“Phobos Events”—Signatures of Solar Wind Interaction with a Gas Torus?
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List of Missions Using SPICE (PDF)
1/7/20 Data Restorations Selected Past Users Current/Pending Users Examples of Possible Future Users Apollo 15, 16 [L] Magellan [L] Cassini Orbiter NASA Discovery Program Mariner 2 [L] Clementine (NRL) Mars Odyssey NASA New Frontiers Program Mariner 9 [L] Mars 96 (RSA) Mars Exploration Rover Lunar IceCube (Moorehead State) Mariner 10 [L] Mars Pathfinder Mars Reconnaissance Orbiter LunaH-Map (Arizona State) Viking Orbiters [L] NEAR Mars Science Laboratory Luna-Glob (RSA) Viking Landers [L] Deep Space 1 Juno Aditya-L1 (ISRO) Pioneer 10/11/12 [L] Galileo MAVEN Examples of Users not Requesting NAIF Help Haley armada [L] Genesis SMAP (Earth Science) GOLD (LASP, UCF) (Earth Science) [L] Phobos 2 [L] (RSA) Deep Impact OSIRIS REx Hera (ESA) Ulysses [L] Huygens Probe (ESA) [L] InSight ExoMars RSP (ESA, RSA) Voyagers [L] Stardust/NExT Mars 2020 Emmirates Mars Mission (UAE via LASP) Lunar Orbiter [L] Mars Global Surveyor Europa Clipper Hayabusa-2 (JAXA) Helios 1,2 [L] Phoenix NISAR (NASA and ISRO) Proba-3 (ESA) EPOXI Psyche Parker Solar Probe GRAIL Lucy EUMETSAT GEO satellites [L] DAWN Lunar Reconnaissance Orbiter MOM (ISRO) Messenger Mars Express (ESA) Chandrayan-2 (ISRO) Phobos Sample Return (RSA) ExoMars 2016 (ESA, RSA) Solar Orbiter (ESA) Venus Express (ESA) Akatsuki (JAXA) STEREO [L] Rosetta (ESA) Korean Pathfinder Lunar Orbiter (KARI) Spitzer Space Telescope [L] [L] = limited use Chandrayaan-1 (ISRO) New Horizons Kepler [L] [S] = special services Hayabusa (JAXA) JUICE (ESA) Hubble Space Telescope [S][L] Kaguya (JAXA) Bepicolombo (ESA, JAXA) James Webb Space Telescope [S][L] LADEE Altius (Belgian earth science satellite) ISO [S] (ESA) Armadillo (CubeSat, by UT at Austin) Last updated: 1/7/20 Smart-1 (ESA) Deep Space Network Spectrum-RG (RSA) NAIF has or had project-supplied funding to support mission operations, consultation for flight team members, and SPICE data archive preparation. -
Science Objectives May Be Summarized As Follows
MAGNETOSPHERE IMAGING INSTRUMENT (MIMI) 9 ON THE CASSINI MISSION TO SATURN/TITAN 2. Scientific Objectives MIMI science objectives may be summarized as follows: Saturn • Determine the global configuration and dynamics of hot plasma in the magneto- sphere of Saturn through energetic neutral particle imaging of ring current, radia- tion belts, and neutral clouds. • Study the sources of plasmas and energetic ions through in situ measurements of energetic ion composition, spectra, charge state, and angular distributions. • Search for, monitor, and analyze magnetospheric substorm-like activity at Saturn. • Determine through the imaging and composition studies the magnetosphere– satellite interactions at Saturn and understand the formation of clouds of neutral hydrogen, nitrogen, and water products. •Investigate the modification of satellite surfaces and atmospheres through plasma and radiation bombardment. • Study Titan’s cometary interaction with Saturn’s magnetosphere (and the solar wind) via high-resolution imaging and in situ ion and electron measurements. • Measure the high energy (Ee > 1 MeV, Ep > 15 MeV) particle component in the inner (L < 5 RS) magnetosphere to assess cosmic ray albedo neutron decay (CRAND) source characteristics. •Investigate the absorption of energetic ions and electrons by the satellites and rings in order to determine particle losses and diffusion processes within the mag- netosphere. • Study magnetosphere–ionosphere coupling through remote sensing of aurora and in situ measurements of precipitating energetic ions and electrons. Jupiter • Study ring current(s), plasma sheet, and neutral clouds in the magnetosphere and magnetotail of Jupiter during Cassini flyby, using global imaging and in situ mea- surements. S. M. KRIMIGIS ET AL. 10 Interplanetary • Determine elemental and isotopic composition of local interstellar medium through measurements of interstellar pickup ions. -
Managing Software Development – the Hidden Risk * Dr
