The Views from Saturn Hearing
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Migration of a Moonlet in a Ring of Solid Particles: Theory And
Migration of a moonlet in a ring of solid particles : Theory and application to Saturn’s propellers. Aur´elien Crida Department of Applied Mathematics and Theoretical Physics, University of Cambridge, Centre for Mathematical Sciences, Wilberforce Road, Cambridge CB3 0WA, UK Laboratoire Cassiop´ee, Universit´ede Nice Sophia-antipolis / CNRS / Observatoire de la Cˆote d’Azur, B.P. 4229, 06304 Nice Cedex 4, France [email protected] John C. B. Papaloizou Department of Applied Mathematics and Theoretical Physics, University of Cambridge, Centre for Mathematical Sciences, Wilberforce Road, Cambridge CB3 0WA, UK Hanno Rein Department of Applied Mathematics and Theoretical Physics, University of Cambridge, Centre for Mathematical Sciences, Wilberforce Road, Cambridge CB3 0WA, UK S´ebastien Charnoz Laboratoire AIM-UMR 7158, CEA/CNRS/Universit´eParis Diderot, IRFU/Service d’Astrophysique, CEA/Saclay, 91191 Gif-sur-Yvette Cedex, France Julien Salmon Laboratoire AIM-UMR 7158, CEA/CNRS/Universit´eParis Diderot, IRFU/Service d’Astrophysique, CEA/Saclay, 91191 Gif-sur-Yvette Cedex, France ABSTRACT Hundred meter sized objects have been identified by the Cassini spacecraft in Saturn’s A ring through the so-called “propeller” features they create in the ring. These moonlets should migrate, arXiv:1006.1573v1 [astro-ph.EP] 8 Jun 2010 due to their gravitational interaction with the ring ; in fact, some orbital variation have been detected. The standard theory of type I migration of planets in protoplanetary disks can’t be applied to the ring system, as it is pressureless. Thus, we compute the differential torque felt by a moonlet embedded in a two-dimensional disk of solid particles, with flat surface density profile, both analytically and numerically. -
Moons of Saturn National Aeronautics and Space Administration Moons of Saturn
National Aeronautics and Space Administration Moons of Saturn www.nasa.gov National Aeronautics and Space Administration Moons of Saturn www.nasa.gov Saturn, the sixth planet from the Sun, is home to a vast array of • Phoebe orbits the planet in a direction opposite that of Saturn’s • Closest Moon to Saturn Pan intriguing and unique worlds. From the cloud-shrouded surface larger moons, as do several of the recently discovered moons. Pan’s Distance from Saturn 133,583 km (83,022 mi) of Titan to crater-riddled Phoebe, each of Saturn’s moons tells • Mimas has an enormous crater on one side, the result of an • Fastest Orbit Pan another piece of the story surrounding the Saturn system. impact that nearly split the moon apart. Pan’s Orbit Around Saturn 13.8 hours Christiaan Huygens discovered the first known moon of Saturn. • Enceladus displays evidence of active ice volcanism: Cassini • Number of Moons Discovered by Voyager 3 The year was 1655 and the moon is Titan. Jean-Dominique Cas- observed warm fractures where evaporating ice evidently escapes (Atlas, Prometheus, and Pandora) sini made the next four discoveries: Iapetus (1671), Rhea (1672), and forms a huge cloud of water vapor over the south pole. • Number of Moons Discovered by Cassini (So Far) 4 Dione (1684), and Tethys (1684). Mimas and Enceladus were • Hyperion has an odd flattened shape and rotates chaotically, (Methone, Pallene, Polydeuces, and the moonlet 2005S1) both discovered by William Herschel in 1789. The next two probably due to a recent collision. discoveries came at intervals of 50 or more years — Hyperion ABOUT THE IMAGES • Pan orbits within the main rings and helps sweep materials out 1 An ultraviolet (1848) and Phoebe (1898). -
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. -
Space Exploration
