Possibility of Life on Jupiter's Moon
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Galileo and the Telescope
Galileo and the Telescope A Discussion of Galileo Galilei and the Beginning of Modern Observational Astronomy ___________________________ Billy Teets, Ph.D. Acting Director and Outreach Astronomer, Vanderbilt University Dyer Observatory Tuesday, October 20, 2020 Image Credit: Giuseppe Bertini General Outline • Telescopes/Galileo’s Telescopes • Observations of the Moon • Observations of Jupiter • Observations of Other Planets • The Milky Way • Sunspots Brief History of the Telescope – Hans Lippershey • Dutch Spectacle Maker • Invention credited to Hans Lippershey (c. 1608 - refracting telescope) • Late 1608 – Dutch gov’t: “ a device by means of which all things at a very great distance can be seen as if they were nearby” • Is said he observed two children playing with lenses • Patent not awarded Image Source: Wikipedia Galileo and the Telescope • Created his own – 3x magnification. • Similar to what was peddled in Europe. • Learned magnification depended on the ratio of lens focal lengths. • Had to learn to grind his own lenses. Image Source: Britannica.com Image Source: Wikipedia Refracting Telescopes Bend Light Refracting Telescopes Chromatic Aberration Chromatic aberration limits ability to distinguish details Dealing with Chromatic Aberration - Stop Down Aperture Galileo used cardboard rings to limit aperture – Results were dimmer views but less chromatic aberration Galileo and the Telescope • Created his own (3x, 8-9x, 20x, etc.) • Noted by many for its military advantages August 1609 Galileo and the Telescope • First observed the -
2020 Technology and Research Initiative Fund Annual Report
FISCAL YEAR 2020 TECHNOLOGY AND RESEARCH INITIATIVE FUND ABOUT THIS REPORT The fiscal year 2020 Arizona Board of Regents Technology and Research Initiative Fund filed in accordance with A.R.S. §15-1648(D) includes the prior year’s TRIF expenditures. The board adopted TRIF five-year project plans, available on the ABOR website, detailing anticipated budgets and expected outcomes. TRIF was established through Proposition 301 that increased the state’s sales tax to be dedicated to K-12, community colleges and Arizona’s public universities. Collection of the tax began on June 1, 2001, and the proposition was extended for another 20 years in 2018. Arizona law establishes TRIF using Proposition 301 sales tax revenue and gives the Arizona Board of Regents the responsibility to administer the fund. TRIF monies are continuously appropriated to ABOR and do not lapse at the end of the fiscal year. The fiscal year 2020 TRIF report details research goals, accomplishments and highlights from the universities that address challenges to the state and society as well as detailed financial information on how the funds were utilized. Through TRIF funds, the institutions are able to accomplish advances in vital research, including COVID-19 research, virus biotech detection, water resources and more. ABOUT THE ARIZONA BOARD OF REGENTS The Arizona Board of Regents is committed to ensuring access for qualified residents of Arizona to undergraduate and graduate institutions; promoting the discovery, application, and dissemination of new knowledge; extending the benefits of university activities to Arizona’s citizens outside the university; and maximizing the benefits derived from the state’s investment in education. -
JUICE Red Book
ESA/SRE(2014)1 September 2014 JUICE JUpiter ICy moons Explorer Exploring the emergence of habitable worlds around gas giants Definition Study Report European Space Agency 1 This page left intentionally blank 2 Mission Description Jupiter Icy Moons Explorer Key science goals The emergence of habitable worlds around gas giants Characterise Ganymede, Europa and Callisto as planetary objects and potential habitats Explore the Jupiter system as an archetype for gas giants Payload Ten instruments Laser Altimeter Radio Science Experiment Ice Penetrating Radar Visible-Infrared Hyperspectral Imaging Spectrometer Ultraviolet Imaging Spectrograph Imaging System Magnetometer Particle Package Submillimetre Wave Instrument Radio and Plasma Wave Instrument Overall mission profile 06/2022 - Launch by Ariane-5 ECA + EVEE Cruise 01/2030 - Jupiter orbit insertion Jupiter tour Transfer to Callisto (11 months) Europa phase: 2 Europa and 3 Callisto flybys (1 month) Jupiter High Latitude Phase: 9 Callisto flybys (9 months) Transfer to Ganymede (11 months) 09/2032 – Ganymede orbit insertion Ganymede tour Elliptical and high altitude circular phases (5 months) Low altitude (500 km) circular orbit (4 months) 06/2033 – End of nominal mission Spacecraft 3-axis stabilised Power: solar panels: ~900 W HGA: ~3 m, body fixed X and Ka bands Downlink ≥ 1.4 Gbit/day High Δv capability (2700 m/s) Radiation tolerance: 50 krad at equipment level Dry mass: ~1800 kg Ground TM stations ESTRAC network Key mission drivers Radiation tolerance and technology Power budget and solar arrays challenges Mass budget Responsibilities ESA: manufacturing, launch, operations of the spacecraft and data archiving PI Teams: science payload provision, operations, and data analysis 3 Foreword The JUICE (JUpiter ICy moon Explorer) mission, selected by ESA in May 2012 to be the first large mission within the Cosmic Vision Program 2015–2025, will provide the most comprehensive exploration to date of the Jovian system in all its complexity, with particular emphasis on Ganymede as a planetary body and potential habitat. -
An Impacting Descent Probe for Europa and the Other Galilean Moons of Jupiter
An Impacting Descent Probe for Europa and the other Galilean Moons of Jupiter P. Wurz1,*, D. Lasi1, N. Thomas1, D. Piazza1, A. Galli1, M. Jutzi1, S. Barabash2, M. Wieser2, W. Magnes3, H. Lammer3, U. Auster4, L.I. Gurvits5,6, and W. Hajdas7 1) Physikalisches Institut, University of Bern, Bern, Switzerland, 2) Swedish Institute of Space Physics, Kiruna, Sweden, 3) Space Research Institute, Austrian Academy of Sciences, Graz, Austria, 4) Institut f. Geophysik u. Extraterrestrische Physik, Technische Universität, Braunschweig, Germany, 5) Joint Institute for VLBI ERIC, Dwingelo, The Netherlands, 6) Department of Astrodynamics and Space Missions, Delft University of Technology, The Netherlands 7) Paul Scherrer Institute, Villigen, Switzerland. *) Corresponding author, [email protected], Tel.: +41 31 631 44 26, FAX: +41 31 631 44 05 1 Abstract We present a study of an impacting descent probe that increases the science return of spacecraft orbiting or passing an atmosphere-less planetary bodies of the solar system, such as the Galilean moons of Jupiter. The descent probe is a carry-on small spacecraft (< 100 kg), to be deployed by the mother spacecraft, that brings itself onto a collisional trajectory with the targeted planetary body in a simple manner. A possible science payload includes instruments for surface imaging, characterisation of the neutral exosphere, and magnetic field and plasma measurement near the target body down to very low-altitudes (~1 km), during the probe’s fast (~km/s) descent to the surface until impact. The science goals and the concept of operation are discussed with particular reference to Europa, including options for flying through water plumes and after-impact retrieval of very-low altitude science data. -
The Acceler the Accelerating Circulation of Jupiter's Great Red
The accelerating circulation of Jupiter’s Great Red Spot John H. Rogers A report of the Jupiter Section (Director: John H. Rogers) Jupiter’s Great Red Spot (GRS) has been evolving, with fluctuations, since it was first observed in the 19th century. It has shown trends of decreasing length, decelerating drift rate, and possibly accelerating internal circulation. This paper documents how these trends have pro- gressed since the time of the Voyager encounters in 1979, up to 2006, from ground-based amateur observations.1 The trends in length and drift rate have continued; the GRS is now smaller than ever before.2 The internal circulation period was directly measured in 2006 for the first time since the Voyager flybys, and is now 4.5 days, which confirms that the period is shortening.3 In contrast, the 90-day oscillation of the GRS in longitude continues unchanged, and may be accompanied by a very small oscillation in latitude. Introduction =–110, +105°/month: the mean speed of the SEBs and STBn jets) through 63 m/s (DL2 = +130°/month: the mean