Managing Software Development – The Hidden Risk * Dr. Steve Jolly Sensing & Exploration Systems Lockheed Martin Space Systems Company *Based largely on the work: “Is Software Broken?” by Steve Jolly, NASA ASK Magazine, Spring 2009; and the IEEE Fourth International Conference of System of Systems Engineering as “System of Systems in Space 1 Exploration: Is Software Broken?”, Steve Jolly, Albuquerque, New Mexico June 1, 2009 Brief history of spacecraft development • Example of the Mars Exploration Program – Danger – Real-time embedded systems challenge – Fault protection 2 Robotic Mars Exploration 2011 Mars Exploration Program Search: Search: Search: Determine: Characterize: Determine: Aqueous Subsurface Evidence for water Global Extent Subsurface Bio Potential Minerals Ice Found Found of Habitable Ice of Site 3 Found Environments Found In Work Image Credits: NASA/JPL Mars: Easy to Become Infamous … 1. [Unnamed], USSR, 10/10/60, Mars flyby, did not reach Earth orbit 2. [Unnamed], USSR, 10/14/60, Mars flyby, did not reach Earth orbit 3. [Unnamed], USSR, 10/24/62, Mars flyby, achieved Earth orbit only 4. Mars 1, USSR, 11/1/62, Mars flyby, radio failed 5. [Unnamed], USSR, 11/4/62, Mars flyby, achieved Earth orbit only 6. Mariner 3, U.S., 11/5/64, Mars flyby, shroud failed to jettison 7. Mariner 4, U.S. 11/28/64, first successful Mars flyby 7/14/65 8. Zond 2, USSR, 11/30/64, Mars flyby, passed Mars radio failed, no data 9. Mariner 6, U.S., 2/24/69, Mars flyby 7/31/69, returned 75 photos 10. Mariner 7, U.S., 3/27/69, Mars flyby 8/5/69, returned 126 photos 11. -
Dust Clouds and Plasmoids in Saturn's Magnetosphere
Dust clouds and plasmoids in Saturn’s Magnetosphere as seen with four Cassini instruments Emil Khalisi1 Max-Planck-Institute for Nuclear Physics, Saupfercheckweg 1, D–69117 Heidelberg, Germany Abstract We revisit the evidence for a ”dust cloud” observed by the Cassini space- craft at Saturn in 2006. The data of four instruments are simultaneously compared to interpret the signatures of a coherent swarm of dust that would have remained near the equatorial plane for as long as six weeks. The con- spicuous pattern, as seen in the dust counters of the Cosmic Dust Analyser (CDA), clearly repeats on three consecutive revolutions of the spacecraft. That particular cloud is estimated to about 1.36 Saturnian radii in size, and probably broadening. We also present a reconnection event from the magnetic field data (MAG) that leave behind several plasmoids like those reported from the Voyager flybys in the early 1980s. That magnetic bubbles happened at the dawn side of Saturn’s magnetosphere. At their nascency, the magnetic field showed a switchover of its alignment, disruption of flux tubes and a recovery on a time scale of about 30 days. However, we cannot rule out that different events might have taken place. Empirical evidence is shown at another occasion when a plasmoid was carrying a cloud of tiny dust particles such that a connection between plasmoids and coherent dust clouds is probable. Keywords: Dust clouds, Saturn, Cassini mission, Cosmic Dust Analyser, arXiv:1702.01579v1 [astro-ph.EP] 6 Feb 2017 Magnetosphere URL: DOI: http://dx.doi.org/10.1016/j.asr.2016.12.030 (Emil Khalisi) 1Corresponding author: [email protected] Preprint accepted by Advances in Space Research [JASR13029] 7th February 2017 1. -
Dynamical Meteorology of the Martian Atmosphere
Aspects of Martian Meteorology From SurfaceDynamical Observations Meteorology Including of from the the Martian2012 Mars Atmosphere “Curiosity” Rover Mars Science Laboratory Curiosity The “Curiosity” rover in clean room at JPL Mars Science Laboratory Curiosity Mars Science Laboratory Curiosity Mars Science Laboratory Curiosity Outline • Basics – orbit, topography, atmospheric composition • Basics – dust, dust everywhere • History of Mars planetary missions 1962-today • Satellite measurments of atmospheric temperature • Surface T, P and u,v observations • Pressure record – annual cycle, baroclinic waves • Pressure record – diurnal variations (atmospheric tides) • Mars General Circulation Models (GCMs) • Model simulations of atmospheric tides • I am curious about Curiosity! Mars orbit and annual cycle • Measure time through the year (or position through the o orbit) by Ls (“Areocentric longitude”) (defined so that Ls=0 is NH spring equinox “March 21”) • Aphelion 249,209,300 km • Perihelion 206,669,000 km o • Ls of perihelion 250 - late SH spring Mars orbit and annual cycle • Measure time through the year (or position through the o orbit) by Ls (“Areocentric longitude”) (defined so that Ls=0 is NH spring equinox “March 21”) 2 2 Ra /Rp = 1.42 (vs. 1.07 for Earth) • Aphelion 249,209,300 km • Perihelion 206,669,000 km o • Ls of perihelion 250 - late SH spring CO2 Ice Cap Helas Basin Tharsus Rise Helas Basin Equatorial section through smoothed topography Equatorial section through smoothed topography Zonal wavenumber 2 topography • 1962 Mars -
The Formation of the Martian Moons Rosenblatt P., Hyodo R
The Final Manuscript to Oxford Science Encyclopedia: The formation of the Martian moons Rosenblatt P., Hyodo R., Pignatale F., Trinh A., Charnoz S., Dunseath K.M., Dunseath-Terao M., & Genda H. Summary Almost all the planets of our solar system have moons. Each planetary system has however unique characteristics. The Martian system has not one single big moon like the Earth, not tens of moons of various sizes like for the giant planets, but two small moons: Phobos and Deimos. How did form such a system? This question is still being investigated on the basis of the Earth-based and space-borne observations of the Martian moons and of the more modern theories proposed to account for the formation of other moon systems. The most recent scenario of formation of the Martian moons relies on a giant impact occurring at early Mars history and having also formed the so-called hemispheric crustal dichotomy. This scenario accounts for the current orbits of both moons unlike the scenario of capture of small size asteroids. It also predicts a composition of disk material as a mixture of Mars and impactor materials that is in agreement with remote sensing observations of both moon surfaces, which suggests a composition different from Mars. The composition of the Martian moons is however unclear, given the ambiguity on the interpretation of the remote sensing observations. The study of the formation of the Martian moon system has improved our understanding of moon formation of terrestrial planets: The giant collision scenario can have various outcomes and not only a big moon as for the Earth. -
Hi, This Is Steve Nerlich from Cheap Astronomy and This Is Fobos-Grunt
Hi, this is Steve Nerlich from Cheap Astronomy www.cheapastro.com and this is Fobos-Grunt. Cheap Astronomy originally did a podcast on the Fobos-Grunt mission in 2009, it didn’t make the launch window – so now it’s scheduled for a late 2011, early 2012 launch window. Launch windows to Mars come around once every 26 months. If Fobos-Grunt doesn’t launch this time there will be another 26 months wait until early 2014. This is all because Mars has a 687 day solar orbit, which is close to, though not quite twice the time that of Earth’s solar orbit. This means there’s only one opportunity, when the two planets are in just the right spots to launch a spacecraft, give it a bit of a push up the Sun’s gravity well to Mars’ orbit, just at the right time that Mars is passing by that particular point. The recent history of launches to Mars reads like this: in 2007, the highly successful though now ice-entombed Phoenix mission launched; in 2005 the fabulous Mars Reconnaissance Orbiter launched; in 2003, there was Europe’s Mars Express and its lander Beagle 2, which kind of crashed, and of course Spirit and Opportunity, the Mars rovers; in 2001 Mars Odyssey was launched, a trusty workhorse still in operation today, that amongst other things can relay signals from a Mars rover. If you use the Mars launch window, the travel time to Mars is around 7 to 10 months. Alternatively, you could launch at a different time and perhaps try to pursue Mars around its orbit, in which it moves at 24 kilometres a second. -
India to Pull Ahead of China with Mangalyaan's Success