S. HRG. 108–977 SPACE EXPLORATION HEARING BEFORE THE SUBCOMMITTEE ON SCIENCE, TECHNOLOGY AND SPACE OF THE COMMITTEE ON COMMERCE, SCIENCE, AND TRANSPORTATION UNITED STATES SENATE ONE HUNDRED EIGHTH CONGRESS FIRST SESSION JULY 30, 2003 Printed for the use of the Committee on Commerce, Science, and Transportation ( U.S. GOVERNMENT PRINTING OFFICE 88–583 PDF WASHINGTON : 2014 For sale by the Superintendent of Documents, U.S. Government Printing Office Internet: bookstore.gpo.gov Phone: toll free (866) 512–1800; DC area (202) 512–1800 Fax: (202) 512–2104 Mail: Stop IDCC, Washington, DC 20402–0001 VerDate Nov 24 2008 10:31 Jul 09, 2014 Jkt 075679 PO 00000 Frm 00001 Fmt 5011 Sfmt 5011 S:\GPO\DOCS\88583.TXT JACKIE SENATE COMMITTEE ON COMMERCE, SCIENCE, AND TRANSPORTATION ONE HUNDRED EIGHTH CONGRESS FIRST SESSION JOHN MCCAIN, Arizona, Chairman TED STEVENS, Alaska ERNEST F. HOLLINGS, South Carolina, CONRAD BURNS, Montana Ranking TRENT LOTT, Mississippi DANIEL K. INOUYE, Hawaii KAY BAILEY HUTCHISON, Texas JOHN D. ROCKEFELLER IV, West Virginia OLYMPIA J. SNOWE, Maine JOHN F. KERRY, Massachusetts SAM BROWNBACK, Kansas JOHN B. BREAUX, Louisiana GORDON H. SMITH, Oregon BYRON L. DORGAN, North Dakota PETER G. FITZGERALD, Illinois RON WYDEN, Oregon JOHN ENSIGN, Nevada BARBARA BOXER, California GEORGE ALLEN, Virginia BILL NELSON, Florida JOHN E. SUNUNU, New Hampshire MARIA CANTWELL, Washington FRANK R. LAUTENBERG, New Jersey JEANNE BUMPUS, Republican Staff Director and General Counsel ROBERT W. CHAMBERLIN, Republican Chief Counsel KEVIN D. KAYES, Democratic Staff Director and Chief Counsel GREGG ELIAS, Democratic General Counsel SUBCOMMITTEE ON SCIENCE, TECHNOLOGY, AND SPACE SAM BROWNBACK, Kansas, Chairman TED STEVENS, Alaska JOHN B. -
The Formation of the Martian Moons Rosenblatt P., Hyodo R
The Final Manuscript to Oxford Science Encyclopedia: The formation of the Martian moons Rosenblatt P., Hyodo R., Pignatale F., Trinh A., Charnoz S., Dunseath K.M., Dunseath-Terao M., & Genda H. Summary Almost all the planets of our solar system have moons. Each planetary system has however unique characteristics. The Martian system has not one single big moon like the Earth, not tens of moons of various sizes like for the giant planets, but two small moons: Phobos and Deimos. How did form such a system? This question is still being investigated on the basis of the Earth-based and space-borne observations of the Martian moons and of the more modern theories proposed to account for the formation of other moon systems. The most recent scenario of formation of the Martian moons relies on a giant impact occurring at early Mars history and having also formed the so-called hemispheric crustal dichotomy. This scenario accounts for the current orbits of both moons unlike the scenario of capture of small size asteroids. It also predicts a composition of disk material as a mixture of Mars and impactor materials that is in agreement with remote sensing observations of both moon surfaces, which suggests a composition different from Mars. The composition of the Martian moons is however unclear, given the ambiguity on the interpretation of the remote sensing observations. The study of the formation of the Martian moon system has improved our understanding of moon formation of terrestrial planets: The giant collision scenario can have various outcomes and not only a big moon as for the Earth. -
NASA Center for Climate Simulation: Data Supporting Science
