Titan and the Moons of Saturn Telesto Titan
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Arxiv:1912.09192V2 [Astro-Ph.EP] 24 Feb 2020
Draft version February 25, 2020 Typeset using LATEX preprint style in AASTeX62 Photometric analyses of Saturn's small moons: Aegaeon, Methone and Pallene are dark; Helene and Calypso are bright. M. M. Hedman,1 P. Helfenstein,2 R. O. Chancia,1, 3 P. Thomas,2 E. Roussos,4 C. Paranicas,5 and A. J. Verbiscer6 1Department of Physics, University of Idaho, Moscow, ID 83844 2Cornell Center for Astrophysics and Planetary Science, Cornell University, Ithaca NY 14853 3Center for Imaging Science, Rochester Institute of Technology, Rochester NY 14623 4Max Planck Institute for Solar System Research, G¨ottingen,Germany 37077 5APL, John Hopkins University, Laurel MD 20723 6Department of Astronomy, University of Virginia, Charlottesville, VA 22904 ABSTRACT We examine the surface brightnesses of Saturn's smaller satellites using a photometric model that explicitly accounts for their elongated shapes and thus facilitates compar- isons among different moons. Analyses of Cassini imaging data with this model reveals that the moons Aegaeon, Methone and Pallene are darker than one would expect given trends previously observed among the nearby mid-sized satellites. On the other hand, the trojan moons Calypso and Helene have substantially brighter surfaces than their co-orbital companions Tethys and Dione. These observations are inconsistent with the moons' surface brightnesses being entirely controlled by the local flux of E-ring par- ticles, and therefore strongly imply that other phenomena are affecting their surface properties. The darkness of Aegaeon, Methone and Pallene is correlated with the fluxes of high-energy protons, implying that high-energy radiation is responsible for darkening these small moons. Meanwhile, Prometheus and Pandora appear to be brightened by their interactions with nearby dusty F ring, implying that enhanced dust fluxes are most likely responsible for Calypso's and Helene's excess brightness. -
Cassini Update
Cassini Update Dr. Linda Spilker Cassini Project Scientist Outer Planets Assessment Group 22 February 2017 Sols%ce Mission Inclina%on Profile equator Saturn wrt Inclination 22 February 2017 LJS-3 Year 3 Key Flybys Since Aug. 2016 OPAG T124 – Titan flyby (1584 km) • November 13, 2016 • LAST Radio Science flyby • One of only two (cf. T106) ideal bistatic observations capturing Titan’s Northern Seas • First and only bistatic observation of Punga Mare • Western Kraken Mare not explored by RSS before T125 – Titan flyby (3158 km) • November 29, 2016 • LAST Optical Remote Sensing targeted flyby • VIMS high-resolution map of the North Pole looking for variations at and around the seas and lakes. • CIRS last opportunity for vertical profile determination of gases (e.g. water, aerosols) • UVIS limb viewing opportunity at the highest spatial resolution available outside of occultations 22 February 2017 4 Interior of Hexagon Turning “Less Blue” • Bluish to golden haze results from increased production of photochemical hazes as north pole approaches summer solstice. • Hexagon acts as a barrier that prevents haze particles outside hexagon from migrating inward. • 5 Refracting Atmosphere Saturn's• 22unlit February rings appear 2017 to bend as they pass behind the planet’s darkened limb due• 6 to refraction by Saturn's upper atmosphere. (Resolution 5 km/pixel) Dione Harbors A Subsurface Ocean Researchers at the Royal Observatory of Belgium reanalyzed Cassini RSS gravity data• 7 of Dione and predict a crust 100 km thick with a global ocean 10’s of km deep. Titan’s Summer Clouds Pose a Mystery Why would clouds on Titan be visible in VIMS images, but not in ISS images? ISS ISS VIMS High, thin cirrus clouds that are optically thicker than Titan’s atmospheric haze at longer VIMS wavelengths,• 22 February but optically 2017 thinner than the haze at shorter ISS wavelengths, could be• 8 detected by VIMS while simultaneously lost in the haze to ISS. -
