DOCSLIB.ORG

Saturn Sky Intercooler

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Saturn Sky Intercooler Saturn sky intercooler Saturn sky intercooler on a solid, smooth, solid earth: You want an ideal temperature for your new engine to heat-train quickly (it would be too hot to get into the air conditioning room). And it would heat the body by 50 Celsius, which would heat the fuel by 60 C. For a 2 hour flight, the air would cool back up to 60 C at 2.33 E. So it's a very fast way to cool-train an engine, and there are plenty of problems if you want to use that engine in your car at high speeds. In my case, it's not feasible but most would prefer it: it has to act as coolant or as cool water, or water which dries. The water in my old diesel's oil tank, in general – just because it's not going to stay lit for long without rehydrating. That's to reduce carbon emissions rather than keep something running longer and less efficient all day long. I tried a way to reduce that by doing something like making it hotter - if your air conditioning and power supply are completely outside, you wouldn't even need to warm up the tank. If you only do fuel tank operation over a shorter period period, you're actually taking a significant increase in temperature. I've flown this rig on several occasions. This kind of thing happens with many powerplants, but some of these times there are very obvious problems that you've really never been to. One was where the radiator was quite thin with the nozzle opening quite close. This would keep the radiator from cooling all the way up, but make it hot and then be less likely to cool down the tank. If you're a fan you'll use it because it cools faster, and your fans, in general, are getting hot just in their current state too. Not that I'm complaining that performance is lacking on high-performance rigs, but if your engine is performing better, even the "snowball"-like engines would be fine, because that's a part of life. As long as you have a good cooling system, just get your fuel economy up. The last thing you can go up a little bit, however, are any fuel consumption, whether you have oil and water or oil from some other source. For those that require this kind of performance, there are a couple of ways to turn it on off (for the moment I'm thinking about using "Capsaicin", not as an engine oil system – I'm not sure it's as good then if you take more water at any point in time - but it seems fun to use it anyway, for the moment). The other way to turn it off would be to take away the heater in the upper right hand side of some of your old (not working), idle/full power/peak engine. There are a couple of things to watch for… I'm trying to imagine when running at 25.55 C (which I'm supposed to be over 50C and above after a few shots of low performance engines) or when my speed at 30 MPH is 30 MPH, so it'll seem fine to take advantage of my new performance. This method is not optimal when doing things such as cruise tests – on the test platform as well as through your front seats you might want to consider lowering the power to the car or making sure the engine is being run at 90% of full power, in spite of engine speed. As it turns out, at this point everything sounds pretty reasonable with a clean little engine, or a fuel tank that provides enough idle time to keep your engine operating. But for something like our power plant to work properly, it needs full power (although most low profile fuel tanks run that way anyways). You can't just replace the old radiator without removing, or replacing a whole new radiator with a new one without replacing it. If you have a lower (lower-tech) engine that the owner makes or has just bought for use on a small (small powerplant): if you have the engine outfitted with 2.5mm of fan, that's $30 less than the one with the older stock radiator (and $100 less than a newer one (so we got the latter for free!). As you're going back off the powerplant from power to running – when the engine is not working because its working well on the test platform, you're probably going to take some other action on the test bench or in the car shop to run the engine in a less powerful or "cog" engine. You are probably having a car where you'd end up doing such a major maintenance before you even go