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Calculating the Potato Radius of Asteroids Using the Height of Mt. Everest
Calculating the Potato Radius of Asteroids using the Height of Mt. Everest M. E. Caplan∗ Center for the Exploration of Energy and Matter, Indiana University, Bloomington, IN 47408 (Dated: November 16, 2015) Abstract At approximate radii of 200-300 km, asteroids transition from oblong `potato' shapes to spheres. This limit is known as the Potato Radius, and has been proposed as a classification for separating asteroids from dwarf planets. The Potato Radius can be calculated from first principles based on the elastic properties and gravity of the asteroid. Similarly, the tallest mountain that a planet can support is also known to be based on the elastic properties and gravity. In this work, a simple novel method of calculating the Potato Radius is presented using what is known about the maximum height of mountains and Newtonian gravity for a spherical body. This method does not assume any knowledge beyond high school level mechanics, and may be appropriate for students interested in applications of physics to astronomy. arXiv:1511.04297v1 [physics.ed-ph] 7 Nov 2015 1 I. INTRODUCTION Spacecraft are currently exploring asteroids and dwarf planets, such as the Near Earth Asteroid Rendezvous mission (NEAR) landing on Eros,1 the Dawn mission orbiting Ceres and Vesta,2 and the New Horizons flyby of Pluto and Charon.3 Additionally, the Mars Re- connaissance Orbiter (MRO) has observed the Martian moons Phobos and Deimos.4 These missions observe a remarkable variety of shapes for these bodies, shown in Fig. 1. Smaller asteroids have irregular shapes while dwarf planets (large asteroids) are nearly spherical. -
Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur
Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur To cite this version: Alex Soumbatov-Gur. Phobos, Deimos: Formation and Evolution. [Research Report] Karpov institute of physical chemistry. 2019. hal-02147461 HAL Id: hal-02147461 https://hal.archives-ouvertes.fr/hal-02147461 Submitted on 4 Jun 2019 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. Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur The moons are confirmed to be ejected parts of Mars’ crust. After explosive throwing out as cone-like rocks they plastically evolved with density decays and materials transformations. Their expansion evolutions were accompanied by global ruptures and small scale rock ejections with concurrent crater formations. The scenario reconciles orbital and physical parameters of the moons. It coherently explains dozens of their properties including spectra, appearances, size differences, crater locations, fracture symmetries, orbits, evolution trends, geologic activity, Phobos’ grooves, mechanism of their origin, etc. The ejective approach is also discussed in the context of observational data on near-Earth asteroids, main belt asteroids Steins, Vesta, and Mars. The approach incorporates known fission mechanism of formation of miniature asteroids, logically accounts for its outliers, and naturally explains formations of small celestial bodies of various sizes. -
The Moon (~1700Km) an Asteroid (~50Km)
1) inventory Solar System 2) spin/orbit/shape 3) heated by the Sun overview 4) how do we fnd out Inventory 1 star (99.9% of M) 8 planets (99.9% of L) - Terrestrial: Mercury Venus Earth Mars - Giant: Jupiter Saturn Uranus Neptune Lots of small bodies incl. dwarf planets Ceres Pluto Eris Maybe a 9th planet? Moons of Jupiter Inventory (cont'd) 4 Galilean satellites (Ganymede, Callisto, Io & Europa), 3 Many moons & rings ~10 km (close to Jupiter, likely primordial) Mercury: 0 Venus: 0 Earth: 1 (1700km) Mars: 2 (~10km) Jupiter: 69 + rings Saturn: 62 + rings Uranus: 27 + rings Neptune: 14 + rings 2001J3: 4km Even among dwarf planets, asteroids, Kuiper belt objects, and comets. E.g., Pluto: 5 Eris: 1 Moons of Mars: Deimos & Phobos, ~10km Atmosphere no thick thick little thick Inventory (cont'd) ~105 known small objects in the - Asteroid belt (Ceres ~300 km) - Kuiper belt (Eris, Pluto, Sedna, Quaoar, ~1000 km) Estimated: ~1012 comets in the - Oort cloud (~ 104 AU) Associated: - zodiacal dust (fre-works on the sky: comets & meteorites) What are planets? IAU (for solar system): Orbits Sun, massive enough to be round and to have cleared its neighbourhood. More general: 6 1) no nuclear fusion (not even deuterium): Tc < 10 K 2) pressure provided by electron degeneracy and/or Coulomb force (l ~ h/p ~ d) (d ~ atomic radius) 3) can be solid or gaseous (with solid cores) --- similar density Mass & Mean r M [g/cm3] R~M J Jupiter 1.0 1.33 R R~M1/3 Saturn 0.3 0.77 R~M-1/3 Neptune 0.05 1.67 Uranus 0.04 1.24 Earth 0.003 5.52 Venus 0.002 5.25 planets brown dwarfs stars Mars 0.0003 3.93 Mercury 0.0002 5.43 3 MJ 13 MJ 80 MJ M Orbits inclination: largely coplanar (history) direction: all the same eccentricity: a few percent (except for Mercury) Titus-Bode (ftting) law (1766) planetary orbits appear to (almost) satisfy a single relation 'Predict' the existence of the asteroid belt (1801: Ceres discovered) coincidence or something deeper? other systems? Computer simulations indicate that planets are as maximally packed as allowed by stability. -
A New Model of the Crustal Magnetic Field of Mars Using MGS and MAVEN
RESEARCH ARTICLE A New Model of the Crustal Magnetic Field of Mars Using 10.1029/2018JE005854 MGS and MAVEN Key Points: 1 1 2 3 • MGS and MAVEN magnetic field Benoit Langlais , Erwan Thébault , Aymeric Houliez , Michael E. Purucker , 4 measurements are combined into a and Robert J. Lillis high-resolution magnetic field model • The new model extends up to SH 1Laboratoire de Planétologie et Géodynamique, Université de Nantes, Université d'Angers, CNRS, UMR 6112, Nantes, degree 134, corresponding to 160-km France, 2Observatoire Royal de Belgique, Uccle, Belgium, 3Planetary Magnetospheres Laboratory, NASA Goddard horizontal resolution at the Martian Space Flight Center, Greenbelt, MD, USA, 4Space Science Laboratory, University of California, Berkeley, CA, USA surface • It enables local studies, where geologic and magnetic features can be compared Abstract While devoid of an active magnetic dynamo field today, Mars possesses a remanent magnetic field that may reach several thousand nanoteslas locally. The exact origin and the events that have shaped the crustal magnetization remain largely enigmatic. Three magnetic field data sets from two spacecraft Supporting Information: • Supporting Information S1 collected over 13 cumulative years have sampled the Martian magnetic field over a range of altitudes •TableS1 from 90 up to 6,000 km: (a) Mars Global Surveyor (MGS) magnetometer (1997–2006), (b) MGS Electron Reflectometer (1999–2006), and (c) Mars Atmosphere and Volatile EvolutioN (MAVEN) magnetometer Correspondence to: (2014 to today). In this paper we combine these complementary data sets for the first time to build a new B. Langlais, model of the Martian internal magnetic field. This new model improves upon previous ones in several [email protected] aspects: comprehensive data coverage, refined data selection scheme, modified modeling scheme, discrete-to-continuous transformation of the model, and increased model resolution. -
Elemental Analysis of Lunar Meteorites Using Laser-Induced Breakdown Spectroscopy
52nd Lunar and Planetary Science Conference 2021 (LPI Contrib. No. 2548) 1729.pdf ELEMENTAL ANALYSIS OF LUNAR METEORITES USING LASER-INDUCED BREAKDOWN SPECTROSCOPY. A. J. Ogura1 ([email protected]), K. Yumoto1, Y. Cho1, T. Niihara2, S. Kameda3, and S. Sugita1, 1Department of Earth and Planetary Science, The University of Tokyo, Tokyo, Japan, 2School of Engineering, The University of Tokyo, 3College of science, Rikkyo University. Introduction: Laser-induced breakdown chromite-spinel, olivine, and pyroxene as phenocrysts spectroscopy (LIBS) is an elemental analysis method in the dark groundmass [9]. NWA11474 is based on the spectra from plasma generated by focused characterized with gray groundmass and white laser pulses. In-situ measurements with LIBS have feldspathic clasts (Fig. 1). All samples were measured already been