Volvo-Wheel-Brochure.Pdf
S40, V50 (2004.5 on) VOLVO ALLOY WHEELS Adaro: Silverstone Caligo: Silverstone Castalia: Silverstone Cepheus: Silverstone Clava: Black Chrome Cygnus: Silverstone Medea: Silver Bright Medusa: Silver Bright Sagitta: Silver Bright Sculptor: Silver Bright Stylla: Silverstone S40, V40 (up to model year 2004) Adaro (15”) Adrastea (16”) Amalthea (17”) Andromeda (16”) Antlia (15”) Aquarius (17”) Ares (16”) Argo (15”) Argon (15”) Ares: Silver Bright Crater: Silver Cronus: Silver Bright Galactica: Silverstone Helia: Silver Spectra: Dark Silver Stellar: Silverstone Telesto: Silverstone C70 Andromeda: Silver Bright Ariane (15”) Arrakis (17”) Atlantis (18”) Caligo (16”) Canisto (17”) Capella (18”) Castalia (16”) Centaurus (16”) Cepheus (16”) Canisto: White Silver and Anthracite Centaurus: White Silver Ceres: Silver Bright Comet C: Silver Bright Cratos: Silver Bright Helios: Dark Silver Helium: White Silver Propus C: Silverstone Solar: Silver Bright Triton: Silver Zeus: Silver Bright Ceres (16”) Cetus (15”) Clava (16”) Columba (16”) Comet (17”) Crater (16”) Cratos (17”) Cronos (16”) Cygnus (16”) S60, S80, V70 (2001 on) Adrastea: Silverstone (excluding S80, XC70) Amalthea: Silver Bright Argon: Silverstone (excluding XC70) Arrakis: Silver Bright (S60, S80 only) Capella: Silver Bright Icarus: Silverstone Interceptor: Silver Bright (S60, S80 only) Lysithea: Silverstone (excluding XC70) Metis: Silverstone Mimas: Silverstone (excluding S80, XC70) Miram: Silverstone Galactica (16”) Helia (16”) Helium (16”) Icarus (16”) Interceptor (17”) Lysithea (15”) Medea -
Tidal Heating in Enceladus
Icarus 188 (2007) 535–539 www.elsevier.com/locate/icarus Note Tidal heating in Enceladus Jennifer Meyer ∗, Jack Wisdom Massachusetts Institute of Technology, Cambridge, MA 02139, USA Received 20 February 2007; revised 3 March 2007 Available online 19 March 2007 Abstract The heating in Enceladus in an equilibrium resonant configuration with other saturnian satellites can be estimated independently of the physical properties of Enceladus. We find that equilibrium tidal heating cannot account for the heat that is observed to be coming from Enceladus. Equilibrium heating in possible past resonances likewise cannot explain prior resurfacing events. © 2007 Elsevier Inc. All rights reserved. Keywords: Enceladus; Saturn, satellites; Satellites, dynamics; Resonances, orbital; Tides, solid body 1. Introduction One mechanism for heating Enceladus that passes the Mimas test is the secondary spin–orbit libration model (Wisdom, 2004). Fits to the shape of Enceladus is a puzzle. Cassini observed active plumes emanating from Enceladus from Voyager images indicated that the frequency of small amplitude Enceladus (Porco et al., 2006). The plumes consist almost entirely of water oscillations about the Saturn-pointing orientation of Enceladus was about 1/3 vapor, with entrained water ice particles of typical size 1 µm. Models of the of the orbital frequency. In the phase-space of the spin–orbit problem near the plumes suggest the existence of liquid water as close as 7 m to the surface damped synchronous state the stable equilibrium bifurcates into a period-tripled (Porco et al., 2006). An alternate model has the water originate in a clathrate state. If Enceladus were trapped in this bifurcated state, then there could be sev- reservoir (Kieffer et al., 2006). -