India is set to join the elite list of members after the US, Russia and Europe to have successfully launched termed successful only after the spacecraft manages to insert itself into the Mars orbit on September 21, INDIA TO PULL a spacecraft to Mars. The attempts made by Japan and China (using a Russian rocket) have failed so far. 2014. China had successfully sent two spacecraft, Chang’e 1 and Chang’e 2, into the lunar orbit and is India is banking on its most-successful PSLV rocket, which had put its first spacecraft, Chandrayaan-1, preparing to send a landing and rover mission, Chang’e 3, to the moon in December 2013. Here is a look AHEAD OF into the lunar orbit in 2008. The same rocket flew Mangalyaan on Tuesday. However, the mission will be at all the missions to Mars: LAUNCH DATE Mar 2 LAUNCH DATE Aug. 4 LAUNCH DATE June 10 COUNTRYEurope COUNTRY US CHINA WITH COUNTRYUS LAUNCH DATE May 30 MISSION GOAL Mars SPACECRAFT SPACECRAFT Rosetta SPACECRAFT Phoenix COUNTRY US orbit LAUNCH DATE Mars Exploration Rover A (Spirit) MISSION GOAL Comet MISSION GOAL Mars MANGALYAAN'S SPACECRAFT COMMENTS Aug 5 MISSION GOAL Rover landing COMMENTS Success landing COMMENTS Mariner-9 (Mariner I) Success COUNTRY Success COMMENTS Success LAUNCH DATE LAUNCH DATE Jul 18 LAUNCH DATE USSR LAUNCH DATE LAUNCH DATE LAUNCH DATE SUCCESS LAUNCH DATE Aug. 12 LAUNCH DATE Feb 25 SPACECRAFT Aug 20 Sep 9 Nov 7 LAUNCH DATE LAUNCH DATE July 7 COUNTRY USSR Dec 4 LAUNCH DATE June 2 COUNTRY US Nov. -
Impact of Io's Volcanic Activity to Environment and Dynamics in the Jovian Magnetosphere : from HISAKI Results
Impact of Io's volcanic activity to environment and dynamics in the Jovian magnetosphere : from HISAKI results F. Tsuchiya(1) , K. Yoshioka(2), T. Kimura(1), G. Murakami(3), A. Yamazaki(3), M. Kagitani(1), C. Tao(4), H. Kita(3), R. Koga(1), F. Suzuki(2), R. Hikida(2), Y. Kasaba(1), H. Misawa(1), and T. Sakanoi(1), I. Yoshikawa(2) (1)Tohoku Univ., (2)Univ. Tokyo, (3)ISAS/JAXA, (4)NICT - Launch : Sep 14, 2013, The Hisaki satellite - Size:1m×1m×4m - Orbit:950km×1150km (LEO) EUV spectrograph (EXCEED): Major specifications - Inclination: 30 deg - Wavelength range: 55-145nm - Orbital period : 106 min - Spectral resolution: 0.4-1.0nm Difficult to observe a moon itself - Spatial coverage ~370 arc-sec But designed to observed plasma - Spatial resolution : 17 arc-sec torus and aurora simultaneously Allowed transition lines of FUV/EUV aurora S,O ions (satellite origin) H2 Lyman & Werner bands Mission periods Aurora & gas torus slit Energy flow from outer to inner part of magnetosphere (Primary) 2013-09 - 2014-11 (Extended 1) 2014-12 - 2017-03 (Extended 2) 2017-04 - 2020-03 Yoshioka et al. 2013, Yoshikawa et al. 2014, Yamazaki et al. 2014 2 Summary of the HISAKI findings • Jupiter 1. Internally driven energy release process & inward transport of the energy Yoshioka et al. 2014, Kimura et al. 2015, Badman et al. 2015, Yoshikawa et al. 2016, 2017, Suzuki et al. 2018 2. Solar wind influence on the magnetosphere (plasma torus, radiation belt, and aurora) Kimura et al. 2016, Tao et al. 2016a, 2016b, Kita et al. -
Open Research Online Oro.Open.Ac.Uk
Open Research Online The Open University’s repository of research publications and other research outputs Mars Phobos and Deimos Survey (M-PADS) – A Martian Moons Orbiter and Phobos Lander Journal Item How to cite: Ball, Andrew J.; Price, Michael E.; Walker, Roger J.; Dando, Glyn C.; Wells, Nigel S. and Zarnecki, John C. (2009). Mars Phobos and Deimos Survey (M-PADS) – A Martian Moons Orbiter and Phobos Lander. Advances in Space Research, 43(1) pp. 120–127. For guidance on citations see FAQs. c 2008 COSPAR. Published by Elsevier Ltd. Version: [not recorded] Link(s) to article on publisher’s website: http://dx.doi.org/doi:10.1016/j.asr.2008.04.007 Copyright and Moral Rights for the articles on this site are retained by the individual authors and/or other copyright owners. For more information on Open Research Online’s data policy on reuse of materials please consult the policies page. oro.open.ac.uk Mars Phobos and Deimos Survey (M-PADS)—A Martian Moons Orbiter and Phobos Lander Andrew J. Balla, Michael E. Priceb, Roger J. Walkerb,†, Glyn C. Dandob, Nigel S. Wellsb, and John C. Zarneckia aPlanetary and Space Sciences Research Institute, Centre for Earth, Planetary, Space & Astronomical Research, The Open University, Walton Hall, Milton Keynes, Buckinghamshire MK7 6AA, UK. Email: [email protected] bSpace Department, QinetiQ, Cody Technology Park, Farnborough, Hampshire GU14 0LX, UK †Now at ESA ESTEC, Noordwijk, Netherlands Abstract We describe a Mars ‘Micro Mission’ for detailed study of the martian satellites Phobos and Deimos. The mission involves two ~330 kg spacecraft equipped with solar electric propulsion to reach Mars orbit. -