National Aeronautics and Space Administration view Volume 6 Issue 5 NASA Center for Climate Simulation: Data Supporting Science Pg 4 Hubble Fan Gets New Crew Photo and Patch After Fire Destroys His Home Pg 8 goddard Doolittle Raider Visits Goddard Pg 12 www.nasa.gov 02 Student Project to Protect GoddardView Astronauts Wins Award Volume 6 Issue 5 By Keith Henry A NASA-sponsored student team has won the Penn State University College of Engi- Table of Contents neering Senior Design Project award for their contributions to the study of astronaut safety. The project is the culmination of undergraduate study for a bachelor’s degree in Goddard Updates industrial, electrical, mechanical, nuclear, and other engineering disciplines. Projects Student Project to Protect Astronauts Wins Award – 2 were sponsored by more than 50 different companies and organizations. NASA Celebrates Success of First TDRS with Special Event – 3 The award is judged on technical content, customer satisfaction, project manage- NASA Center for Climate Simulation: Data Supporting ment, oral presentation, and display. Nearly 100 undergraduate engineering students Science – 4 The Goddard Crater – 5 Community competed for the top prize. Celebrate Goddard Photo Gallery – 6 A five-member team from Pennsylvania State University designed and built a function- NASA Completes Critical Design Review of Landsat ing scale model of a collapsible strut, one concept being studied by NASA to absorb Data Continuity Mission – 7 excess energy upon Earth reentry for either a water or land landing. A series of these Hubble Fan Gets New Crew Photo and Patch After struts―special-purpose shock absorbers―would attach to the crew seat pallet that sup- Fires Destroys His Home – 8 ports up to six astronaut seats. -
NASA Advisory Council Science Committee Meeting, March 6-7, 2012
NASA Advisory Council Science Committee Meeting, March 6-7, 2012 Table of Contents Welcome and Introduction 3 Science Mission Directorate (SMD) 4 Planetary Science Division (PSD) 7 Astrophysics Division (APD) 9 Heliophysics Division (HPD) 12 Earth Science Division (EDP) 14 Planetary Protection 16 James Webb Space Telescope (JWST) 18 Launch Services 19 Discussion with NAC Chair 20 Discussion of findings/recommendations 20 Appendix A- Attendees Appendix B- Membership roster Appendix C- Presentations Appendix D- Agenda Prepared by Joan M. Zimmermann 2 NASA Advisory Council Science Committee Meeting, March 6-7, 2012 March 6, 2012 Welcome and Introduction Dr. Wesley Huntress, Chair for the NASA Advisory Council (NAC) Science Committee (SC) opened the meeting, welcoming the new Acting Chair for the Heliophysics Subcommittee (HPS) Robert McPherron, and William McKinnon representing the Planetary Science Subcommittee (PSS). He welcomed Dr. Barbara Giles as the newly named as Director of the Heliophysics Division (HPD). Other changes include a newly appointed Chair for the NAC, Dr. Steven Squyres, an exceptional planetary scientist, and Chair of the Steering Committee for the National Research Council’s 2011 Planetary Science Decadal Survey. Dr. John Grunsfeld has taken the place of Dr. Edward Weiler as Associate Administrator (AA) of the Science Mission Directorate (SMD). Dr. Grunsfeld is an astrophysicist and astronaut with great experience and knowledge in human spaceflight and robotic exploration. Noting that Dr. Weiler had retired abruptly in response to the FY13 budget, Dr. Huntress expressed regret at the loss of an effective AA, but was pleased to see Dr. Grunsfeld take the new position. Dr. T. -
Origin and Evolution of Saturn's Ring System
Origin and Evolution of Saturn’s Ring System Chapter 17 of the book “Saturn After Cassini-Huygens” Saturn from Cassini-Huygens, Dougherty, M.K.; Esposito, L.W.; Krimigis, S.M. (Ed.) (2009) 537-575 Sébastien CHARNOZ * Université Paris Diderot/CEA/CNRS Paris, France Luke DONES Southwest Research Institute Colorado, USA Larry W. ESPOSITO University of Colorado Colorado, USA Paul R. ESTRADA SETI Institute California, USA Matthew M. HEDMAN Cornell University New York, USA (*): to whom correspondence should be addressed : [email protected] 1 ABSTRACT: The origin and long-term evolution of Saturn’s rings is still an unsolved problem in modern planetary science. In this chapter we review