The Orbits of Saturn's Small Satellites Derived From
The Astronomical Journal, 132:692–710, 2006 August A # 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE ORBITS OF SATURN’S SMALL SATELLITES DERIVED FROM COMBINED HISTORIC AND CASSINI IMAGING OBSERVATIONS J. N. Spitale CICLOPS, Space Science Institute, 4750 Walnut Street, Suite 205, Boulder, CO 80301; [email protected] R. A. Jacobson Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109-8099 C. C. Porco CICLOPS, Space Science Institute, 4750 Walnut Street, Suite 205, Boulder, CO 80301 and W. M. Owen, Jr. Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109-8099 Received 2006 February 28; accepted 2006 April 12 ABSTRACT We report on the orbits of the small, inner Saturnian satellites, either recovered or newly discovered in recent Cassini imaging observations. The orbits presented here reflect improvements over our previously published values in that the time base of Cassini observations has been extended, and numerical orbital integrations have been performed in those cases in which simple precessing elliptical, inclined orbit solutions were found to be inadequate. Using combined Cassini and Voyager observations, we obtain an eccentricity for Pan 7 times smaller than previously reported because of the predominance of higher quality Cassini data in the fit. The orbit of the small satellite (S/2005 S1 [Daphnis]) discovered by Cassini in the Keeler gap in the outer A ring appears to be circular and coplanar; no external perturbations are appar- ent. Refined orbits of Atlas, Prometheus, Pandora, Janus, and Epimetheus are based on Cassini , Voyager, Hubble Space Telescope, and Earth-based data and a numerical integration perturbed by all the massive satellites and each other. -
Lesson 3: Moons, Rings Relationships
GETTING TO KNOW SATURN LESSON Moons, Rings, and Relationships 3 3–4 hrs Students design their own experiments to explore the fundamental force of gravity, and then extend their thinking to how gravity acts to keep objects like moons and ring particles in orbit. Students use the contexts of the Solar System and the Saturn system MEETS NATIONAL to explore the nature of orbits. The lesson SCIENCE EDUCATION enables students to correct common mis- STANDARDS: conceptions about gravity and orbits and to Science as Inquiry • Abilities learn how orbital speed decreases as the dis- Prometheus and Pandora, two of Saturn’s moons, “shepherd” necessary to Saturn’s F ring. scientific inquiry tance from the object being orbited increases. Physical Science • Motions and PREREQUISITE SKILLS BACKGROUND INFORMATION forces Working in groups Background for Lesson Discussion, page 66 Earth and Space Science Reading a chart of data Questions, page 71 • Earth in the Plotting points on a graph Answers in Appendix 1, page 225 Solar System 1–21: Saturn 22–34: Rings 35–50: Moons EQUIPMENT, MATERIALS, AND TOOLS For the teacher Materials to reproduce Photocopier (for transparencies & copies) Figures 1–10 are provided at the end of Overhead projector this lesson. Chalkboard, whiteboard, or large easel FIGURE TRANSPARENCY COPIES with paper; chalk or markers 11 21 For each group of 3 to 4 students 31 Large plastic or rubber ball 4 1 per student Paper, markers, pencils 5 1 1 per student 6 1 for teacher 7 1 (optional) 1 for teacher 8 1 per student 9 1 (optional) 1 per student 10 1 (optional) 1 for teacher 65 Saturn Educator Guide • Cassini Program website — http://www.jpl.nasa.gov/cassini/educatorguide • EG-1999-12-008-JPL Background for Lesson Discussion LESSON 3 Science as inquiry The nature of Saturn’s rings and how (See Procedures & Activities, Part I, Steps 1-6) they move (See Procedures & Activities, Part IIa, Step 3) Part I of the lesson offers students a good oppor- tunity to experience science as inquiry. -