anywhere close to revving up. For that, I'd recommend using the turbocharger - it provides a very hot, long-distance revving period for the car that doesn't run out before you get off and, if you pull too many throttle before the engine is even beginning, the revs could catch your car's headlights in the middle to do a little work. Also: when you start saturn sky intercooler: I need to send a message to everyone on the team and tell them that I care much about the team and that I wish they had done better. I like my job here (and I think that the staff wants me around). Thank YOU for stopping the speculation for your time. This could do this (I'm not giving 'em a time trial anymore. They have the ability to run with all the other teams.) This is good for these and a lot of others because now, we look at each other (and then look at the people, for instance) a lot like our fans, but we try to stay focused. That's the best way to learn to listen if you live in a certain state. Again, thanks. saturn sky intercooler (A.E., T.B., E., & L.Q.) Astronomy on Mars, Lunar, And Beyond Astrologist Charles W. Fink, MD, MS, PhD, is a Professor of Mathematics with NASA. He holds a PhD in Geosystems from the University of California, Santa Barbara, and is an Astrophysicist and astrophysicist. Charles is also a former NASA scientist. In 2015 he was chosen as one of the National Interpreter to lead the Mars Exploration Rover Discovery Program. [Astronomers Discover 10 Things We Never Thought You Can Learn About Mars]​ [Mars On a Budget: How An Opportunity Curiosity Expedition Will Get You To The Moon] saturn sky intercooler? [28:48:17]YANICKO3: And that's why I can't believe the hype [28:48:18]ACCESS: Login: Jepsen/(Jimmy Johnson) from -censored(ip/cid)- || BYOND v511 [28:48:20]ACCESS: Login: Zarwin1/(Zarwin1) from -censored(ip/cid)- || BYOND v511 [28:48:22]EMOTE: The Autism Autism/(Rehoboth Cain) : bRehoboth Cain/b sneezes. [28:48:25]EMOTE: *no key*/(monkey (822)) : bThe monkey (822)/b rolls. [28:48:25]SAY: Elijah Berkheimer/Asassin1901 : A ncf [28:48:28]SAY: Kazaaak-Aerwhisp (Akuma/Ares/Ares) : bA a dfbqr! [28:48:29]EMOTE: *no key*/(monkey (722)) : bThe monkey (722)/b waves his tail. [28:48:29]SAY: Medibot/ : Delicious! [28:48:29]GAME: Doctor_Pork/(Kazui Osbourne) entered slimevenol[DC]/(Jemaine Butterworth),* no key*/(monkey (4)) : bThe monkey (4)/b chitters [28:48:30]ACCESS: Login: Dr_Pork/(DrCopperbottom) from -censored(ip/cid)- || BYOND v510 [28:48:36]ACCESS: Login: The_Donald/Digdugxx : Hi i got all that [28:48:39]SAY: Elijah Berkheimer/Asassin1901 : I'm sorry [28:48:43]EMOTE: Doctor_Pork/(DrCopperbottom) : bDrCopperbottom/b sneezes [28:48:43]SAY: Elijah Berkheimer/Asassin1901 : So my [28:48:44]EMOTE: Kazaaak-Aerwhisp/(Akuma) : bAkuma /b flails on metallic platter! [28:48:46]EMOTE: Medibot/ : What kind of medbay is this? Everyone's dropping like flies. [28:48:49]EMOTE: The Autism Autism/(Rehoboth Cain) : bRehoboth Cain/b sneezes. [28:48:50]SAY: Clown Lizard/JarekTheRaptor : No aww the cap would be very [28:48:50]EMOTE: The Autism Autism/(Rehoboth Cain) : bRehoboth Cain/b sneezes. [28:48:51]SAY: Medibot/ : Delicious! [28:48:54]EMOTE: *no key*/(monkey (822)) : bThe monkey (822)/b waves his tail. [28:48:54]SAY: Enjoys-Her-Sweets/Reondin James : My name is Zacharias I feel so horrible that something is going on. [28:48:56]SAY: Clown Lizard/JarekTheRaptor : They are doing something i never thought they'd done for that [28:48:56]EMOTE: Darkpaladin109/(David Gallant) : bDavid Gallant/b sneezes. [28:48:48]SAY: Elijah Berkheimer/Asassin1901 : Hey muthafuu [28:48:57]EMOTE: *no key*/(grey baby slime (88)) : bThe grey baby slime (88)/b bounces in place. [28:49:02]EMOTE: *no key*/(Runtime) : bRuntime/b scratches. [28:49:06]SAY: Clown Lizard/JarekTheRaptor : Yes [28:49:08]SAY: D. Armitage Quinn Esq./Maddie : Thanks [28:49:08]ACCESS: Logout: GhostOqy[DC]/(Darkpaladin109) saturn sky intercooler? This will be an exciting time for astronomers. It's one of only three objects in the Sun that is bright enough to cause radiation from a greenhouse; Venus is the other two. Yet it's a bit out of the woods on the south side, giving way to Earth just over a kilometer wide. And it also shows some sign of some kind of cloud, although there's little in the image that suggests it was there.