speed of the SEBs jet when a STropD is present) to 110–140 m/s (the The Great Red Spot (GRS) is a giant anticyclone in Jupiter’s maximum internal wind speed recorded in the Voyager im- atmosphere, circulating anticlockwise, with winds that are ages: Table 1a). Images by the Galileo Orbiter in 2000 re- among the most rapid in the solar system (see reference 1, corded a further acceleration to ~145–190 m/s.11,12 pp.188-197). The circulation was already suspected in the These wind speeds were derived by tracking small cloud early 20th century (ref.1, p.256), and the first tentative obser- tracers over short intervals in spacecraft images. -
Lecture 23: Jupiter Solar System Jupiter's Orbit
Lecture 23: Jupiter Solar System Jupiter’s Orbit •The semi-major axis of Jupiter’s orbit is a = 5.2 AU Jupiter Sun a •Kepler’s third law relates the semi-major axis to the orbital period 1 Jupiter’s Orbit •Kepler’s third law relates the semi-major axis a to the orbital period P 2 3 ⎛ P ⎞ = ⎛ a ⎞ ⎜ ⎟ ⎜ ⎟ ⎝ years⎠ ⎝ AU ⎠ •Solving for the period P yields 3/ 2 ⎛ P ⎞ = ⎛ a ⎞ ⎜ ⎟ ⎜ ⎟ ⎝ years ⎠ ⎝ AU ⎠ •Since a = 5.2 AU for Jupiter, we obtain P = 11.9 Earth years •Jupiter’s orbit has eccentricity e = 0.048 Jupiter’s Orbit •The distance from the Sun varies by about 10% during an orbit Dperihelion = 4.95 AU Daphelion = 5.45 AU •Like Mars, Jupiter is easiest to observe during favorable opposition •At this time, the Earth-Jupiter distance is only about 3.95 AU Earth Jupiter Jupiter Sun (perihelion) (aphelion) •Jupiter appears full during favorable opposition Bulk Properties of Jupiter •Jupiter is the largest planet in the solar system •We have for the radius and mass of Jupiter Rjupiter = 71,400 km = 11.2 Rearth 30 Mjupiter = 1.9 x 10 g = 318 Mearth •The volume of Jupiter is therefore given by 4 V = π R 3 jupiter 3 jupiter 30 3 •Hence Vjupiter = 1.5 x 10 cm 2 Bulk Properties of Jupiter •The average density of Jupiter is therefore M × 30 ρ = jupiter = 1.9 10 g jupiter × 30 3 Vjupiter 1.5 10 cm •We obtain ρ = −3 jupiter 1.24 g cm •This is much less than the average density of the Earth •Hence there is little if any iron and no dense core inside Jupiter Bulk Properties of Jupiter •The average density of the Earth is equal to −3 ρ⊕ = 6 g cm •The density -
PDS Mission Interface for Europa Mission Status of Planning for Data Archiving
PDS Mission Interface for Europa Mission Status of Planning for Data Archiving CARTOGRAPHY AND IMAGING SCIENCES (“Imaging”) NODE PDS Lead Node Lisa Gaddis (USGS, Astrogeology) August 2016 Overview Common goals PDS4 Archiving roles, responsibilities EM archiving deliverables Data and Archive Working Group (DAWG) Archiving assignments Archiving activities to date Archiving schedule Current archiving activities Where we are now August 2016 2 Common Goals The PDS and Europa Mission (EM) will work together to ensure that we Organize, document and format EM digital planetary data in a standardized manner Collect complete, well-documented, peer-reviewed planetary data into archives Make planetary data available and useful to the science community ○ Provide online data delivery tools & services Ensure the long-term preservation and usability of the data August 2016 3 PDS4 The new PDS, an integrated data system to improve access ○ Required for all missions (e.g., used by LADEE, MAVEN) A re-architected, modern, online data system ○ Data are organized into bundles Includes all data for a particular instrument (e.g., PDF/A documents) ○ Bundles have collections Grouped files with a similar origin (e.g., Document Collection) Improves efficiency of ingestion and distribution of data ○ Uses Extensible Markup Language (XML) and standard data format templates ○ Self-consistent information model & software system ○ Information for Data Providers https://pds.nasa.gov/pds4/about ○ PDS4 Concepts Document https://pds.nasa.gov/pds4/doc/concepts/Concepts_150909.pdf -
Using the Galileo Solid-State Imaging Instrument As a Sensor of Jovian