the current state of our knowledge on this long- standing question for the main rings (A, Cassini Division, B, C), the F Ring, and the diffuse rings (E and G). During the Voyager era, models of evolutionary processes affecting the rings on long time scales (erosion, viscous spreading, accretion, ballistic transport, etc.) had suggested that Saturn’s rings are not older than 10 8 years. In addition, Saturn’s large system of diffuse rings has been thought to be the result of material loss from one or more of Saturn’s satellites. In the Cassini era, high spatial and spectral resolution data have allowed progress to be made on some of these questions. Discoveries such as the “propellers” in the A ring, the shape of ring-embedded moonlets, the clumps in the F Ring, and Enceladus’ plume provide new constraints on evolutionary processes in Saturn’s rings. At the same time, advances in numerical simulations over the last 20 years have opened the way to realistic models of the rings’ fine scale structure, and progress in our understanding of the formation of the Solar System provides a better-defined historical context in which to understand ring formation. -
Astro2010: the Astronomy and Astrophysics Decadal Survey
Astro2010: The Astronomy and Astrophysics Decadal Survey Notices of Interest 1. 4 m space telescope for terrestrial planet imaging and wide field astrophysics Point of Contact: Roger Angel, University of Arizona Summary Description: The proposed 4 m telescope combines capabilities for imaging terrestrial exoplanets and for general astrophysics without compromising either. Extremely high contrast imaging at very close inner working angle, as needed for terrestrial planet imaging, is accomplished by the powerful phase induced amplitude apodization method (PIAA) developed by Olivier Guyon. This method promises 10-10 contrast at 2.0 l/D angular separation, i.e. 50 mas for a 4 m telescope at 500 nm wavelength. The telescope primary mirror is unobscured with off-axis figure, as needed to achieve such high contrast. Despite the off-axis primary, the telescope nevertheless provides also a very wide field for general astrophysics. A 3 mirror anastigmat design by Jim Burge delivers a 6 by 24 arcminute field whose mean wavefront error of 12 nm rms, i.e.diffraction limited at 360 nm wavelength. Over the best 10 square arcminutes the rms error is 7 nm, for diffraction limited imaging at 200 nm wavelength. Any of the instruments can be fed by part or all of the field, by means of a flat steering mirror at the exit pupil. To allow for this, the field is curved with a radius equal to the distance from the exit pupil. The entire optical system fits in a 4 m diameter cylinder, 8 m long. Many have considered that only by using two spacecraft, a conventional on-axis telescope and a remote occulter, could high contrast and wide field imaging goals be reconciled. -
Moons and Rings
The Rings of Saturn 5.1 Saturn, the most beautiful planet in our solar system, is famous for its dazzling rings. Shown in the figure above, these rings extend far into space and engulf many of Saturn’s moons. The brightest rings, visible from Earth in a small telescope, include the D, C and B rings, Cassini’s Division, and the A ring. Just outside the A ring is the narrow F ring, shepherded by tiny moons, Pandora and Prometheus. Beyond that are two much fainter rings named G and E. Saturn's diffuse E ring is the largest planetary ring in our solar system, extending from Mimas' orbit to Titan's orbit, about 1 million kilometers (621,370 miles). The particles in Saturn's rings are composed primarily of water ice and range in size from microns to tens of meters. The rings show a tremendous amount of structure on all scales. Some of this structure is related to gravitational interactions with Saturn's many moons, but much of it remains unexplained. One moonlet, Pan, actually orbits inside the A ring in a 330-kilometer-wide (200-mile) gap called the Encke Gap. The main rings (A, B and C) are less than 100 meters (300 feet) thick in most places. The main rings are much younger than the age of the solar system, perhaps only a few hundred million years old. They may have formed from the breakup of one of Saturn's moons or from a comet or meteor that was torn apart by Saturn's gravity. -
