The Origin of (90) Antiope from Component-Resolved Near-Infrared Spectroscopy◊
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Multiple Asteroid Systems: Dimensions and Thermal Properties from Spitzer Space Telescope and Ground-Based Observations*
Multiple Asteroid Systems: Dimensions and Thermal Properties from Spitzer Space Telescope and Ground-Based Observations* F. Marchisa,g, J.E. Enriqueza, J. P. Emeryb, M. Muellerc, M. Baeka, J. Pollockd, M. Assafine, R. Vieira Martinsf, J. Berthierg, F. Vachierg, D. P. Cruikshankh, L. Limi, D. Reichartj, K. Ivarsenj, J. Haislipj, A. LaCluyzej a. Carl Sagan Center, SETI Institute, 189 Bernardo Ave., Mountain View, CA 94043, USA. b. Earth and Planetary Sciences, University of Tennessee 306 Earth and Planetary Sciences Building Knoxville, TN 37996-1410 c. SRON, Netherlands Institute for Space Research, Low Energy Astrophysics, Postbus 800, 9700 AV Groningen, Netherlands d. Appalachian State University, Department of Physics and Astronomy, 231 CAP Building, Boone, NC 28608, USA e. Observatorio do Valongo/UFRJ, Ladeira Pedro Antonio 43, Rio de Janeiro, Brazil f. Observatório Nacional/MCT, R. General José Cristino 77, CEP 20921-400 Rio de Janeiro - RJ, Brazil. g. Institut de mécanique céleste et de calcul des éphémérides, Observatoire de Paris, Avenue Denfert-Rochereau, 75014 Paris, France h. NASA Ames Research Center, Mail Stop 245-6, Moffett Field, CA 94035-1000, USA i. NASA/Goddard Space Flight Center, Greenbelt, MD 20771, United States j. Physics and Astronomy Department, University of North Carolina, Chapel Hill, NC 27514, U.S.A * Based in part on observations collected at the European Southern Observatory, Chile Programs Numbers 70.C-0543 and ID 72.C-0753 Corresponding author: Franck Marchis Carl Sagan Center SETI Institute 189 Bernardo Ave. Mountain View CA 94043 USA [email protected] Abstract: We collected mid-IR spectra from 5.2 to 38 µm using the Spitzer Space Telescope Infrared Spectrograph of 28 asteroids representative of all established types of binary groups. -
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. -
Workshop on Analysis of Returned Comet Nucleus Samples
WORKSHOP ON Analysis of Returned Comet Nucleus Samples JANUARY 16-18,1989 MILPITAS, CALIFORNIA SPONSORED BY LUNAR AND PLANETARY INSTITUTE NASA AMES RESEARCH CENTER WORKSHOP ON Analysis of Returned Comet Nucleus Samples JANUARY 16-18, 1989 MILPITAS, CALIFORNIA SPONSORED BY LUNAR AND PLANETARY INSTITUTE NASA AMES RESEARCH CENTER Cover photo courtesy of H. U. Keller. Copyright held by Max-Planck-Jnstitut fur Aeronomie, Lindau- Katlenburg, FRG. Available from the Lunar and Planetary Institute as part of the Comet Halley image sequence ( #C3443 ). PROGRAM COMMITI'EE MEMBERS Thomas Ahrens Eberhard Gri.in California Institute of Technology Max-Planck-Institut filr Kemphysik Lou Allamandola Martha Hanner NASA Ames Research Center let Propulsion Laboratory David Blake Alan Harris (Ex Officio) NASA Ames Research Center let Propulsion Laboratory Donald Brownlee John Kerridge University of Washington University of California, Los Angeles Theodore E. Bunch Yves Langevin NASA Ames Research Center Universite de Paris, Sud Humberto Campins Larry Nyquist, Convener Planetary Science Institute NASA Johnson Space Center Sherwood Chang, Convener Gerhard Schwehm NASA Ames Research Center European Space Agency, ESTEC JeffCuzzi Paul Weissman NASA Ames Research Center Jet Propulsion Laboratory Monday. .Januacy 16th 7:00 - 8:00 a.m. Registration 8:00a.m. Welcome & Introduction to Workshop Sherwood Chang, NASA, Ames Research Center 8:10a.m. Rosetta - Comet Nucleus Sample Return Mission: Status Report Geoffrey Briggs, NASA Headquarters Dr. Marcello Coradini, European Space Agency SESSION lA Chairman: Sherwood Chang 8:30a.m. - 12:00 Noon SOURCES AND NATURE OF COMETARY COMPONENTS Invited Speaker Presentations Nuclear Synthesis and Isotopic Composition of Insteller Grains Alexander Tielens Interstellar and Cometary Dust John Mathis Refractory Solids in Chondrites and Comets: How Similar? John Wood 10:30 a.m. -