conducted on planetary missions taking in a vacuum chamber maintained at < 3 × 10-2 Pa. advantages of multiple capabilities of LIBS, such as Data acquisition. We used an Nd:YAG laser (1064 high-spatial resolution (hundreds of microns), rapid, nm, 2 Hz repetition rate, 30 mJ pulse energy). The laser and remote analysis without sample pretreatment (>3 m spot diameter was 800 �m. The spectra were obtained distance in minutes) [1]. Such examples include at a distance of 1 m with an exposure time of 50 ms. 5- ChemCam on NASA’s Curiosity rover [1], SuperCam 9 spots were measured per sample and 100 spectra were on the Perseverance rover [2], and China’s Tianwen-1 obtained per laser spot. The lunar meteorite NWA 479 rover [3]. was measured at light-toned phenocrysts and darker LIBS would be a powerful tool for lunar groundmass. -
Our Solar System
This graphic of the solar system was made using real images of the planets and comet Hale-Bopp. It is not to scale! To show a scale model of the solar system with the Sun being 1cm would require about 64 meters of paper! Image credit: Maggie Mosetti, NASA This book was produced to commemorate the Year of the Solar System (2011-2013, a martian year), initiated by NASA. See http://solarsystem.nasa.gov/yss. Many images and captions have been adapted from NASA’s “From Earth to the Solar System” (FETTSS) image collection. See http://fettss.arc.nasa.gov/. Additional imagery and captions compiled by Deborah Scherrer, Stanford University, California, USA. Special thanks to the people of Suntrek (www.suntrek.org,) who helped with the final editing and allowed me to use Alphonse Sterling’s awesome photograph of a solar eclipse! Cover Images: Solar System: NASA/JPL; YSS logo: NASA; Sun: Venus Transit from NASA SDO/AIA © 2013-2020 Stanford University; permission given to use for educational and non-commericial purposes. Table of Contents Why Is the Sun Green and Mars Blue? ............................................................................... 4 Our Sun – Source of Life ..................................................................................................... 5 Solar Activity ................................................................................................................... 6 Space Weather ................................................................................................................. 9 Mercury -
Radar Sounder Evidence of Thick, Porous Sediments in Meridiani
PUBLICATIONS Geophysical Research Letters RESEARCH LETTER Radar sounder evidence of thick, porous sediments 10.1002/2017GL074431 in Meridiani Planum and implications Key Points: for ice-filled deposits on Mars • The MARSIS radar sounder has detected subsurface echoes deep Thomas R. Watters1 , Carl J. Leuschen2, Bruce A. Campbell1 , Gareth A. Morgan1 , within the Meridiani Planum deposits 3 1 4 5 • The time delay between surface and Andrea Cicchetti , John A. Grant , Roger J. Phillips , and Jeffrey J. Plaut subsurface echoes is consistent with 1 2 deposits having a low bulk value of Center for Earth and Planetary Studies, Smithsonian Institution, Washington, District of Columbia, USA, Center for Remote the real dielectric constant Sensing of Ice Sheets, University of Kansas, Lawrence, Kansas, USA, 3Infocom Department, La Sapienza University of Rome, • New compaction relationships for Rome, Italy, 4Department of Earth and Planetary Sciences and McDonnell Center for the Space Sciences, Washington Mars indicate that a low dielectric University, St. Louis, Missouri, USA, 5Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA constant can be accounted for without invoking pore-filling water ice Abstract Meridiani Planum is one of the most intensely studied regions on Mars, yet little is known about Supporting Information: the physical properties of the deposits below those examined by the Opportunity rover. We report the • Supporting Information S1 detection of subsurface echoes within the Meridiani Planum deposits from data obtained by the Mars Advanced Radar for Subsurface and Ionospheric Sounding (MARSIS) instrument. The delay time between the Correspondence to: T. R. Watters, surface and subsurface returns is indicative of materials with a real dielectric constant of 3.6 ± 0.6. -