The Pulse of the Volcano: Discovery of Episodic Activity at Prometheus on Io
Lunar and Planetary Science XXXIV (2003) 1455.pdf THE PULSE OF THE VOLCANO: DISCOVERY OF EPISODIC ACTIVITY AT PROMETHEUS ON IO. A. G. Da- vies. Jet Propulsion Laboratory-California Institute of Technology, ms 183-601, 4800 Oak Grove Drive, Pasadena, CA 91109-8099. (tel: 818-393-1775. email: [email protected]). Introduction: The temporal behaviour of thermal est e-corrected thermal emission during November 1997 output from a volcano yields valuable clues to the pro- (33 GW/µm), more than four times that seen in June cesses taking place at and beneath the surface. Galileo 1996 (orbit G1; see [3]) and Amirani showed its greatest Near Infrared Mapping Spectrometer (NIMS) data show thermal emission (up to May 1998) during May 1997 that the ionian volcanoes Prometheus and Amirani (orbit G8), nearly 100 GW/µm, nearly five times that have significant thermal emission in excess of non- seen during orbit G1. Including observations where e > volcanic background emission in every geometrically 60º, Amirani’s maximum observed 5 µm output is 291 appropriate NIMS observation. The 5 µm brightness of GW/µm (May 1998), and the Prometheus maximum is 54 these volcanoes shows considerable variation from GW/µm (May 1998). orbit to orbit. Prometheus in particular exhibits an epi- sodicity that yields valuable constraints to the mecha- x = time between peaks in months nisms of magma supply and eruption. This work is part 60 of an on-going study to chart and quantify the thermal 50 emission of Io’s volcanoes, determine mass eruption 9 rates, and note eruption style. -
Hesiod Theogony.Pdf
Hesiod (8th or 7th c. BC, composed in Greek) The Homeric epics, the Iliad and the Odyssey, are probably slightly earlier than Hesiod’s two surviving poems, the Works and Days and the Theogony. Yet in many ways Hesiod is the more important author for the study of Greek mythology. While Homer treats cer- tain aspects of the saga of the Trojan War, he makes no attempt at treating myth more generally. He often includes short digressions and tantalizes us with hints of a broader tra- dition, but much of this remains obscure. Hesiod, by contrast, sought in his Theogony to give a connected account of the creation of the universe. For the study of myth he is im- portant precisely because his is the oldest surviving attempt to treat systematically the mythical tradition from the first gods down to the great heroes. Also unlike the legendary Homer, Hesiod is for us an historical figure and a real per- sonality. His Works and Days contains a great deal of autobiographical information, in- cluding his birthplace (Ascra in Boiotia), where his father had come from (Cyme in Asia Minor), and the name of his brother (Perses), with whom he had a dispute that was the inspiration for composing the Works and Days. His exact date cannot be determined with precision, but there is general agreement that he lived in the 8th century or perhaps the early 7th century BC. His life, therefore, was approximately contemporaneous with the beginning of alphabetic writing in the Greek world. Although we do not know whether Hesiod himself employed this new invention in composing his poems, we can be certain that it was soon used to record and pass them on. -