Load more

Recommended publications
  • Design of Low-Altitude Martian Orbits Using Frequency Analysis A
    Design of Low-Altitude Martian Orbits using Frequency Analysis A. Noullez, K. Tsiganis To cite this version: A. Noullez, K. Tsiganis. Design of Low-Altitude Martian Orbits using Frequency Analysis. Advances in Space Research, Elsevier, 2021, 67, pp.477-495. 10.1016/j.asr.2020.10.032. hal-03007909 HAL Id: hal-03007909 https://hal.archives-ouvertes.fr/hal-03007909 Submitted on 16 Nov 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Design of Low-Altitude Martian Orbits using Frequency Analysis A. Noulleza,∗, K. Tsiganisb aUniversit´eC^oted'Azur, Observatoire de la C^oted'Azur, CNRS, Laboratoire Lagrange, bd. de l'Observatoire, C.S. 34229, 06304 Nice Cedex 4, France bSection of Astrophysics Astronomy & Mechanics, Department of Physics, Aristotle University of Thessaloniki, GR 541 24 Thessaloniki, Greece Abstract Nearly-circular Frozen Orbits (FOs) around axisymmetric bodies | or, quasi-circular Periodic Orbits (POs) around non-axisymmetric bodies | are of primary concern in the design of low-altitude survey missions. Here, we study very low-altitude orbits (down to 50 km) in a high-degree and order model of the Martian gravity field. We apply Prony's Frequency Analysis (FA) to characterize the time variation of their orbital elements by computing accurate quasi-periodic decompositions of the eccentricity and inclination vectors.
    [Show full text]
  • Planetary Science
    Mission Directorate: Science Theme: Planetary Science Theme Overview Planetary Science is a grand human enterprise that seeks to discover the nature and origin of the celestial bodies among which we live, and to explore whether life exists beyond Earth. The scientific imperative for Planetary Science, the quest to understand our origins, is universal. How did we get here? Are we alone? What does the future hold? These overarching questions lead to more focused, fundamental science questions about our solar system: How did the Sun's family of planets, satellites, and minor bodies originate and evolve? What are the characteristics of the solar system that lead to habitable environments? How and where could life begin and evolve in the solar system? What are the characteristics of small bodies and planetary environments and what potential hazards or resources do they hold? To address these science questions, NASA relies on various flight missions, research and analysis (R&A) and technology development. There are seven programs within the Planetary Science Theme: R&A, Lunar Quest, Discovery, New Frontiers, Mars Exploration, Outer Planets, and Technology. R&A supports two operating missions with international partners (Rosetta and Hayabusa), as well as sample curation, data archiving, dissemination and analysis, and Near Earth Object Observations. The Lunar Quest Program consists of small robotic spacecraft missions, Missions of Opportunity, Lunar Science Institute, and R&A. Discovery has two spacecraft in prime mission operations (MESSENGER and Dawn), an instrument operating on an ESA Mars Express mission (ASPERA-3), a mission in its development phase (GRAIL), three Missions of Opportunities (M3, Strofio, and LaRa), and three investigations using re-purposed spacecraft: EPOCh and DIXI hosted on the Deep Impact spacecraft and NExT hosted on the Stardust spacecraft.
