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A Deeper Look at the Colors of the Saturnian Irregular Satellites Arxiv
A deeper look at the colors of the Saturnian irregular satellites Tommy Grav Harvard-Smithsonian Center for Astrophysics, MS51, 60 Garden St., Cambridge, MA02138 and Instiute for Astronomy, University of Hawaii, 2680 Woodlawn Dr., Honolulu, HI86822 [email protected] James Bauer Jet Propulsion Laboratory, California Institute of Technology 4800 Oak Grove Dr., MS183-501, Pasadena, CA91109 [email protected] September 13, 2018 arXiv:astro-ph/0611590v2 8 Mar 2007 Manuscript: 36 pages, with 11 figures and 5 tables. 1 Proposed running head: Colors of Saturnian irregular satellites Corresponding author: Tommy Grav MS51, 60 Garden St. Cambridge, MA02138 USA Phone: (617) 384-7689 Fax: (617) 495-7093 Email: [email protected] 2 Abstract We have performed broadband color photometry of the twelve brightest irregular satellites of Saturn with the goal of understanding their surface composition, as well as their physical relationship. We find that the satellites have a wide variety of different surface colors, from the negative spectral slopes of the two retrograde satellites S IX Phoebe (S0 = −2:5 ± 0:4) and S XXV Mundilfari (S0 = −5:0 ± 1:9) to the fairly red slope of S XXII Ijiraq (S0 = 19:5 ± 0:9). We further find that there exist a correlation between dynamical families and spectral slope, with the prograde clusters, the Gallic and Inuit, showing tight clustering in colors among most of their members. The retrograde objects are dynamically and physically more dispersed, but some internal structure is apparent. Keywords: Irregular satellites; Photometry, Satellites, Surfaces; Saturn, Satellites. 3 1 Introduction The satellites of Saturn can be divided into two distinct groups, the regular and irregular, based on their orbital characteristics. -
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. -
Reddy Saturn's Small Wonders Astronomy 46 No 03 (2018)-1.Pdf
Saturn’s small wonders Usually known for its rings, the Saturn system is also home to some of our solar system’s most intriguing moons. by Francis Reddy Above: NASA’s Cassini mission took images as the spacecraft approached ye candy is not in short supply at Saturn. and Calypso orbit along with Tethys — an (left) and departed (right) For visitors who tire of watching the plan- arrangement thus far unseen among any other Saturn’s moon Phoebe et’s stormy atmosphere or gazing into the moons in the solar system. during its only close flyby of the satellite. Cassini solar system’s most beautiful and complex And this is just for starters. “The Saturn sys- passed just 1,285 miles ring system, there's always the giant satel- tem is full of surprises,” says Paul Schenk, a plan- (2,068 km) above the lite Titan to explore. This colossal moon etary geologist at the Lunar and Planetary surface on June 11, 2004. is bigger than Mercury and sports a hazy Institute in Houston. There’s a satellite that likely Phoebe is thought to be a centaur that might have orange atmosphere denser than Earth’s, originated in the Kuiper Belt, the storehouse of become a Jupiter-family producing methane rains that flow across icy bodies beyond Neptune’s orbit; a piebald comet, had Saturn not Titan’s icy landscape and pool into vast lakes. moon nearly encircled by an equatorial ridge captured it. NASA/JPL-CALTECH But look again. Even Saturn’s small moons containing some of the tallest mountains in the display some unusual dynamic relationships. -
Accretion of Saturn's Mid-Sized Moons During the Viscous
Accretion of Saturn’s mid-sized moons during the viscous spreading of young massive rings: solving the paradox of silicate-poor rings versus silicate-rich moons. Sébastien CHARNOZ *,1 Aurélien CRIDA 2 Julie C. CASTILLO-ROGEZ 3 Valery LAINEY 4 Luke DONES 5 Özgür KARATEKIN 6 Gabriel TOBIE 7 Stephane MATHIS 1 Christophe LE PONCIN-LAFITTE 8 Julien SALMON 5,1 (1) Laboratoire AIM, UMR 7158, Université Paris Diderot /CEA IRFU /CNRS, Centre de l’Orme les Merisiers, 91191, Gif sur Yvette Cedex France (2) Université de Nice Sophia-antipolis / C.N.R.S. / Observatoire de la Côte d'Azur Laboratoire Cassiopée UMR6202, BP4229, 06304 NICE cedex 4, France (3) Jet Propulsion Laboratory, California Institute of Technology, M/S 79-24, 4800 Oak Drive Pasadena, CA 91109 USA (4) IMCCE, Observatoire de Paris, UMR 8028 CNRS / UPMC, 77 Av. Denfert-Rochereau, 75014, Paris, France (5) Department of Space Studies, Southwest Research Institute, Boulder, Colorado 80302, USA (6) Royal Observatory of Belgium, Avenue Circulaire 3, 1180 Uccle, Bruxelles, Belgium (7) Université de Nantes, UFR des Sciences et des Techniques, Laboratoire de Planétologie et Géodynamique, 2 rue de la Houssinière, B.P. 92208, 44322 Nantes Cedex 3, France (8) SyRTE, Observatoire de Paris, UMR 8630 du CNRS, 77 Av. Denfert-Rochereau, 75014, Paris, France (*) To whom correspondence should be addressed ([email protected]) 1 ABSTRACT The origin of Saturn’s inner mid-sized moons (Mimas, Enceladus, Tethys, Dione and Rhea) and Saturn’s rings is debated. Charnoz et al. (2010) introduced the idea that the smallest inner moons could form from the spreading of the rings’ edge while Salmon et al. -
