essential to the mission. This is the once larger differentiated body or otherwise was formed from objective of the Psyche’s magnetics control program described accretion of unmelted metal-rich material.