Instrumental Methods for Professional and Amateur
Instrumental Methods for Professional and Amateur Collaborations in Planetary Astronomy Olivier Mousis, Ricardo Hueso, Jean-Philippe Beaulieu, Sylvain Bouley, Benoît Carry, Francois Colas, Alain Klotz, Christophe Pellier, Jean-Marc Petit, Philippe Rousselot, et al. To cite this version: Olivier Mousis, Ricardo Hueso, Jean-Philippe Beaulieu, Sylvain Bouley, Benoît Carry, et al.. Instru- mental Methods for Professional and Amateur Collaborations in Planetary Astronomy. Experimental Astronomy, Springer Link, 2014, 38 (1-2), pp.91-191. 10.1007/s10686-014-9379-0. hal-00833466 HAL Id: hal-00833466 https://hal.archives-ouvertes.fr/hal-00833466 Submitted on 3 Jun 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Instrumental Methods for Professional and Amateur Collaborations in Planetary Astronomy O. Mousis, R. Hueso, J.-P. Beaulieu, S. Bouley, B. Carry, F. Colas, A. Klotz, C. Pellier, J.-M. Petit, P. Rousselot, M. Ali-Dib, W. Beisker, M. Birlan, C. Buil, A. Delsanti, E. Frappa, H. B. Hammel, A.-C. Levasseur-Regourd, G. S. Orton, A. Sanchez-Lavega,´ A. Santerne, P. Tanga, J. Vaubaillon, B. Zanda, D. Baratoux, T. Bohm,¨ V. Boudon, A. Bouquet, L. Buzzi, J.-L. Dauvergne, A. -
Comet Hitchhiker
Comet Hitchhiker NIAC Phase I Final Report June 30, 2015 Masahiro Ono, Marco Quadrelli, Gregory Lantoine, Paul Backes, Alejandro Lopez Ortega, H˚avard Grip, Chen-Wan Yen Jet Propulsion Laboratory, California Institute of Technology David Jewitt University of California, Los Angeles Copyright 2015. All rights reserved. Mission Concept - Pre-decisional - for Planning and Discussion Purposes Only. This research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration, and in part at University of California, Los Angeles. Comet Hitchhiker NASA Innovative Advanced Concepts Preface Yes, of course the Hitchhiker’s Guide to the Galaxy was in my mind when I came up with a concept of a tethered spacecraft hitching rides on small bodies, which I named Comet Hitchhiker. Well, this NASA-funded study is not exactly about traveling through the Galaxy; it is rather about exploring our own Solar System, which may sound a bit less exciting than visiting extraterrestrial civilizations, building a hyperspace bypass, or dining in the Restaurant at the End of the Universe. However, for the “primitive ape-descended life forms that have just begun exploring the universe merely a half century or so ago, our Solar System is still full of intellectually inspiring mysteries. So far the majority of manned and unmanned Solar System travelers solely depend on a fire breathing device called rocket, which is known to have terrible fuel efficiency. You might think there is no way other than using the gas-guzzler to accelerate or decelerate in an empty vacuum space. -
Lab Navigates First Asteroid Landing