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 -
Spectropolarimetry of the Two Faces of Saturn's Moon Iapetus
Spectropolarimetry of the two faces of Saturn’s moon Iapetus C. Ejeta1, H. Böhnhardt1, S. Bagnulo2, G. P. Tozzi3, K. Muinonen4 1. Max-Planck-Institut für Sonnensystemforschung, katlenburg-Lindau 2. Armagh Observatory, N. Ireland, UK 3. INAF – OSS. Astrofisico di Arcetri, Frienze, Italy 4. Department of Physics, University of Helsinki, Finland Outlines • Polarimetry of Galilean satellites of Jupiter • Iapetus Observing Program • Method of performing linear spectropolarimetry • Conclusions and Outlook Polarimetry of Galilean Satellites Mishchenko et al, 2010, in Polarimetric remote sensing of SSOs (book) Io: ==> has a surface of partly absorbing crystals believed to be resulted from evaporates released from mantle. ==> Pure water frost is not likely to be present. Europa: ==> has a water frost dominated surface. Ganymede: ==> has an alternating frosted areas, mostly composed of water, with interstitial dark terrain most probably of a rocky nature. Galilean Satellites --- Callisto Leading hemisphere: ==> covered mostly by a layer of pulverized rocks, of the “regolith” type . Trailing hemisphere: ==> covered mostly by rock or gravel free of fine regolithic powder . Rosenbush, Icarus, 2002 Polarimetry of Saturn’s B ring & Iapetus Rosenbush et al. JQSRT, 2006 Rosenbush et al., 2002, in Optics of cosmic dust (book) ==> deposits of aggregates and sub-micrometer-sized icy particles on its surface. Iapetus Iapetus Observing Program Western Bright Eastern Dark Date α (in deg.) Date α(in deg.) 2009/04/03 2.7 2009/05/13 5.7 2009/06/22 6.0 2010/01/11 5.7 2010/02/18 3.3 2010/03/30 0.9 2010/05/07 4.5 2010/06/16 6.1 2010/07/27 5.1 2011/02/14 4.6 2011/01/05 5.9 2011/05/03 3.0 2011/03/25 1.1 2011/07/21 5.8 2011/06/10 5.6 2011/12/31 5.5 2011/12/01 5.5 2012/03/19 2.9 2012/02/08 5.5 2012/06/05 4.7 2012/04/26 1.2 2012/08/24 4.8 2012/07/14 6.0 2013/02/02 5.7 2013/03/13 4.3 2013/04/22 0.7 2013/05/30 3.2 2013/07/09 5.6 2013/08/18 5.6 Method FORS2 at the ESO VLT Schematic concept of spectro-polarimetry Method…. -
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 ............................................................................... -
The Habitability of Icy Exomoons
University of Groningen Master thesis Astronomy The habitability of icy exomoons Supervisor: Author: Prof. Floris F.S. Van Der Tak Jesper N.K.Y. Tjoa Dr. Michael \Migo" Muller¨ June 27, 2019 Abstract We present surface illumination maps, tidal heating models and melting depth models for several icy Solar System moons and use these to discuss the potential subsurface habitability of exomoons. Small icy moons like Saturn's Enceladus may maintain oceans under their ice shells, heated by en- dogenic processes. Under the right circumstances, these environments might sustain extraterrestrial life. We investigate the influence of multiple orbital and physical characteristics of moons on the subsurface habitability of these bodies and model how the ice melting depth changes. Assuming a conduction only model, we derive an analytic expression for the melting depth dependent on seven- teen physical and orbital parameters of a hypothetical moon. We find that small to mid-sized icy satellites (Enceladus up to Uranus' Titania) locked in an orbital resonance and in relatively close orbits to their host planet are best suited to sustaining a subsurface habitable environment, and may do so largely irrespective of their host's distance from the parent star: endogenic heating is the primary key to habitable success, either by tidal heating or radiogenic processes. We also find that the circumplanetary habitable edge as formulated by Heller and Barnes (2013) might be better described as a manifold criterion, since the melting depth depends on seventeen (more or less) free parameters. We conclude that habitable exomoons, given the right physical characteristics, may be found at any orbit beyond the planetary habitable zone, rendering the habitable zone for moons (in principle) arbitrarily large. -
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 …………………………………………………………………. -
Saturn's Moon Iapetus Is the Yin-Yang of the Solar System 13 September 2007