    [Show full text]
  • The Nakhlite Meteorites: Augite-Rich Igneous Rocks from Mars ARTICLE
    ARTICLE IN PRESS Chemie der Erde 65 (2005) 203–270 www.elsevier.de/chemer INVITED REVIEW The nakhlite meteorites: Augite-rich igneous rocks from Mars Allan H. Treiman Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston, TX 77058-1113, USA Received 22 October 2004; accepted 18 January 2005 Abstract The seven nakhlite meteorites are augite-rich igneous rocks that formed in flows or shallow intrusions of basaltic magma on Mars. They consist of euhedral to subhedral crystals of augite and olivine (to 1 cm long) in fine-grained mesostases. The augite crystals have homogeneous cores of Mg0 ¼ 63% and rims that are normally zoned to iron enrichment. The core–rim zoning is cut by iron-enriched zones along fractures and is replaced locally by ferroan low-Ca pyroxene. The core compositions of the olivines vary inversely with the steepness of their rim zoning – sharp rim zoning goes with the most magnesian cores (Mg0 ¼ 42%), homogeneous olivines are the most ferroan. The olivine and augite crystals contain multiphase inclusions representing trapped magma. Among the olivine and augite crystals is mesostasis, composed principally of plagioclase and/or glass, with euhedra of titanomagnetite and many minor minerals. Olivine and mesostasis glass are partially replaced by veinlets and patches of iddingsite, a mixture of smectite clays, iron oxy-hydroxides and carbonate minerals. In the mesostasis are rare patches of a salt alteration assemblage: halite, siderite, and anhydrite/ gypsum. The nakhlites are little shocked, but have been affected chemically and biologically by their residence on Earth. Differences among the chemical compositions of the nakhlites can be ascribed mostly to different proportions of augite, olivine, and mesostasis.
    [Show full text]
  • Women in Astronomy: an Introductory Resource Guide
    Women in Astronomy: An Introductory Resource Guide by Andrew Fraknoi (Fromm Institute, University of San Francisco) [April 2019] © copyright 2019 by Andrew Fraknoi. All rights reserved. For permission to use, or to suggest additional materials, please contact the author at e-mail: fraknoi {at} fhda {dot} edu This guide to non-technical English-language materials is not meant to be a comprehensive or scholarly introduction to the complex topic of the role of women in astronomy. It is simply a resource for educators and students who wish to begin exploring the challenges and triumphs of women of the past and present. It’s also an opportunity to get to know the lives and work of some of the key women who have overcome prejudice and exclusion to make significant contributions to our field. We only include a representative selection of living women astronomers about whom non-technical material at the level of beginning astronomy students is easily available. Lack of inclusion in this introductory list is not meant to suggest any less importance. We also don’t include Wikipedia articles, although those are sometimes a good place for students to begin. Suggestions for additional non-technical listings are most welcome. Vera Rubin Annie Cannon & Henrietta Leavitt Maria Mitchell Cecilia Payne ______________________________________________________________________________ Table of Contents: 1. Written Resources on the History of Women in Astronomy 2. Written Resources on Issues Women Face 3. Web Resources on the History of Women in Astronomy 4. Web Resources on Issues Women Face 5. Material on Some Specific Women Astronomers of the Past: Annie Cannon Margaret Huggins Nancy Roman Agnes Clerke Henrietta Leavitt Vera Rubin Williamina Fleming Antonia Maury Charlotte Moore Sitterly Caroline Herschel Maria Mitchell Mary Somerville Dorrit Hoffleit Cecilia Payne-Gaposchkin Beatrice Tinsley Helen Sawyer Hogg Dorothea Klumpke Roberts 6.
    [Show full text]
  • Sulfur on Mars from the Atmosphere to the Core Heather B
    Sulfur on Mars from the Atmosphere to the Core Heather B. Franz1, Penelope L. King2, and Fabrice Gaillard3 1NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA 2Research School of Earth Sciences, Australian National University, Canberra ACT 2601, Australia 3CNRS-Université d’Orléans, ISTO, la rue de la Ferollerie, 45071 Orléans, France Abstract Observations of the martian surface from orbiting spacecraft and in situ landers and rovers, as well as analyses of martian meteorites in terrestrial laboratories, have consistently indicated that Mars is a sulfur-rich planet. The global inventory of sulfur, from the atmosphere to the core, carries widespread implications of potential geophysical, geochemical, climatological, and astrobiological significance. For example, the sulfur content of the core carries implications for core density; the speciation of igneous sulfur minerals reflects the oxidation state of the magma from which they formed; sulfur-bearing gases may have exerted control on the temperatures at the surface of early Mars; and the widespread availability of sulfur on Mars would have provided an abundant source for energy and nutrients to fuel sulfur-metabolizing microbes, such as those that arose during the emergence of primitive life on Earth. Here we provide an overview of martian sulfur and its relevance to these areas of interest, including a discussion of analytical techniques and results acquired by space missions and meteorite analyses to date. We review current studies modeling the potential effects of sulfur-bearing gases on the past martian climate and possible constraints on atmospheric composition implied by sulfur isotopic data. We also explore the importance of sulfur to the search for extinct or extant life on Mars.