F e b ru a ry 16, 2001 I n s i d e Volume 31 Number 4 News Briefs . 2 Leadership Transition . 3 Special Events Calendar . 2 Letters, Passings . 4 Entertainer Reaches Out . 2 Classifieds . 4 Jet Propulsion Laboratory the landing and the fact that the spacecraft is still alive and communicating with Lab Earth. NEAR Shoemaker project managers at APL said Wednesday that communications navigates with the spacecraft continue. The team will extend operations through Feb. 24 to gath- er data from the spacecraft’s gamma ray first spectrometer, which will track the abun- dance of elements on the surface of the asteroid. asteroid The NEAR Shoemaker navigation team at JPL also included Miller, Bill Owen, Mike Wang, Cliff Helfrich, Peter Antreasian and landing Steve Chesley, Eric Carranza and John Bordi. JPL’s Dr. Donald Yeomans serves as the mission’s radio science principal inves- By Martha Heil JPL navigation team made history February 12, when it guided the tigator, and JPLers Jon Giorgini and Alex and Mark Whalen Konopliv are team members. a NEAR Shoemaker spacecraft to a controlled landing on asteroid The last image from NEAR Shoemaker Eros, the first time such a maneuver has been attempted. was snapped a mere 120 meters (394 feet) from the asteroid’s surface and covers an The spacecraft, built and managed for Eros is about 32 kilometers (20 miles) area 6 meters (20 feet) wide. As NEAR NASA by the Johns Hopkins Applied across, or about the size of New York City’s Shoemaker touched down, it began send- Physics Laboratory (APL) in Laurel, Md., Manhattan Island. -
Zákryt Jasné Hvězdy Saturnem
Zákrytová a astrometrická sekce ČAS leden 2006 (1) Zajímavosti: NENECHTE SI UJÍT Zákryt jasné hv ězdy Saturnem 25. ledna 2006 ve čer mimo jiné i Evropu čeká velice zajímavá ř ě Č podívaná. Planeta Saturn okrášlená prstencem p řejde p řes relativn ě Situace, jak vypadá p i pohledu z hv zdy. asy udávané v malé vložené ě ě č jasnou hv ězdu a ze Zem ě budeme mít možnost sledovat nejen zákryt tabulce jsou platné pro Mainz (N mecko). Pro jiná místa v Evrop jsou asy v tabulce za článkem. stálice vlastní planetou, ale i její poblikávání za jednotlivými prstenci. Velice zajímavé bude jist ě pokusit se celý úkaz nahrát speciálními videokamerami v ohnisku dlouhofokálních teleobjektiv ů či dalekohled ů. Zajímavá a nevšední podívaná však čeká jist ě i na ty, kdo se na úkaz budou chtít pouze vizuáln ě podívat. Lednový zákryt hv ězdy Saturnem je jist ě zajímavou údálostí, ale nemá p říliš velkou publicitu. Úkaz bude viditelný z Evropy, Afriky a Asie. P řičemž z jižní Afriky bude možno sledovat pouze zákryty hv ězdy prstenci a zákryt vlastní planetou tuto oblast již mine. U nás, ve st řední Evrop ě, by úkaz m ěl za čít v 18:45 UT, kdy se hv ězda dostane k vn ějšímu okraji soustavy prstenc ů. V tom čase bude planeta již dostate čně vysoko nad východním obzorem (h=26°; A=92°). Zákryt Pr ůchod hv ězdy oblastí systému satelit ů planety Saturn p ři pohledu ze Země kotou čkem planety pak nastane v intervalu 20:08 UT (D – vstup) až 20:49 (R – (geocentrický pohled). -
A Low Density of 0.8 G Cm-3 for the Trojan Binary Asteroid 617 Patroclus
Publisher: NPG; Journal: Nature:Nature; Article Type: Physics letter DOI: 10.1038/nature04350 A low density of 0.8 g cm−3 for the Trojan binary asteroid 617 Patroclus Franck Marchis1, Daniel Hestroffer2, Pascal Descamps2, Jérôme Berthier2, Antonin H. Bouchez3, Randall D. Campbell3, Jason C. Y. Chin3, Marcos A. van Dam3, Scott K. Hartman3, Erik M. Johansson3, Robert E. Lafon3, David Le Mignant3, Imke de Pater1, Paul J. Stomski3, Doug M. Summers3, Frederic Vachier2, Peter L. Wizinovich3 & Michael H. Wong1 1Department of Astronomy, University of California, 601 Campbell Hall, Berkeley, California 94720, USA. 2Institut de Mécanique Céleste et de Calculs des Éphémérides, UMR CNRS 8028, Observatoire de Paris, 77 Avenue Denfert-Rochereau, F-75014 Paris, France. 3W. M. Keck Observatory, 65-1120 Mamalahoa Highway, Kamuela, Hawaii 96743, USA. The Trojan population consists of two swarms of asteroids following the same orbit as Jupiter and located at the L4 and L5 stable Lagrange points of the Jupiter–Sun system (leading and following Jupiter by 60°). The asteroid 617 Patroclus is the only known binary Trojan1. The orbit of this double system was hitherto unknown. Here we report that the components, separated by 680 km, move around the system’s centre of mass, describing a roughly circular orbit. Using this orbital information, combined with thermal measurements to estimate +0.2 −3 the size of the components, we derive a very low density of 0.8 −0.1 g cm . The components of 617 Patroclus are therefore very porous or composed mostly of water ice, suggesting that they could have been formed in the outer part of the Solar System2. -