Pre-Mission Insights on the Interior of Mars Suzanne E
Pre-mission InSights on the Interior of Mars Suzanne E. Smrekar, Philippe Lognonné, Tilman Spohn, W. Bruce Banerdt, Doris Breuer, Ulrich Christensen, Véronique Dehant, Mélanie Drilleau, William Folkner, Nobuaki Fuji, et al. To cite this version: Suzanne E. Smrekar, Philippe Lognonné, Tilman Spohn, W. Bruce Banerdt, Doris Breuer, et al.. Pre-mission InSights on the Interior of Mars. Space Science Reviews, Springer Verlag, 2019, 215 (1), pp.1-72. 10.1007/s11214-018-0563-9. hal-01990798 HAL Id: hal-01990798 https://hal.archives-ouvertes.fr/hal-01990798 Submitted on 23 Jan 2019 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. Open Archive Toulouse Archive Ouverte (OATAO ) OATAO is an open access repository that collects the wor of some Toulouse researchers and ma es it freely available over the web where possible. This is an author's version published in: https://oatao.univ-toulouse.fr/21690 Official URL : https://doi.org/10.1007/s11214-018-0563-9 To cite this version : Smrekar, Suzanne E. and Lognonné, Philippe and Spohn, Tilman ,... [et al.]. Pre-mission InSights on the Interior of Mars. (2019) Space Science Reviews, 215 (1). -
Human Exploration of Mars Design Reference Architecture 5.0
July 2009 “We are all . children of this universe. Not just Earth, or Mars, or this System, but the whole grand fireworks. And if we are interested in Mars at all, it is only because we wonder over our past and worry terribly about our possible future.” — Ray Bradbury, 'Mars and the Mind of Man,' 1973 Cover Art: An artist’s concept depicting one of many potential Mars exploration strategies. In this approach, the strengths of combining a central habitat with small pressurized rovers that could extend the exploration range of the crew from the outpost are assessed. Rawlings 2007. NASA/SP–2009–566 Human Exploration of Mars Design Reference Architecture 5.0 Mars Architecture Steering Group NASA Headquarters Bret G. Drake, editor NASA Johnson Space Center, Houston, Texas July 2009 ACKNOWLEDGEMENTS The individuals listed in the appendix assisted in the generation of the concepts as well as the descriptions, images, and data described in this report. Specific contributions to this document were provided by Dave Beaty, Stan Borowski, Bob Cataldo, John Charles, Cassie Conley, Doug Craig, Bret Drake, John Elliot, Chad Edwards, Walt Engelund, Dean Eppler, Stewart Feldman, Jim Garvin, Steve Hoffman, Jeff Jones, Frank Jordan, Sheri Klug, Joel Levine, Jack Mulqueen, Gary Noreen, Hoppy Price, Shawn Quinn, Jerry Sanders, Jim Schier, Lisa Simonsen, George Tahu, and Abhi Tripathi. Available from: NASA Center for AeroSpace Information National Technical Information Service 7115 Standard Drive 5285 Port Royal Road Hanover, MD 21076-1320 Springfield, VA 22161 Phone: 301-621-0390 or 703-605-6000 Fax: 301-621-0134 This report is also available in electronic form at http://ston.jsc.nasa.gov/collections/TRS/ CONTENTS 1 Introduction ...................................................................................................................... -
The Structure of Martian Magnetosphere at the Dayside Terminator Region As Observed on MAVEN Spacecraft
Confidential manuscript submitted to Journal of Geophysical Research: Space Physics The Structure of Martian Magnetosphere at the Dayside Terminator Region as Observed on MAVEN Spacecraft O. L. Vaisberg1, V. N. Ermakov1,2, S. D. Shuvalov1, L. M. Zelenyi1, J. Halekas3, G. A. DiBraccio4, J. McFadden5, and E. M. Dubinin6 1 Space Research Institute of the Russian Academy of Sciences, Moscow, Russia. 2 National Research Nuclear University MEPhI, Moscow, Russia. 