Saturn's moon Iapetus is the yin-yang of the solar system 13 September 2007 Images returned late Tuesday and early Wednesday show a surface that is heavily cratered, along with the mountain ridge that runs along the moon's equator. Many of the close-up observations focused on studying the strange 20-km high mountain ridge that gives the moon a walnut- shaped appearance. "The images are really stunning," said Tilmann Denk, Cassini imaging scientist at the Free University in Berlin, Germany, who was responsible for the imaging observation planning. "Every new picture contained its own charm. I was most pleased about the images showing huge mountains rising over the horizon. I knew about this scenic viewing opportunity for more than seven years, and now the real images have suddenly materialised." This flyby was nearly 100 times closer to Iapetus than Cassini's 2004 flyby, bringing the spacecraft to Cassini zooms in, for the first time, on the patchy, bright about 1640 km from the surface. The moon's and dark mountains on Saturn's two-toned moon, irregular walnut shape, the mountain ridge that lies Iapetus. The mountains were originally identified in images from the NASA Voyager spacecraft taken more almost directly on the equator and Iapetus’ than 25 years earlier. The image was acquired during brightness contrast are among the key mysteries Cassini's only close flyby of Iapetus. The terrain seen scientists are trying to solve. here is located on the equator of Iapetus at approximately 199° West, in the transition region "There is never a dull moment on this mission," between the moon's bright and dark hemispheres. -
Rotation Periods of Irregular Satellites of Saturn
EPSC Abstracts Vol. 6, EPSC-DPS2011-1452, 2011 EPSC-DPS Joint Meeting 2011 c Author(s) 2011 Rotation Periods of Irregular Satellites of Saturn T. Denk (1), S. Mottola (2), Th. Roatsch (2), H. Rosenberg (1), and G. Neukum (1) (1) FU Berlin, Germany ([email protected]), (2) DLR Berlin, Germany Abstract ~60x to ~240x closer to the objects than the Earth is, and long duration observations are possible because Rotation periods of six irregular moons of Saturn there is no 24-h day/night cycle at Cassini. Dis- have been measured as follows: Siarnaq ~06:40 h; advantages are the relatively small telescope mirror Ymir ~07:20 h; Albiorix 13:19±0:08 h; Bebhionn of the Cassini ISS camera (0.17 m), the smaller field- ~16 h; Paaliaq ~19 h; Kiviuq 21:49±0:13 h (Tab. 1). of-view of the ISS resulting in a significantly higher pointing accuracy requirement, and the inability of doing image quality checks and exposure parameter 1. Introduction adaptations during data acquisition. We observe irregular moons of Saturn with the Imaging Experiment (ISS) of the Cassini spacecraft 2. Results [1]. Motivation is the determination of basic properties of these objects like rotation periods, polar Measured rotation periods for seven satellites are axes orientations, object sizes and shapes, phase shown in Tab. 1. The values vary significantly: curves, colors, or the search for binaries. This might While Siarnaq, with a period of ~6 h 40 min., rotates allow a better understanding of the impact history in relatively fast, Kiviuq needs almost 22 h for one the saturnian system including the question about the day/night cycle. -
Iapetus' Geophysics: Rotation Rate, Shape, and Equatorial Ridge
Icarus 190 (2007) 179–202 www.elsevier.com/locate/icarus Iapetus’ geophysics: Rotation rate, shape, and equatorial ridge J.C. Castillo-Rogez a,∗,D.L.Matsona,C.Sotina,b, T.V. Johnson a, J.I. Lunine c, P.C. Thomas d a Jet Propulsion Laboratory, California Institute of Technology, M/S 230-260, 4800 Oak Grove Drive, Pasadena, CA 91109, USA b UMR – CNRS 6112 Laboratoire de planétologie et géodynamique de Nantes, 2, rue de la Houssinière, 44322 Nantes Cedex 3, France c Lunar and Planetary Laboratory, 1629 E. University Blvd., Tucson, AZ 85721-0092, USA d Department of Astronomy, Cornell University, 422 Space Sciences Building, Ithaca, NY 14853, USA Received 23 July 2006; revised 30 January 2007 Available online 28 March 2007 Abstract Iapetus has preserved evidence that constrains the modeling of its geophysical history from the time of its accretion until now. The evidence is (a) its present 79.33-day rotation or spin rate, (b) its shape that corresponds to the equilibrium figure for a hydrostatic body rotating with a period of ∼16 h, and (c) its high, equatorial ridge, which is unique in the Solar System. This paper reports the results of an investigation into the coupling between Iapetus’ thermal and orbital evolution for a wide range of conditions including the spatial distributions with time of composition, porosity, short-lived radioactive isotopes (SLRI), and temperature. The thermal model uses conductive heat transfer with temperature-dependent conductivity. Only models with a thick lithosphere and an interior viscosity in the range of about the water ice melting point can explain the observed shape.