IMPLICATIONS of ASTEROIDAL SATELLITES. W.J. Merline1 and C.R
64th Annual Meteoritical Society Meeting (2001) 5457.pdf IMPLICATIONS OF ASTEROIDAL SATELLITES. W.J. Merline1 and C.R. Chapman2, 1Southwest Research Institute ([email protected]), 2Southwest Research Institute ([email protected]) There has been a recent revolution in asteroid astron- strange objects like the highly elongated metallic ob- omy that may have important implications for meteor- ject Kleopatra and the recently discovered distant sat- ite parent bodies. In short, in the last 8 years, it has ellite of a Kuiper Belt Object, could be a remnant from been found that numerous asteroids are double bodies accretionary processes. or have small satellites orbiting about them. The first one to be discovered (the 1.8 km moonlet found by the In thinking about where meteorites come from, it Galileo spacecraft to be orbiting around 31 km-sized would help parent-body modelers to have a mental Ida during a 1993 flyby) could have been a fluke, since framework that includes the kinds of configurations the accepted theoretical perspective at the time was now being discovered and the potential processes these that such satellites would be very rare or absent. How- bodies have been through before delivering meteorites ever, we now know that at least several percent of to our collections. Certainly there are implications main-belt asteroids are binaries and that a large per- from the existence of asteroidal satellites for the char- centage of Earth-approaching asteroids are binaries. acter of rubble piles, exposure ages of asteroidal rocks, and so on. The existence of double impact craters on It is not known with certainty how these satellites are the Earth and other planets may now have a more natu- created, but it is likely to be due to several different ral explanation. -
Physical Properties of (21) Lutetia
Astronomy & Astrophysics manuscript no. Lutetia˙aa12 c ESO 2018 November 18, 2018 The triaxial ellipsoid dimensions, rotational pole, and bulk density of ESA Rosetta target asteroid (21) Lutetia ⋆ Jack D. Drummond1, A. Conrad2, W. J. Merline3, B. Carry4,5, C. R. Chapman3, H. A. Weaver6, P. M. Tamblyn3, J. C. Christou7, and C. Dumas8 1 Starfire Optical Range, Directed Energy Directorate, Air Force Research Laboratory, 3550 Aberdeen Av SE, Kirtland AFB, New Mexico 87117-5776, USA 2 W.M. Keck Observatory, 65-1120 Mamalahoa Highway, Kamuela, HI, 96743, USA 3 Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA 4 LESIA, Observatoire de Paris, 5 place Jules Janssen, 92190 MEUDON, France 5 Universit´eParis 7 Denis-Diderot, 5 rue Thomas Mann, 75205 PARIS CEDEX, France 6 Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723-6099, USA 7 Gemini Observatory, 670 N. A’ohoku Place, Hilo, Hawaii, 96720, USA 8 ESO, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago de Chile, Chile Received September 15, 1996; accepted March 16, 1997 ABSTRACT Context. Asteroid (21) Lutetia is the target of the ESA Rosetta mission flyby in 2010 July. Aims. We seek the best size estimates of the asteroid, the direction of its spin axis, and its bulk density, assuming its shape is well described by a smooth featureless triaxial ellipsoid, and to evaluate the deviations from this assumption. Methods. We derive these quantities from the outlines of the asteroid in 307 images of its resolved apparent disk obtained with adaptive optics (AO) at Keck II and VLT, and combine these with recent mass determinations to estimate a bulk density. -