3 Department of Physics and Astronomy, University of Iowa, Iowa City, Iowa, USA. 4 NASA Goddard Space Flight Center, Maryland, USA. 5 Space Sciences Laboratory, U.C., Berkeley, Berkeley, CA, USA. 6 Max-Planck-Institute for Solar System Research, Gottingen, Germany. Corresponding author: Oleg Vaisberg ([email protected]) Key Points: ● The dayside magnetosphere of Mars at ~700 SZA is a permanent domain of ~200 km thickness between the magnetosheath and the ionosphere + + ● Magnetopause is defined by a steep gradient of O and O2 densities which increase by factor of 102-10 3 at interface with the ionosphere ● The structure of the magnetosphere is controlled by the solar wind magnetic field direction. Confidential manuscript submitted to Journal of Geophysical Research: Space Physics Abstract We analyzed 44 passes of the MAVEN spacecraft through the magnetosphere, arranged by the angle between electric field vector and the projection of spacecraft position radius vector in the YZ plane in MSE coordinate system (θE). All passes were divided into 3 angular sectors near 0°, 90° and 180° θE angles in order to estimate the role of IMF direction in plasma and magnetic properties of dayside Martian magnetosphere. -
Our Solar System
Reader Moons of Our Solar System by Mick Roszel Genre Build Background Access Content Extend Language Expository • The Solar • Diagrams • Word Nonfi ction System • Captions Meanings • Planets and and Labels Moons • Glossary • Moon • Fact Box Geography Scott Foresman Reading Street 4.5.5 ì<(sk$m)=becbbi<ISBN 0-328-14211-5 +^-Ä-U-Ä-U 114211_CVR.indd4211_CVR.indd CCover1over1 33/8/05/8/05 99:26:20:26:20 PPMM Talk About It 1. What is a moon? 2. Look at the diagram on page 4. Describe three things itMoons shows about our of solar Oursystem. Write About It 3. How manySolar moons does S eachystem planet have? Make a graph on a separateby Micksheet Roszel of paper. Put one dot in the graph for each moon. 10 5 0 Mercury Venus Earth Mars Jupiter Extend Language A sphere is a round object, shaped like a ball or a planet. In sphere, pronounce the ph like f. Which of the following things can be called a sphere? the Earth’s moon a crater a soccer ball a coin Photographs Cover ©Omni-Photo Communications, Inc.; 1 ©Photo Researchers, Inc.; 2 ©Omni-Photo Communications, Inc.; 3 ©Bettmann/Corbis; 4 ©Luciano Corbella/DK Images; 5 (CR, BR) ©Corbis; 6 (CL) ©Photo Researchers, Inc., (BR) ©Tom Stack & Associates, Inc.; 7 ©Getty Images; 8 ©Digital Vision; 9 ©Jet Propulsion Laboratory/NASA; 10 ©Roger Ressmeyer/ NASA/Corbis. ISBN: 0-328-14211-5 Copyright © Pearson Education, Inc. All Rights Reserved. Printed in the United States of America. This publication is protected by Copyright, and permission should be obtained from the publisher prior to any prohibited reproduction, storage in a retrieval system, or transmission in any form by any means, electronic, mechanical, photocopying, recording, or likewise. -
Getting to Mars How Close Is Mars?
Getting to Mars How close is Mars? Exploring Mars 1960-2004 Of 42 probes launched: 9 crashed on launch or failed to leave Earth orbit 4 failed en route to Mars 4 failed to stop at Mars 1 failed on entering Mars orbit 1 orbiter crashed on Mars 6 landers crashed on Mars 3 flyby missions succeeded 9 orbiters succeeded 4 landers succeeded 1 lander en route Score so far: Earthlings 16, Martians 25, 1 in play Mars Express Mars Exploration Rover Mars Exploration Rover Mars Exploration Rover 1: Meridiani (Opportunity) 2: Gusev (Spirit) 3: Isidis (Beagle-2) 4: Mars Polar Lander Launch Window 21: Jun-Jul 2003 Mars Express 2003 Jun 2 In Mars orbit Dec 25 Beagle 2 Lander 2003 Jun 2 Crashed at Isidis Dec 25 Spirit/ Rover A 2003 Jun 10 Landed at Gusev Jan 4 Opportunity/ Rover B 2003 Jul 8 Heading to Meridiani on Sunday Launch Window 1: Oct 1960 1M No. 1 1960 Oct 10 Rocket crashed in Siberia 1M No. 2 1960 Oct 14 Rocket crashed in Kazakhstan Launch Window 2: October-November 1962 2MV-4 No. 1 1962 Oct 24 Rocket blew up in parking orbit during Cuban Missile Crisis 2MV-4 No. 2 "Mars-1" 1962 Nov 1 Lost attitude control - Missed Mars by 200000 km 2MV-3 No. 1 1962 Nov 4 Rocket failed to restart in parking orbit The Mars-1 probe Launch Window 3: November 1964 Mariner 3 1964 Nov 5 Failed after launch, nose cone failed to separate Mariner 4 1964 Nov 28 SUCCESS, flyby in Jul 1965 3MV-4 No.