Volcanism on Io II Eruption Plumes on Io Ionian Plumes: SO2 Source
Volcanism on Io II GLY 424/524 April 22, 2002 Eruption Plumes on Io Ionian Plumes: SO2 Source • Low gravity, atmospheric pressure • Liquid SO2 “pockets” beneath the surface • Plumes on Io ~60 - 450 km – Superheated upon contact with magma – Old Faithful would be 35 km tall on Io – Boil, erupt • Powered by SO and SO2 • Vertical crustal recycling of SO2 “snow” – Tvashtar plume detected August 2001 and “frost” deposits – 500 km tall • Most plumes from lava flow front rather – Particles determined to be SO2 “snowflakes” than vent – Interaction of hot lava with old SO2 “snow” Sulfur gas (S2 or SO2) lands on the cold surface. Atoms rearrange into (S3, S4), which give the surface a red color. Eventually, S8 forms ordinary pale yellow sulfur. 1 Io Volcanic Styles Io Volcanic Styles Continued • Promethean • Pillanian – Prometheus = type locale – Pillan = type locale • Also Amirani • Also Tvashtar • Zamama • I-31A hot-spot • Culann – Short-lived, high-effusion-rate eruptions – Long-lived, steady eruptions • Large pyroclastic deposits • Produces compound flow field • Open-channel or open-sheet flows • Takes years to decades • Associated with “wandering” plumes • Lava lakes – Extensive plume deposits – Loki = type locale – Extensive, rapidly emplace flows • Also Emakong, Pele, Tupan – High temperatures Prometheus Prometheus Prometheus Prometheus • Io’s “Old Faithful” – Active since 1979 – Observed by Voyager 1 • Eruption Plume – 80 km tall – Plume source migrated 85 km to the west since 1979 • Lava flow – ~100 km long – Apparently originates in caldera 2 Prometheus Caldera & flow-front plume Prometheus Pillan Pele & Pillan April, 1997 September, 1997 July, 1999 12 km/px 5 km/px 12 km/px Pillan ~400 km diameter Pillan eruption • http://www.digitalradiance.com/sng/Io_volc ano.htm 3 Pillan Lava flows High-res images near Pillan Patera 7.2 km long ~9 m/pixel Pillan lava flows; 19 m/px Tvashtar Bright regions are saturated pixels, indicating HOT fire- fountaining on Io Temps >1600K F.o.v. -
Observing the Universe
ObservingObserving thethe UniverseUniverse :: aa TravelTravel ThroughThrough SpaceSpace andand TimeTime Enrico Flamini Agenzia Spaziale Italiana Tokyo 2009 When you rise your head to the night sky, what your eyes are observing may be astonishing. However it is only a small portion of the electromagnetic spectrum of the Universe: the visible . But any electromagnetic signal, indipendently from its frequency, travels at the speed of light. When we observe a star or a galaxy we see the photons produced at the moment of their production, their travel could have been incredibly long: it may be lasted millions or billions of years. Looking at the sky at frequencies much higher then visible, like in the X-ray or gamma-ray energy range, we can observe the so called “violent sky” where extremely energetic fenoena occurs.like Pulsar, quasars, AGN, Supernova CosmicCosmic RaysRays:: messengersmessengers fromfrom thethe extremeextreme universeuniverse We cannot see the deep universe at E > few TeV, since photons are attenuated through →e± on the CMB + IR backgrounds. But using cosmic rays we should be able to ‘see’ up to ~ 6 x 1010 GeV before they get attenuated by other interaction. Sources Sources → Primordial origin Primordial 7 Redshift z = 0 (t = 13.7 Gyr = now ! ) Going to a frequency lower then the visible light, and cooling down the instrument nearby absolute zero, it’s possible to observe signals produced millions or billions of years ago: we may travel near the instant of the formation of our universe: 13.7 By. Redshift z = 1.4 (t = 4.7 Gyr) Credits A. Cimatti Univ. Bologna Redshift z = 5.7 (t = 1 Gyr) Credits A. -