The Veritas and Themis Asteroid Families: 5-14Μm Spectra with The
Icarus 269 (2016) 62–74 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus The Veritas and Themis asteroid families: 5–14 μm spectra with the Spitzer Space Telescope Zoe A. Landsman a,∗, Javier Licandro b,c, Humberto Campins a, Julie Ziffer d, Mario de Prá e, Dale P. Cruikshank f a Department of Physics, University of Central Florida, 4111 Libra Drive, PS 430, Orlando, FL 32826, United States b Instituto de Astrofísica de Canarias, C/Vía Láctea s/n, 38205, La Laguna, Tenerife, Spain c Departamento de Astrofísica, Universidad de La Laguna, E-38205, La Laguna, Tenerife, Spain d Department of Physics, University of Southern Maine, 96 Falmouth St, Portland, ME 04103, United States e Observatório Nacional, R. General José Cristino, 77 - Imperial de São Cristóvão, Rio de Janeiro, RJ 20921-400, Brazil f NASA Ames Research Center, MS 245-6, Moffett Field, CA 94035, United States article info abstract Article history: Spectroscopic investigations of primitive asteroid families constrain family evolution and composition and Received 18 October 2015 conditions in the solar nebula, and reveal information about past and present distributions of volatiles in Revised 30 December 2015 the solar system. Visible and near-infrared studies of primitive asteroid families have shown spectral di- Accepted 8 January 2016 versity between and within families. Here, we aim to better understand the composition and physical Available online 14 January 2016 properties of two primitive families with vastly different ages: ancient Themis (∼2.5 Gyr) and young Ver- Keywords: itas (∼8 Myr). We analyzed the 5 – 14 μm Spitzer Space Telescope spectra of 11 Themis-family asteroids, Asteroids including eight previously studied by Licandro et al. -
Maret Traber. Ph.D
Maret G. Traber, Ph.D. Linus Pauling Institute, 451 Linus Pauling Science Center Oregon State University Corvallis, OR 97331-6512 Phone: 541-737-7977; Fax: 541-737-5077; email: [email protected] EDUCATION Location Degree Year Major University of California, Berkeley, CA B.S. 1972 Nutrition and Food Science University of California, Berkeley, CA Ph.D. 1976 Nutrition RESEARCH AND PROFESSIONAL EXPERIENCE Year Position Institution 1972-76 Research Assistant University of California, Berkeley, CA 1976-77 Instructor of Nutrition Rutgers University, New Brunswick, NJ 1977-80 Assistant Research Scientist Department of Medicine, New York University School of Medicine, New York, NY 1980-83 Associate Research Scientist 1983-86 Research Scientist 1986-89 Research Assistant Professor 1989-93 Research Associate Professor 1994-98 Associate Research Department of Molecular & Cell Biology, Biochemist University of California, Berkeley, CA 1997-2002 Associate Research Department of Internal Medicine, Division of Critical Biochemist Care Medicine, University of California, Davis, CA 1998-present Principal Investigator Linus Pauling Institute, Oregon State University, Corvallis, OR 1998-2002 Associate Professor Department of Nutrition and Food Management Oregon State University, Corvallis, OR 1999-present Member Molecular and Cell Biology Graduate Group, Oregon State University, Corvallis, OR 2002-present Professor Nutrition Program, School of Biological & Population Health Sciences, Oregon State University, Corvallis, OR 2011-present Helen P.