Reddy Saturn's Small Wonders Astronomy 46 No 03 (2018)-1.Pdf
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Index Abulfeda crater chain (Moon), 97 Aphrodite Terra (Venus), 142, 143, 144, 145, 146 Acheron Fossae (Mars), 165 Apohele asteroids, 353–354 Achilles asteroids, 351 Apollinaris Patera (Mars), 168 achondrite meteorites, 360 Apollo asteroids, 346, 353, 354, 361, 371 Acidalia Planitia (Mars), 164 Apollo program, 86, 96, 97, 101, 102, 108–109, 110, 361 Adams, John Couch, 298 Apollo 8, 96 Adonis, 371 Apollo 11, 94, 110 Adrastea, 238, 241 Apollo 12, 96, 110 Aegaeon, 263 Apollo 14, 93, 110 Africa, 63, 73, 143 Apollo 15, 100, 103, 104, 110 Akatsuki spacecraft (see Venus Climate Orbiter) Apollo 16, 59, 96, 102, 103, 110 Akna Montes (Venus), 142 Apollo 17, 95, 99, 100, 102, 103, 110 Alabama, 62 Apollodorus crater (Mercury), 127 Alba Patera (Mars), 167 Apollo Lunar Surface Experiments Package (ALSEP), 110 Aldrin, Edwin (Buzz), 94 Apophis, 354, 355 Alexandria, 69 Appalachian mountains (Earth), 74, 270 Alfvén, Hannes, 35 Aqua, 56 Alfvén waves, 35–36, 43, 49 Arabia Terra (Mars), 177, 191, 200 Algeria, 358 arachnoids (see Venus) ALH 84001, 201, 204–205 Archimedes crater (Moon), 93, 106 Allan Hills, 109, 201 Arctic, 62, 67, 84, 186, 229 Allende meteorite, 359, 360 Arden Corona (Miranda), 291 Allen Telescope Array, 409 Arecibo Observatory, 114, 144, 341, 379, 380, 408, 409 Alpha Regio (Venus), 144, 148, 149 Ares Vallis (Mars), 179, 180, 199 Alphonsus crater (Moon), 99, 102 Argentina, 408 Alps (Moon), 93 Argyre Basin (Mars), 161, 162, 163, 166, 186 Amalthea, 236–237, 238, 239, 241 Ariadaeus Rille (Moon), 100, 102 Amazonis Planitia (Mars), 161 COPYRIGHTED -
Annualreport2005 Web.Pdf
Vision Statement The Space Science Institute is a thriving center of talented, entrepreneurial scientists, educators, and other professionals who make outstanding contributions to humankind’s understanding and appreciation of planet Earth, the Solar System, the galaxy, and beyond. 2 | Space Science Institute | Annual Report 2005 From Our Director Excite. Explore. Discover. These words aptly describe what we do in the research realm as well as in education. In fact, they defi ne the essence of our mission. Our mission is facilitated by a unique blend of on- and off-site researchers coupled with an extensive portfolio of education and public outreach (EPO) projects. This past year has seen SSI grow from $4.1M to over $4.3M in grants, an increase of nearly 6%. We now have over fi fty full and part-time staff. SSI’s support comes mostly from NASA and the National Sci- ence Foundation. Our Board of Directors now numbers eight. Their guidance and vision—along with that of senior management—have created an environment that continues to draw world-class scientists to the Institute and allows us to develop educa- tion and outreach programs that benefi t millions of people worldwide. SSI has a robust scientifi c research program that includes robotic missions such as the Mars Exploration Rovers, fl ight missions such as Cassini and the Spitzer Space Telescope, Hubble Space Telescope (HST), and ground-based programs. Dr. Tom McCord joined the Institute in 2005 as a Senior Research Scientist. He directs the Bear Fight Center, a 3,000 square-foot research and meeting facility in Washington state. -
Rings and Moons of Saturn 1 Rings and Moons of Saturn
PYTS/ASTR 206 – Rings and Moons of Saturn 1 Rings and Moons of Saturn PTYS/ASTR 206 – The Golden Age of Planetary Exploration Shane Byrne – [email protected] PYTS/ASTR 206 – Rings and Moons of Saturn 2 In this lecture… Rings Discovery What they are How to form rings The Roche limit Dynamics Voyager II – 1981 Gaps and resonances Shepherd moons Voyager I – 1980 – Titan Inner moons Tectonics and craters Cassini – ongoing Enceladus – a very special case Outer Moons Captured Phoebe Iapetus and Hyperion Spray-painted with Phoebe debris PYTS/ASTR 206 – Rings and Moons of Saturn 3 We can divide Saturn’s system into three main parts… The A-D ring zone Ring gaps and