The Temperature and Width of an Active Fissure on Enceladus
Icarus 226 (2013) 1128–1137 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus The temperature and width of an active fissure on Enceladus measured with Cassini VIMS during the 14 April 2012 South Pole flyover ⇑ Jay D. Goguen a, , Bonnie J. Buratti a, Robert H. Brown b, Roger N. Clark c, Phillip D. Nicholson d, Matthew M. Hedman d, Robert R. Howell a,e,1, Christophe Sotin a, Dale P. Cruikshank f, Kevin H. Baines a, Kenneth J. Lawrence a, John R. Spencer g, David G. Blackburn h a Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, United States b University of Arizona, Lunar and Planetary Laboratory, Tucson, AZ 85721, United States c US Geological Survey, Denver, CO 80225, United States d Astronomy Dept., Cornell University, Ithaca, NY 14853, United States e University of Wyoming, Dept. of Geology and Geophysics, Laramie, WY 82071, United States f NASA Ames Research Center, Moffett Field, CA 94035, United States g Southwest Research Institute, Boulder, CO 80302, United States h The Planetary Institute for Space Research and Technologies, Lowell, AR 72745, United States article info abstract Article history: The width and temperature of the active fissures on Saturn’s satellite Enceladus provide key observable Received 30 March 2013 constraints on physical models of these geyser-like eruptions. We analyze a sequence of high spatial res- Revised 5 July 2013 olution near-infrared spectra acquired with VIMS at 0.025 s intervals during a 74 km altitude flyover of Accepted 8 July 2013 the South Pole of Enceladus by the Cassini spacecraft on 14 April 2012 UTC. -
Diameter/Density Table of Planetary Bodies Budapest 2011
Cosmic Materials Space Research Group Eötvös Loránd University Diameter/Density table of Planetary boDies Budapest 2011 3 2 >10 >6 >5.5 >5 >4.5 >4 >3.75 >3.5 >3.25 >3 >2.75 >2.5 >2.25 >2 >1.75 >1.5 >1.25 >1 >0.75 >0.5 >0.25 >0 g/cm m Puffy 8 k Puffy 7 m WASP-17b k M HAT-P-1b m 0 171000 0.51 . 247000 0.16 . k 0 9 0 1 1130K 6 0 6 1 0 , 2-75 4 0 3 HD 209458 7 6 5 Osiris , > 1 3 > 2800K 6 187000 0.4 . 5 1 WASP-14b > 182000 5.5 . 1187K 10 165K 778.5 134K 1433 HAT-P-2b Jupiter Saturn 139000 12-14 . 142984 1.33 34% 120536 0.69 34% 0 9 0 0 2 0 8 5 , 8 8 , 6 1 6 7 > 7 > > 1650K 6 712K 4 Kepler-4b GJ 436 b 51000 2.86 . 62000 1.4 . 0 2 0 0 3 0 4 , 6 4 , 8 72K ice giant 4503 4 76K ice giant 2876 8 3 > Neptune 3 > Uranus 1500K 3 > 49528 1.64 29% 51118 1.27 30% Corot-7b 20,000 5-10 . 900K? 13 Ocean Planet 2 Mu Arae c GJ 1214 b 34000 1.8-2.5. 10M ? . 300K? 127 0 8 0 0 5 Kepler-22b 0 2 1 2 9 1 30000 ?? .? 9 1 > 1 > > 1180K 2 287K 149 735K 108 55Cnc-e Earth Venus 15000? 6? . 12742 5.51 29% 12102 5.20 90% 0 9 0 0 8 0 6 2 6 9 > 9 > > 200-340K 58 210K 228 Galilean Jupiter III Mercury Mars Ganymede 4878 5.43 12% 6792 3.93 25% 5268 1.94 43% Saturn VI 0 0 0 2 Titan 0 8 7 8 4 > 5152 1.88 22% ] 4 > > Galilean Jupiter IV m k [ Callisto R ] 4820 1.83 22% E m Galilean Jupiter I 136199 SDO 10120 T k E [ Io Moon Eris M A R 3660 3.53 63% 3474 3.35 12% ~2600 2.2-2.5 86% I D E 0 T 0 0 8 0 4 1 E 4 2 > 2 > M > A I D Uranus III Galilean Jupiter II 136108 TNO 6452 Neptune I Uranus II Saturn V Triton Titania Umbirel Rhea Europa Haumea 1576 1.71 17% 1569 3.01 67% 1960×996 2.6-3.3 1353 2.06 76% Uranus I 1169 1.4 10% 1532 1.24 94*% 134340 KBO5874 Ariel Saturn VIII 0 1162 1.66 23% 5 0 0 .