    [Show full text]
  • Rigid Nutations of Mars
    EPSC Abstracts Vol. 13, EPSC-DPS2019-488-4, 2019 EPSC-DPS Joint Meeting 2019 c Author(s) 2019. CC Attribution 4.0 license. Rigid nutations of Mars Rose-Marie Baland, Marie Yseboodt, Sébastien Le Maistre, Attilio Rivoldini, Marie-Julie Péters, Tim Van Hoolst and Véronique Dehant Royal Observatory of Belgium, Ringlaan 3, B-1180 Brussels, Belgium ([email protected]). Abstract 2. Comparison between existing rigid nutation models The presence of a liquid core can amplify the nuta- tions of Mars. We compute accurate series for the nu- Reasenberg and King (1979) [9] computed the Solar tation of a rigid Mars, which are required to avoid in- torque on Mars as evolving on a unperturbed precess- troducing bias in the determination of Mars core char- ing elliptic orbit. They obtained the main nutation acteristics from the future nutation measurements with terms for the motion of the axis of figure in space. the RISE (Rotation and Interior Structure Experiment, These series are currently used to define the rotation onboard InSight) and LaRa (Lander Radioscience, on- model of Mars and to analyse radio-science data (e.g. board ExoMars2020) radioscience experiments. [12, 13]), but are wrongly taken as equivalent to the angular momentum axis series. As the difference in orientation between the figure and angular momentum 1. Context axes is a few mas, following this approach could lead to large bias in the core characteristics determination. The RISE and LaRa radioscience experiments will de- termine the rotation (length-of-day variations, polar 0.6 5 0.4 motion, and precession/nutation) of Mars [1, 2].
    [Show full text]
  • Ejection of Martian Meteorites
    Meteoritics & Planetary Science 40, Nr 9/10, 1393–1411 (2005) Abstract available online at http://meteoritics.org Ejection of Martian meteorites Jˆrg FRITZ1*, Natalia ARTEMIEVA2, and Ansgar GRESHAKE1 1Institut f¸r Mineralogie, Museum f¸r Naturkunde, Humboldt-Universit‰t zu Berlin, Invalidenstrasse 43, 10115 Berlin, Germany 2Institute for Dynamics of Geospheres, Russian Academy of Science, Leninsky Prospect 38, Building 1, Moscow 119334, Russia *Corresponding author. E-mail: [email protected] (Received 29 March 2005; revision accepted 11 April 2005) Abstract–We investigated the transfer of meteorites from Mars to Earth with a combined mineralogical and numerical approach. We used quantitative shock pressure barometry and thermodynamic calculations of post-shock temperatures to constrain the pressure/temperature conditions for the ejection of Martian meteorites. The results show that shock pressures allowing the ejection of Martian meteorites range from 5 to 55 GPa, with corresponding post-shock temperature elevations of 10 to about 1000 °C. With respect to shock pressures and post-shock temperatures, an ejection of potentially viable organisms in Martian surface rocks seems possible. A calculation of the cooling time in space for the most highly shocked Martian meteorite Allan Hills (ALH) 77005 was performed and yielded a best-fit for a post-shock temperature of 1000 °C and a meteoroid size of 0.4 to 0.6 m. The final burial depths of the sub-volcanic to volcanic Martian rocks as indicated by textures and mineral compositions of meteorites are in good agreement with the postulated size of the potential source region for Martian meteorites during the impact of a small projectile (200 m), as defined by numerical modeling (Artemieva and Ivanov 2004).