shepherd moons The E ring zone Ring supplies by Enceladus Tethys, Dione and Rhea have a lot of similarities The distant satellites Iapetus, Hyperion, Phoebe Linked together by exchange of material PYTS/ASTR 206 – Rings and Moons of Saturn 4 Discovery of Saturn’s Rings Discovered by Galileo Appearance in 1610 baffled him “…to my very great amazement Saturn was seen to me to be not a single star, but three together, which almost touch each other" It got more confusing… In 1612 the extra “stars” had disappeared “…I do not know what to say…" PYTS/ASTR 206 – Rings and Moons of Saturn 5 In 1616 the extra ‘stars’ were back Galileo’s telescope had improved He saw two “half-ellipses” He died in 1642 and never figured it out In the 1650s Huygens figured out that Saturn was surrounded by a flat disk The disk disappears when seen edge on He discovered Saturn’s -
Next - Saturn’S Moon Cassini Mission - July 1, 2004
Next - Saturn’s moon Cassini Mission - July 1, 2004 • 74 Orbits of Saturn • 44 close flybys of Titan • 8 close targeted flybys of other satellites • 30 additional satellite flybys at distances less than 62,100 mi • Many Saturn & Ring Occultation opportunities 4 year path of Cassini Saturn’s Moons • Moons show less variation in properties than Jupiter’s moons, & Saturn’s ring system is more extensive: smaller mass of Saturn? Lower temperature of sub- nebula?? Something else? • Moons are half ice, half rock, but most have density range ~ 1.1 - 1.4 g cm-3. The moons are smaller - less compression of ice than previously discussed icy moons • Many moons have high lunar-like crater counts Pandora Mimas - the “Deathstar” moon • Density = 1.2 g cm-3 • Crater size = 80mi x 6 mi • Moon Diameter = 247 mi • Rotation period =0.94 days • Orbital period = 0.94 days Mimas Occulting Janus Mimas & Saturn’s Rings Enceladus • Density = 1.1 g cm-3 • Rotation period = 1.4 days • Orbital period = 1.4 days • Surface: a mixture of soft craters & complex fracture terrains • terrains ~ few hundred million yr old Enceladus - Activity • Cryovolcanism: flow of partially melted ice that mimics lava flows on silicate planets • Spray of H2O + ice particles observed emanating from Enceladus • Looks like Io, but Enceladus isn’t forced into non-circular orbit by companion moons like Io. What is causing this activity?? Blue Streaks • Are warmer than surrounding regions, clearly indicating heat- leak • It’s not clear how the heat reaches the surface Close Approach • Boulders of ice are visible in geologically active region • Sizes ~ 30 - 330 ft in diameter Atmosphere of Enceladus • Has been detected via an occultation of a star. -
Exploring Saturn with Cassini/Huygens
Exploring Saturn with Cassini/Huygens Paul Withers Boston University ([email protected]) How do stellar systems and planets form? How do they evolve over time? How are the building blocks of life made? How can simple physics be applied to these big questions? Tufts Physics Department Seminar 2004.11.05 saturn.jpl.nasa.gov Overview • Before Cassini • Main Research Areas – Saturn – Rings – Icy Satellites – Magnetosphere –Titan • Cassini Mission • First Cassini observations at Saturn • Huygens Mission 1610, Galileo Galilei discovers that Saturn changes shape galileo.rice.edu 1655, Christaan Huygens discovers that Saturn has a satellite, Titan 1659, Huygens proposes that Saturn is surrounded by a thin, flat ring galileo.rice.edu 1670-1675, Giovanni Domenico Cassini discovers four more satellites and a division within the rings www.windows.ucar.edu Saturn • 10 AU, 27o obliquity, circular orbit, 10hr day • 10 x RE, 0.7 g/cc, 10% flattening • Metal/rock core of ~10 ME, metallic H/He layer, molecular H/He, internal He rain • Radiates internal heat • Clouds of NH3, NH4SH, H2O • Dynamics in belts/zones, with ovals/spots imgsrc.hubblesite.org Latitudinal banding (belts/zones) are regions of upwelling/downwelling How deep do they go? Few 100 m/s zonal winds Less colorful than Jupiter due to lower T – we think Ovals are storm systems that interact, merge Polar winds? photojournal.jpl.nasa.gov saturn.jpl.nasa.gov Rings • 1.1 – 8.0 RS, mostly ice, some rock • Range of sizes, microns to metres • Less than 1 km thick • Organized by shepherd moons and additional -