DIRECT EVIDENCE for GRAVITATIONAL INSTABILITY and MOONLET FORMATION in SATURN’S RINGS
The Astrophysical Journal Letters, 718:L176–L180, 2010 August 1 doi:10.1088/2041-8205/718/2/L176 C 2010. The American Astronomical Society. All rights reserved. Printed in the U.S.A. DIRECT EVIDENCE FOR GRAVITATIONAL INSTABILITY AND MOONLET FORMATION IN SATURN’s RINGS K. Beurle, C. D. Murray, G. A. Williams, M. W. Evans1, N. J. Cooper, and C. B. Agnor Astronomy Unit, Queen Mary University of London, Mile End Road, London E1 4NS, UK; [email protected] Received 2010 March 3; accepted 2010 June 30; published 2010 July 14 ABSTRACT New images from the Cassini spacecraft reveal optically thick clumps, capable of casting shadows, and associated structures in regions of Saturn’s F ring that have recently experienced close passage by the adjacent moon Prometheus. Using these images and modeling, we show that Prometheus’ perturbations create regions of enhanced density and low relative velocity that are susceptible to gravitational instability and the formation of distended, yet long-lived, gravitationally coherent clumps. Subsequent collisional damping of these low-density clumps may facilitate their collapse into ∼10–20 km contiguous moonlets. The observed behavior of the F ring is analogous to the case of a marginally stable gas disk being driven to instability and collapse via perturbations from an embedded gas giant planet. Key words: instabilities – planets and satellites: dynamical evolution and stability – planets and satellites: formation – planets and satellites: rings – planet–disk interactions 1. INTRODUCTION (Murray et al. 2008; Charnoz et al. 2005; Charnoz 2009); (2) additional analysis of high-resolution Cassini images of the F Saturn’s ring system is the only local example of an astro- ring (Figure 3 of Murray et al. -
The Rings of Saturn 10
The Rings of Saturn 10 Saturn, the most beautiful planet in our solar system, is famous for its dazzling rings. Shown in the figure above, these rings extend far into space and engulf many of Saturn’s moons. The brightest rings, visible from Earth in a small telescope, include the D, C and B rings, Cassini’s Division, and the A ring. Just outside the A ring is the narrow F ring, shepherded by tiny moons, Pandora and Prometheus. Beyond that are two much fainter rings named G and E. Saturn's diffuse E ring is the largest planetary ring in our solar system, extending from Mimas' orbit to Titan's orbit, about 1 million kilometers (621,370 miles). The particles in Saturn's rings are composed primarily of water ice and range in size from microns to tens of meters. The rings show a tremendous amount of structure on all scales. Some of this structure is related to gravitational interactions with Saturn's many moons, but much of it remains unexplained. One moonlet, Pan, actually orbits inside the A ring in a 330-kilometer-wide (200-mile) gap called the Encke Gap. The main rings (A, B and C) are less than 100 meters (300 feet) thick in most places. The main rings are much younger than the age of the solar system, perhaps only a few hundred million years old. They may have formed from the breakup of one of Saturn's moons or from a comet or meteor that was torn apart by Saturn's gravity. Problem 1 – The dense main rings extend from 7,000 km to 80,000 km above Saturn's equator (Saturn's equatorial radius is 60,300 km).