Using the Galileo Solid-State Imaging Instrument as a Sensor of Jovian Energetic Electrons Ashley Carlton1, Maria de Soria-Santacruz Pich2, Insoo Jun2, Wousik Kim2, and Kerri Cahoy1 1Massachusetts Institute of Technology, Cambridge, 02139, USA (e-mail: [email protected]) 2Jet Propulsion Laboratory, California Institute of Technology, Pasadena, 91109, USA respectively. For the most part, information about the Jovian I. INTRODUCTION environment comes from the Galileo spacecraft Energetic Harsh radiation in the form of ionized, highly energetic Particle Detector (EPD) [Williams et al., 1992] (in Jovian particles is part of the space environment and can affect orbit from December 1995 to September 2003), which had a spacecraft. These particles not only sweep through the solar nearly equatorial orbit. Juno, a NASA spacecraft that entered system in the solar wind and flares and are ejected from Jovian orbit in July 2016, and Europa Clipper, a NASA galactic and extra-galactic supernovae, but also are trapped as mission planned for the 2020s, do not carry instruments belts in planetary magnetic fields. Jupiter’s magnetosphere is capable of measuring high-energy (>1 MeV) electrons. Juno is the largest and strongest of a planet in the solar system. in a polar orbit; Europa Clipper is planned to be in a highly Similar to Earth, Jupiter is roughly a magnetic dipole with a elliptical Jovian orbit, flying-by Jupiter’s moon, Europa, in tilt of ~11° [Khurana et al., 2004]. Jupiter’s magnetic field each orbit. strength is an order of magnitude larger than Earth, and its We develop a technique to extract the high-energy magnetic moment is roughly 18,000 times larger [Bagenal et electron environment using scientific imager data. -
Elliptical Instability in Terrestrial Planets and Moons
A&A 539, A78 (2012) Astronomy DOI: 10.1051/0004-6361/201117741 & c ESO 2012 Astrophysics Elliptical instability in terrestrial planets and moons D. Cebron1,M.LeBars1, C. Moutou2,andP.LeGal1 1 Institut de Recherche sur les Phénomènes Hors Equilibre, UMR 6594, CNRS and Aix-Marseille Université, 49 rue F. Joliot-Curie, BP 146, 13384 Marseille Cedex 13, France e-mail: [email protected] 2 Observatoire Astronomique de Marseille-Provence, Laboratoire d’Astrophysique de Marseille, 38 rue F. Joliot-Curie, 13388 Marseille Cedex 13, France Received 21 July 2011 / Accepted 16 January 2012 ABSTRACT Context. The presence of celestial companions means that any planet may be subject to three kinds of harmonic mechanical forcing: tides, precession/nutation, and libration. These forcings can generate flows in internal fluid layers, such as fluid cores and subsurface oceans, whose dynamics then significantly differ from solid body rotation. In particular, tides in non-synchronized bodies and libration in synchronized ones are known to be capable of exciting the so-called elliptical instability, i.e. a generic instability corresponding to the destabilization of two-dimensional flows with elliptical streamlines, leading to three-dimensional turbulence. Aims. We aim here at confirming the relevance of such an elliptical instability in terrestrial bodies by determining its growth rate, as well as its consequences on energy dissipation, on magnetic field induction, and on heat flux fluctuations on planetary scales. Methods. Previous studies and theoretical results for the elliptical instability are re-evaluated and extended to cope with an astro- physical context. In particular, generic analytical expressions of the elliptical instability growth rate are obtained using a local WKB approach, simultaneously considering for the first time (i) a local temperature gradient due to an imposed temperature contrast across the considered layer or to the presence of a volumic heat source and (ii) an imposed magnetic field along the rotation axis, coming from an external source. -
Planets of the Solar System
Chapter Planets of the 27 Solar System Chapter OutlineOutline 1 ● Formation of the Solar System The Nebular Hypothesis Formation of the Planets Formation of Solid Earth Formation of Earth’s Atmosphere Formation of Earth’s Oceans 2 ● Models of the Solar System Early Models Kepler’s Laws Newton’s Explanation of Kepler’s Laws 3 ● The Inner Planets Mercury Venus Earth Mars 4 ● The Outer Planets Gas Giants Jupiter Saturn Uranus Neptune Objects Beyond Neptune Why It Matters Exoplanets UnderstandingU d t di theth formationf ti and the characteristics of our solar system and its planets can help scientists plan missions to study planets and solar systems around other stars in the universe. 