Appendix A: Association of Lunar and Planetary Observers Forms
12SHO_APPa(164-173).qxd 21/9/05 11:44 AM Page 164 Appendix A: Association of Lunar and Planetary Appendix A: ALPO Forms Observers Forms Association of Lunar and Planetary Observers (ALPO) Saturn Section: Central Meridian (CM) Transit Data and Sectional Sketches (Attach this form to main observation form) Observer: __________________________________________________ Object: ___________________________________ S UT Date:___________ UT Time:__________ p d f Location:_____________________(do sectional drawing at right) 2 CM I: ________° CM II: ________° d : _______ d : _______ 1 2 d1 N Object: ___________________________________ S UT Date:___________ UT Time:__________ Location:_____________________(do sectional drawing at right) p d f 2 ° ° CM I: ________ CM II: ________ d1: _______ d2: _______ d1 N Object: ___________________________________ S UT Date:___________ UT Time:__________ p d f Location:_____________________(do sectional drawing at right) 2 CM I: ________° CM II: ________° d : _______ d : _______ 1 2 d1 N Object: ___________________________________ S UT Date:___________ UT Time:__________ p d f Location:_____________________(do sectional drawing at right) 2 ° ° CM I: ________ CM II: ________ d1: _______ d2: _______ d1 N Sectional Sketch Notation: d1 = longitudinal extent in arc sec ( ) p = preceding (all directions are IAU) d2 = latitudinal extent in arc sec ( ) f = following Copyright ©2002 JLB. All rights reserved. 164 12SHO_APPa(164-173).qxd 21/9/05 11:44 AM Page 165 Association of Lunar and Planetary Observers (ALPO) Saturn -
Mission Science Highlights and Science Objectives Assessment
CASSINI FINAL MISSION REPORT 2019 1 MISSION SCIENCE HIGHLIGHTS AND SCIENCE OBJECTIVES ASSESSMENT Cassini-Huygens, humanity’s most distant planetary orbiter and probe to date, provided the first in- depth, close up study of Saturn, its magnificent rings and unique moons, including Titan and Enceladus, and its giant magnetosphere. Discoveries from the Cassini-Huygens mission revolutionized our understanding of the Saturn system and fundamentally altered many of our concepts of where life might be found in our solar system and beyond. Cassini-Huygens arrived at Saturn in 2004, dropped the parachuted probe named Huygens to study the atmosphere and surface of Saturn’s planet-sized moon Titan, and orbited Saturn for the next 13 years making remarkable discoveries. When it was running low on fuel, the Cassini orbiter was programmed to vaporize in Saturn’s atmosphere in 2017 to protect the ocean worlds, Enceladus and Titan, where it discovered potential habitats for life. CASSINI FINAL MISSION REPORT 2019 2 CONTENTS MISSION SCIENCE HIGHLIGHTS AND SCIENCE OBJECTIVES ASSESSMENT ........................................................ 1 Executive Summary................................................................................................................................................ 5 Origin of the Cassini Mission ....................................................................................................................... 5 Instrument Teams and Interdisciplinary Investigations ............................................................................... -
Geology and Stratigraphy of Saturn's Moon Tethys