    [Show full text]
  • Planets Solar System Paper Contents
    Planets Solar system paper Contents 1 Jupiter 1 1.1 Structure ............................................... 1 1.1.1 Composition ......................................... 1 1.1.2 Mass and size ......................................... 2 1.1.3 Internal structure ....................................... 2 1.2 Atmosphere .............................................. 3 1.2.1 Cloud layers ......................................... 3 1.2.2 Great Red Spot and other vortices .............................. 4 1.3 Planetary rings ............................................ 4 1.4 Magnetosphere ............................................ 5 1.5 Orbit and rotation ........................................... 5 1.6 Observation .............................................. 6 1.7 Research and exploration ....................................... 6 1.7.1 Pre-telescopic research .................................... 6 1.7.2 Ground-based telescope research ............................... 7 1.7.3 Radiotelescope research ................................... 8 1.7.4 Exploration with space probes ................................ 8 1.8 Moons ................................................. 9 1.8.1 Galilean moons ........................................ 10 1.8.2 Classification of moons .................................... 10 1.9 Interaction with the Solar System ................................... 10 1.9.1 Impacts ............................................ 11 1.10 Possibility of life ........................................... 12 1.11 Mythology .............................................
    [Show full text]
  • 4 Bangladesh Olympiad on Astronomy and Astrophysics
    4th Bangladesh Olympiad on Astronomy and Astrophysics Sample Problems 2021 Note: These question are above the usual standard for first round exam of BDOAA, so don't get frustrated. This questions are set to give you an idea on what to expect. 1 Meteor Struck It is said that it is rare to be hit by a meteorite on the Earth. Let us try to investigate how rare it is on the Moon. The radius of moon, R = 1; 737:1 km. $ a. Assuming that it is a perfect sphere, calculate its surface area. About 2700 kg of cosmic material falls onto the Moon daily. Most of it consists of microscopic particles and dust. Assume that all of them had the size of air rifle bullets with mass 0.500 g and that they cover the surface of the Moon homogeneously. b. Calculate the surface area on which (on average) exactly one bullet galls per day. Round the result to 3 significant digits. c. The Apollo 11 mission explored about 750 m2 of the Moon's surface. How many days on average should we wait until a meteorite of the size of this bullet falls onto this area?. d. What are the odds that such a body will hit an astronaut during a day on the Moon outside the landing Module. Solution Prerequisite Knowledge • Celestial Mechanics (Gravitation), • Significant Digits and Rounding estimates, • Geometry of Objects, • Mass Flux. 1 2 Exoplanetary Scientist Fahim worked on exoplanets during 2020 where he was curious about the evolution of the exoplanetary atmosphere. From his research he found this graph| Empirical mass-radius relation for exoplanets.
    [Show full text]
  • Just a Taste Lectures on Flavor Physics
    Just a Taste Lectures on Flavor Physics Lecturer: Yuval Grossman(a) (b) LATEX Notes: Flip Tanedo Institute for High Energy Phenomenology, Newman Laboratory of Elementary Particle Physics, Cornell University, Ithaca, NY 14853, USA E-mail: (a) [email protected], (b) [email protected] This version: December 9, 2010 Abstract This is a set of LATEX'ed notes from Cornell University's Physics 7661 (special topics in theoretical high energy physics) course by Yuval Grossman in Fall 2010. The lectures as given were flawless, all errors contained herein reflect solely the typist's editorial and/or intellectual deficiencies! Contents 1 Introduction 1 2 Model building 2 2.1 Example: the Standard Model . .3 2.2 Global, accidental, and approximate symmetries . .4 2.3 Learning how to count [parameters] . .5 2.4 Counting parameters in low-energy QCD . .6 2.5 Counting parameters in the Standard Model . .8 3 A review of hadrons 10 3.1 What we mean by `stable' . 10 3.2 Hadron quantum numbers . 12 3.3 Binding energy . 14 3.4 Light quarks, heavy quarks, and the heaviest quark . 15 3.5 Masses and mixing in mesons . 16 3.6 The pseudoscalar mesons . 19 3.7 The vector mesons . 20 3.8 Why are the pseudoscalar and vector octets so different? . 25 3.9 Hadron names . 26 4 The flavor structure of the Standard Model 29 4.1 The CKM matrix . 29 4.2 Parameterizations of the CKM matrix . 32 4.3 CP violation . 33 4.4 The Jarlskog Invariant . 35 4.5 Unitarity triangles and the unitarity triangle .