746 Chapter 27 hhq10sena_psscho.inddq10sena_psscho.indd 774646 PDF 88/15/08/15/08 88:43:46:43:46 AAMM Inquiry Lab Planetary Distances 20 min Turn to Appendix E and find the table entitled Question to Get You Started “Solar System Data.” Use the data from the How would the distance of a planet from the sun “semimajor axis” row of planetary distances to affect the time it takes for the planet to complete devise an appropriate scale to model the distances one orbit? between planets. Then find an indoor or outdoor space that will accommodate the farthest distance. Mark some index cards with the name of each planet, use a measuring tape to measure the distances according to your scale, and place each index card at its correct location. 747 hhq10sena_psscho.inddq10sena_psscho.indd 774747 22/26/09/26/09 111:42:301:42:30 AAMM These reading tools will help you learn the material in this chapter. -
The Solar System Cause Impact Craters
ASTRONOMY 161 Introduction to Solar System Astronomy Class 12 Solar System Survey Monday, February 5 Key Concepts (1) The terrestrial planets are made primarily of rock and metal. (2) The Jovian planets are made primarily of hydrogen and helium. (3) Moons (a.k.a. satellites) orbit the planets; some moons are large. (4) Asteroids, meteoroids, comets, and Kuiper Belt objects orbit the Sun. (5) Collision between objects in the Solar System cause impact craters. Family portrait of the Solar System: Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, Neptune, (Eris, Ceres, Pluto): My Very Excellent Mother Just Served Us Nine (Extra Cheese Pizzas). The Solar System: List of Ingredients Ingredient Percent of total mass Sun 99.8% Jupiter 0.1% other planets 0.05% everything else 0.05% The Sun dominates the Solar System Jupiter dominates the planets Object Mass Object Mass 1) Sun 330,000 2) Jupiter 320 10) Ganymede 0.025 3) Saturn 95 11) Titan 0.023 4) Neptune 17 12) Callisto 0.018 5) Uranus 15 13) Io 0.015 6) Earth 1.0 14) Moon 0.012 7) Venus 0.82 15) Europa 0.008 8) Mars 0.11 16) Triton 0.004 9) Mercury 0.055 17) Pluto 0.002 A few words about the Sun. The Sun is a large sphere of gas (mostly H, He – hydrogen and helium). The Sun shines because it is hot (T = 5,800 K). The Sun remains hot because it is powered by fusion of hydrogen to helium (H-bomb). (1) The terrestrial planets are made primarily of rock and metal. -
Thermal Structure and Composition of Jupiter's Great Red Spot from High-Resolution Thermal Imaging
Thermal Structure and Composition of Jupiter’s Great Red Spot from High-Resolution Thermal Imaging Leigh N. Fletchera,b, G. S. Ortona, O. Mousisc,d, P. Yanamandra-Fishera, P. D. Parrishe,a, P. G. J. Irwinb, B. M. Fishera, L. Vanzif, T. Fujiyoshig, T. Fuseg, A.A. Simon-Millerh, E. Edkinsi, T.L. Haywardj, J. De Buizerk aJet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA, 91109, USA bAtmospheric, Oceanic and Planetary Physics, Department of Physics, University of Oxford, Clarendon Laboratory, Parks Road, Oxford, OX1 3PU, UK cInstitut UTINAM, CNRS-UMR 6213, Observatoire de Besan¸con, Universit´ede Franche-Comt´e, Besan¸con, France dLunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA eSchool of GeoScience, University of Edinburgh, Crew Building, King’s Buildings, Edinburgh, EH9 3JN, UK fPontificia Universidad Catolica de Chile, Department of Electrical Engineering, Av. Vicuna Makenna 4860, Santiago, Chile. gSubaru Telescope, National Astronomical Observatory of Japan, National Institutes of Natural Sciences, 650 North A’ohoku Place, Hilo, Hawaii 96720, USA hNASA/Goddard Spaceflight Center, Greenbelt, Maryland, 20771, USA iUniversity of California, Santa Barbara, Santa Barbara, CA 93106, USA jGemini Observatory, Southern Operations Center, c/o AURA, Casilla 603, La Serena, Chile. kSOFIA - USRA, NASA Ames Research Center, Moffet Field, CA 94035, USA. Abstract Thermal-IR imaging from space-borne and ground-based observatories was used to investigate the temperature, composition and aerosol structure of Jupiter’s Great Red Spot (GRS) and its temporal variability between 1995-2008. An elliptical warm core, extending over 8◦ of longitude and 3◦ of latitude, was observed within the cold anticyclonic vortex at 21◦S.