EPSC Abstracts Vol. 8, EPSC2013-713, 2013 European Planetary Science Congress 2013 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2013 Geology and Stratigraphy of Saturn’s moon Tethys R. J. Wagner (1), K. Stephan (1), N. Schmedemann (2), T. Roatsch (1), E. Kersten (1), G. Neukum (2), and C. C. Porco (3). (1) DLR, Inst. of Planetary Research, Berlin, Germany, (email: [email protected]), (2) Institute of Geosciences, Freie Universitaet Berlin, Germany, (3) Space Science Institute, Boulder/Co., USA. 1. Introduction 3.1 Cratered plains units Tethys is 1066 km in diameter and one of Saturn’s Hilly, rugged, undulating densely cratered plains six mid-sized icy satellites, orbiting Saturn between (cpd) were previously identified in Voyager images the volcanically active moon Enceladus und Dione. [5]. Fine-scale tectonic features such as narrow, The satellite was imaged for the first time by the linear to slightly arcuate fractures, are abundant in cameras aboard Voyager 1 & 2. These images some localities of this unit. A smooth cratered plains showed two major landforms: (a) the 445-km large unit (cps) occurs near the impact basin Penelope. impact basin Odysseus, and (b) the graben system This unit was detected in Voyager images [5], but its Ithaca Chasma [1][2]. The Cassini spacecraft, in boundaries can now be located more precisely in ISS orbit about Saturn since July 1, 2004, has made data. To the south of impact basin Odysseus, the several close passes at Tethys, providing an almost Cassini ISS data revealed a previously unknown hilly complete image coverage at 200 – 500 m/pxl cratered plains unit (cpsc) which has a lower resolutions. -
A Voyage Round Saturn, Its Rings and Moons Transcript
A voyage round Saturn, its rings and moons Transcript Date: Wednesday, 2 November 2011 - 1:00PM Location: Museum of London 2 November 2011 A Voyage Round Saturn, its Moons and Rings Professor Carolin Crawford INTRODUCTION Saturn is the most distant planet easily visible to the unaided eye, and as such it has been watched closely since prehistoric times. Its particular mystery was only unveiled when Galileo Galilei first turned his simple optical telescope to it in 1610, and immediately noticed something strange about the planet. At first he guessed that its elongated shape was due to a couple of large moons to either side of Saturn; two years later these had disappeared, only to be replaced by two arched ‘cup handles’ to the planet by 1616. It wasn’t until Christiaan Huygens was able to observe Saturn with a much improved version of a telescope in 1659 that the mystery was resolved, when he identified the two ‘handles’ as a ring encircling the planet. Huygens also discovered Saturn's largest moon, Titan. A few years later, Jean-Dominique Cassini discovered a further four moons of Saturn, and resolved the surrounding ring into a series of rings, separated by gaps – the most apparent of these gaps has since been named for him. Today we have the opportunity to scrutinise Saturn in detail, with the luxury of remote exploration by robotic spacecraft; and yet the planet and its complex system of rings and moons remains intriguing. Saturn has been visited by spacecraft only four times. Three were brief flybys: Pioneer 11 in 1979, followed by Voyagers 1 and 2 in 1980 and 1981. -
Cassini Mission Science Report – ISS
Volume 1: Cassini Mission Science Report – ISS Carolyn Porco, Robert West, John Barbara, Nicolas Cooper, Anthony Del Genio, Tilmann Denk, Luke Dones, Michael Evans, Matthew Hedman, Paul Helfenstein, Andrew Ingersoll, Robert Jacobson, Alfred McEwen, Carl Murray, Jason Perry, Thomas Roatsch, Peter Thomas, Matthew Tiscareno, Elizabeth Turtle Table of Contents Executive Summary ……………………………………………………………………………………….. 1 1 ISS Instrument Summary …………………………………………………………………………… 2 2 Key Objectives for ISS Instrument ……………………………………………………………… 4 3 ISS Science Assessment …………………………………………………………………………….. 6 4 ISS Saturn System Science Results …………………………………………………………….. 9 4.1 Titan ………………………………………………………………………………………………………………………... 9 4.2 Enceladus ………………………………………………………………………………………………………………… 11 4 3 Main Icy Satellites ……………………………………………………………………………………………………. 16 4.4 Satellite Orbits & Orbital Evolution…………………………………………………….……………………. 21 4.5 Small Satellites ……………………………………………………………………………………………………….. 22 4.6 Phoebe and the Irregular Satellites ………………………………………………………………………… 23 4.7 Saturn ……………………………………………………………………………………………………………………. 25 4.8 Rings ………………………………………………………………………………………………………………………. 28 4.9 Open Questions for Saturn System Science ……………………………………………………………… 33 5 ISS Non-Saturn Science Results …………………………………………………………………. 41 5.1 Jupiter Atmosphere and Rings………………………………………………………………………………… 41 5.2 Jupiter/Exoplanet Studies ………………………………………………………………………………………. 43 5.3 Jupiter Satellites………………………………………………………………………………………………………. 43 5.4 Open Questions for Non-Saturn Science …………………………………………………………………. -