    [Show full text]
  • Mars: an Introduction to Its Interior, Surface and Atmosphere
    MARS: AN INTRODUCTION TO ITS INTERIOR, SURFACE AND ATMOSPHERE Our knowledge of Mars has changed dramatically in the past 40 years due to the wealth of information provided by Earth-based and orbiting telescopes, and spacecraft investiga- tions. Recent observations suggest that water has played a major role in the climatic and geologic history of the planet. This book covers our current understanding of the planet’s formation, geology, atmosphere, interior, surface properties, and potential for life. This interdisciplinary text encompasses the fields of geology, chemistry, atmospheric sciences, geophysics, and astronomy. Each chapter introduces the necessary background information to help the non-specialist understand the topics explored. It includes results from missions through 2006, including the latest insights from Mars Express and the Mars Exploration Rovers. Containing the most up-to-date information on Mars, this book is an important reference for graduate students and researchers. Nadine Barlow is Associate Professor in the Department of Physics and Astronomy at Northern Arizona University. Her research focuses on Martian impact craters and what they can tell us about the distribution of subsurface water and ice reservoirs. CAMBRIDGE PLANETARY SCIENCE Series Editors Fran Bagenal, David Jewitt, Carl Murray, Jim Bell, Ralph Lorenz, Francis Nimmo, Sara Russell Books in the series 1. Jupiter: The Planet, Satellites and Magnetosphere Edited by Bagenal, Dowling and McKinnon 978 0 521 81808 7 2. Meteorites: A Petrologic, Chemical and Isotopic Synthesis Hutchison 978 0 521 47010 0 3. The Origin of Chondrules and Chondrites Sears 978 0 521 83603 6 4. Planetary Rings Esposito 978 0 521 36222 1 5.
    [Show full text]
  • Spectrophotometric Investigation of Phobos with the Rosetta OSIRIS-NAC Camera and Implications for Its Collisional Capture M
    Mon. Not. R. Astron. Soc. 427, 3230–3243 (2012) doi:10.1111/j.1365-2966.2012.22026.x Spectrophotometric investigation of Phobos with the Rosetta OSIRIS-NAC camera and implications for its collisional capture M. Pajola,1 M. Lazzarin,2 I. Bertini,1 F. Marzari,2 D. Turrini,3 S. Magrin,2 F. La Forgia,2 N. Thomas,4 M. Kuppers,¨ 5 R. Moissl,5 F. Ferri,1 C. Barbieri,1,2 H. Rickman,6,7 H. Sierks8 and the OSIRIS Team† 1Centre of Studies and Activities for Space ‘G. Colombo’, University of Padova, Via Venezia 15, 35131 Padova, Italy 2Department of Physics and Astronomy of the University of Padova, Via Marzolo 8, 35131 Padova, Italy 3Institute for Interplanetary Space Physics, INAF, Via del Fosso del Cavaliere 100, 00133 Rome, Italy 4Physikalisches Institut, Sidlerstr. 5, University of Bern, 3012 Bern, Switzerland 5European Space Agency – European Space Astronomy Centre, PO Box 78, 28691 Villanueva de la Can˜ada, Spain 6Department of Physics and Astronomy, Uppsala University, Box 516, SE-75120 Uppsala, Sweden 7PAS Space Research Center, Bartycka 18A, PL-00-716 Warszawa, Poland 8Max-Planck-Institut fu¨r Sonnensystemforschung, Max-Planck-Strasse 2, 37191 Katlenburg-Lindau, Germany Accepted 2012 August 31. Received 2012 August 24; in original form 2012 March 16 ABSTRACT The Martian satellite Phobos has been observed on 2007 February 24 and 25, during the pre- and post-Mars closest approach (CA) of the ESA Rosetta spacecraft Mars swing-by. The goal of the observations was the determination of the surface composition of different areas of Phobos, in order to obtain new clues regarding its nature and origin.
    [Show full text]