China's Mission to Mars S
6 CHINA DAILY | HONG KONG EDITION Friday, July 24, 2020 | 7 CHINA FACTS ABOUT MARS Mars is the fourth planet from the Sun and the Wenchang second-smallest planet in our solar system. HAINAN Lander Mars is one of the four terrestrial planets and is more like Earth than any other planet in the system. TIANWEN 1 The earliest record of the observation of Mars can be traced to ancient Egypt around 2000 BC. The red planet made its first appearances in China’s history around 1300 BC on oracle bone inscriptions. In CHINA’S MISSION TO MARS ancient China, it was named Yinghuo , derived from ancient astronomers’ observations that it moved - like a capricious flame in the night sky. The name Aims to fulfill three scientific objectives orbiting the red includes meanings of war and unrest. It is usually planet for comprehensive observation, landing on the Martian not difficult to see Mars with the naked eye as its Mars surface apparent magnitude is surpassed only by Venus, the surface and sending a rover to roam the landing site. It will compound detector to Earth’s moon and our sun. Mars appears red-orange study high-resolution when seen from Earth because its surface contains spectral signatures of conduct scientific investigations on Mars’ soil, geological lots of iron oxides. Here are some other basic facts surface substances structure, environment, atmosphere and water. about our planetary neighbor: Total surface area: LONG 144,798,500 sq km, about 28 percent of Earth’s MARCH 5 and nearly the same as Earth’s land area LONG JOURNEY Earth-Mars Position of Mars scientific instruments are Equatorial radius: With more than transfer when the carrier The 5-ton spacecraft trajectory is launched mounted on the 3,396 km, about half that of Earth 750 metric tons Length of a solar day on Mars: of propellants, will travel more than orbiter and each Long March 400 million km in the rover 24 hours, 39 minutes, and 35 seconds 5 has a liftoff nearly seven months. -
Energetic Particle Injection Events in the Kronian Magnetosphere: Applications and Properties
Energetic particle injection events in the Kronian magnetosphere: applications and properties Inaugural-Dissertation zur Erlangung des Doktorgrades der Mathematisch-Naturwissenschaftlichen Fakultät der Universität zu Köln vorgelegt von Anna Liane Müller aus Aßlar Köln 2011 Bibliografische Information der Deutschen Bibliothek Die Deutsche Nationalbibliothek verzeichnet diese Publikation in der Deutschen Nationalbibliografie; detaillierte bibliografische Daten sind im Internet über http://dnb.ddb.de abrufbar. 1. Referent: Prof. Dr. Joachim Saur 2. Referent: Prof. Dr. Bülent Tezkan 3. Referent: Dr. Norbert Krupp eingereicht am: 10.12.2010 Tag der mündlichen Prüfung (Disputation): 31.01.2011 ISBN 978-3-942171-44-1 uni-edition GmbH 2011 http://www.uni-edition.de c Anna L. Müller x This work is distributed under a x Creative Commons Attribution 3.0 License Printed in Germany At the touch of love everybody becomes a poet. - Plato Abstract The Kronian magnetosphere is highly dynamical. The inner part between 3 Rs and 13 Rs contains numerous injections of hot plasma with energies up to a few hundred keV. This thesis concentrates on electron measurements of the Magnetospheric Imaging Instrument (MIMI) onboard the Cassini spacecraft. The azimuthal plasma velocity as well as the in- jections of charged particles will be characterized. Due to the magnetic drifts, the injected particles at various energies begin to disperse and leave an imprint in the electron as well as in the ion energy spectrograms of the MIMI instrument. The shape of these profiles strongly depends on the azimuthal velocity distribution of the magnetospheric plasma, the age of the injection events as well as the trajectory of Cassini.