Implications from Ithaca Chasma for the Thermal and Orbital History of Tethys E
GEOPHYSICAL RESEARCH LETTERS, VOL. 35, L19203, doi:10.1029/2008GL035402, 2008 Click Here for Full Article Implications from Ithaca Chasma for the thermal and orbital history of Tethys E. M. A. Chen1 and F. Nimmo1 Received 18 July 2008; revised 8 September 2008; accepted 12 September 2008; published 10 October 2008. [1] Flexural modeling of Ithaca Chasma on Tethys required for Tethys to have been tidally heated to the extent suggests that the elastic thickness and the surface heat suggested by topographic profiles of Ithaca Chasma. flux were 5–7 km and 18–30 mW/m2 respectively, when the feature formed (4 Gyr B.P.). Tidal heating is a plausible 2. Methods heat source, suggesting that Tethys’ eccentricity was higher 2.1. Tidal Dissipation in the past. Depending on Tethys’ internal structure, [4] Models of global tidal dissipation have been applied to eccentricities in the range 0.001 to 0.02 are sufficient to have various icy satellites [Ross and Schubert, 1989; Segatz et al., generated the inferred heat flux. Because the eccentricity 1988; Roberts and Nimmo, 2008]. For a synchronous damping timescale is short, < 20 Myr, it is unlikely that this satellite in an eccentric orbit, the rate of tidal dissipation, eccentricity was primordial. More likely, Tethys’ eccentricity E_ , is a function of the orbital eccentricity, e, the mean increased during passage through a 3:2 resonance with Dione. 2 motion, n, the satellite radius, R , the satellite’s interior In equilibrium, this resonance produces 2.5 mW/m s structure as parameterized by k , the degree-2 complex tidal suggesting that non-equilibrium or periodic heating was 2 Love number, and the gravitational constant, G [Segatz et important, similar to the case for Enceladus at present. -
Tectonic Mapping of Rift Zones on Rhea, Tethys, and Dione P
46th Lunar and Planetary Science Conference (2015) 2251.pdf TECTONIC MAPPING OF RIFT ZONES ON RHEA, TETHYS, AND DIONE P. K. Byrne1, P. M. Schenk1, and P. J. McGovern1. 1Lunar and Planetary Institute, Universities Space Research Association, Houston, TX 77058 ([email protected]). ▪ Large rifts occur on each moon, increasing in Our global topographic products are combined from tectonic complexity from Rhea, to Tethys, to Dione stereophotogrammetry- and photoclinometry-derived ▪ Rifting is oriented ~N–S, concentrated within or DTMs. We have generated photomosaics at effective bordering these bodies’ trailing hemispheres resolutions of 400 m/px for Rhea, and at 250 m/px for ▪ The pattern of deformation is similar despite Tethys and Dione. Our global DTMs of Rhea, Tethys, differences in satellite size and interior structure and Dione have resolutions of 1,000 m/px, 500 m/px, and 400 m/px, respectively. Within ArcGIS, we record Introduction: Rhea, Tethys, and Dione are among the surface traces of tectonic landforms, document the largest moons of Saturn. Each exhibits substantial morphometrics such as overlap between individual extensional tectonic deformation in the form of rift fault segments, and estimate strains across select zones (termed chasmata). With a radius of 561 km, structures and the chasmata in general. Dione is likely primarily composed of water ice but Rift Zone Distributions: The distributions of the may have a silicate core. Tethys is 531 km in radius chasmata on Rhea, Tethys, and Dione, are shown and is composed almost entirely of water ice. Rhea has schematically in Fig. 1. a radius of 764 km and consists primarily of water ice, but whether this moon is differentiated is unknown [1].