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To Appear in Cometary Nuc/Ei in Space and Time, Ed. M. F. A’Hearn, ASP Conference Series, 1999
To appear in Cometary Nuc/ei in Space and Time, ed. M. F. A’Hearn, ASP Conference Series, 1999 Comet Missions in NASA’s New Millennium Program Paul R. Weissman Earth and Space Sciences Division, Jet Propulsion Laboratory, Mail stop 183-601, 4800 Oak Grove Drive, Pasadena, CA 91109 USA Abstract. NASA’s New Millennium Program (NMP) is designed to develop, test, and flight validate new, advanced technologies for plane- tary and Earth exploration missions, using a series of low cost space- craft. Such new technologies include solar-electric propulsion, inflatable- rigidizable structures, autonomous navigation and maneuvers, advanced avionics with low mass and low power requirements, and advanced sensors and concepts for science instruments. Two of NMP’s currently identified interplanetary missions include encounters with comets. The first is the Deep Space 1 mission which was launched in October, 1998 and which will fly by asteroid 1992 KD in 1999 and possibly comet Wilson-Harrington and/or comet Borrelly in 2001. The second NMP comet mission is Deep Space 4/Champollion which will be launched in April, 2003 and which will rendezvous with, orbit and land on periodic comet Tempel 1 in 2006. DS-4/Champollion is a joint project with CNES, the French space agency. 1. Introduction The advent of small, low-cost space missions has brought with it a need for new, advanced technologies which can enable productive missions with the smaller launch vehicles and payloads employed. In order to promote such technologies, NASA has created the New Millennium Program (NMP), administered by the Jet Propulsion Laboratory. New Millennium provides flight opportunities to validate new spacecraft, instrument, and operations technologies through a series of low cost missions. -
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1,. ,-- ,-- ~XECKDING PAGE BLANK WT FIL,,q DYNAMICAL EVIDENCE REGARDING THE RELATIONSHIP BETWEEN ASTEROIDS AND METEORITES GEORGE W. WETHERILL Department of Temcltricrl kgnetism ~amregie~mtittition of Washington Washington, D. C. 20025 Meteorites are fragments of small solar system bodies (comets, asteroids and Apollo objects). Therefore they may be expected to provide valuable information regarding these bodies. How- ever, the identification of particular classes of meteorites with particular small bodies or classes of small bodies is at present uncertain. It is very unlikely that any significant quantity of meteoritic material is obtained from typical ac- tive comets. Relatively we1 1-studied dynamical mechanisms exist for transferring material into the vicinity of the Earth from the inner edge of the asteroid belt on an 210~-~year time scale. It seems likely that most iron meteorites are obtained in this way, and a significant yield of complementary differec- tiated meteoritic silicate material may be expected to accom- pany these differentiated iron meteorites. Insofar as data exist, photometric measurements support an association between Apollo objects and chondri tic meteorites. Because Apol lo ob- jects are in orbits which come close to the Earth, and also must be fragmented as they traverse the asteroid belt near aphel ion, there also must be a component of the meteorite flux derived from Apollo objects. Dynamical arguments favor the hypothesis that most Apollo objects are devolatilized comet resiaues. However, plausible dynamical , petrographic, and cosmogonical reasons are known which argue against the simple conclusion of this syllogism, uiz., that chondri tes are of cometary origin. Suggestions are given for future theoretical , observational, experimental investigations directed toward improving our understanding of this puzzling situation. -
Aqueous Alteration on Main Belt Primitive Asteroids: Results from Visible Spectroscopy1
Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 1 LESIA, Observatoire de Paris, CNRS, UPMC Univ Paris 06, Univ. Paris Diderot, 5 Place J. Janssen, 92195 Meudon Pricipal Cedex, France 2 Univ. Paris Diderot, Sorbonne Paris Cit´e, 4 rue Elsa Morante, 75205 Paris Cedex 13 3 Department of Physics and Astronomy of the University of Padova, Via Marzolo 8 35131 Padova, Italy Submitted to Icarus: November 2013, accepted on 28 January 2014 e-mail: [email protected]; fax: +33145077144; phone: +33145077746 Manuscript pages: 38; Figures: 13 ; Tables: 5 Running head: Aqueous alteration on primitive asteroids Send correspondence to: Sonia Fornasier LESIA-Observatoire de Paris arXiv:1402.0175v1 [astro-ph.EP] 2 Feb 2014 Batiment 17 5, Place Jules Janssen 92195 Meudon Cedex France e-mail: [email protected] 1Based on observations carried out at the European Southern Observatory (ESO), La Silla, Chile, ESO proposals 062.S-0173 and 064.S-0205 (PI M. Lazzarin) Preprint submitted to Elsevier September 27, 2018 fax: +33145077144 phone: +33145077746 2 Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 Abstract This work focuses on the study of the aqueous alteration process which acted in the main belt and produced hydrated minerals on the altered asteroids. Hydrated minerals have been found mainly on Mars surface, on main belt primitive asteroids and possibly also on few TNOs. These materials have been produced by hydration of pristine anhydrous silicates during the aqueous alteration process, that, to be active, needed the presence of liquid water under low temperature conditions (below 320 K) to chemically alter the minerals. -
Education Employment Research Activities
Eric Quirico Curiculum Vitae Professor University Grenoble Alpes / CNRS Institut de Plan´etologieet Astrophysique de Grenoble Domaine Universitaire - BP 53 38041 Grenoble Cedex 9 - France E-mail : [email protected] Education 1992-95 : Ph. D. Thesis : Spectroscopic studies of molecular solids. Application to the study of the surfaces of Triton and Pluto. (University Joseph Fourier) 1990-91 : Master Degree in Material Sciences (Universit´eJoseph Fourier) 1987-90 : Ecole Nationale Sup´erieurede Physique de Marseille (now Ecole Centrale Marseille) 1985-87 : Classes Pr´eparatoiresaux Grandes Ecoles CPGE Sup/P' (Lyc´eeBer- thollet, Annecy - France) Employment 2010-... : Professor - University Joseph Fourier, Institut de Plan´etologieet Astro- physique de Grenoble. 2002-10 : Associate Professor - University Joseph Fourier, Laboratoire de Plan´etologiede Grenoble. 1997-01 : Associate Professor - University Paris XI, Institut d'Astrophysique Spa- tiale 1996-97 : Assistant Professor Laboratoire de Plan´etologieet G´eodynamique, Uni- versity of Nantes - France Research activities Organics in Early Solar System | Pre-accretion origin of organics, and ISM Heritage | Organics, water and minerals co-evolution in primitive asteroids | Carbon-based tracers of parent body thermal metamorphism Surface composition and evolution of small bodies, satellites | Analysis of VNIR reflectance observations | Optical properties of planetary materials and their analogs | Space weathering and surface processes My activities are essentially based on -
The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 38, NUMBER 2, A.D. 2011 APRIL-JUNE 71. LIGHTCURVES OF 10452 ZUEV, (14657) 1998 YU27, AND (15700) 1987 QD Gary A. Vander Haagen Stonegate Observatory, 825 Stonegate Road Ann Arbor, MI 48103 [email protected] (Received: 28 October) Lightcurve observations and analysis revealed the following periods and amplitudes for three asteroids: 10452 Zuev, 9.724 ± 0.002 h, 0.38 ± 0.03 mag; (14657) 1998 YU27, 15.43 ± 0.03 h, 0.21 ± 0.05 mag; and (15700) 1987 QD, 9.71 ± 0.02 h, 0.16 ± 0.05 mag. Photometric data of three asteroids were collected using a 0.43- meter PlaneWave f/6.8 corrected Dall-Kirkham astrograph, a SBIG ST-10XME camera, and V-filter at Stonegate Observatory. The camera was binned 2x2 with a resulting image scale of 0.95 arc- seconds per pixel. Image exposures were 120 seconds at –15C. Candidates for analysis were selected using the MPO2011 Asteroid Viewing Guide and all photometric data were obtained and analyzed using MPO Canopus (Bdw Publishing, 2010). Published asteroid lightcurve data were reviewed in the Asteroid Lightcurve Database (LCDB; Warner et al., 2009). The magnitudes in the plots (Y-axis) are not sky (catalog) values but differentials from the average sky magnitude of the set of comparisons. The value in the Y-axis label, “alpha”, is the solar phase angle at the time of the first set of observations. All data were corrected to this phase angle using G = 0.15, unless otherwise stated. -
IRTF Spectra for 17 Asteroids from the C and X Complexes: a Discussion of Continuum Slopes and Their Relationships to C Chondrites and Phyllosilicates ⇑ Daniel R
Icarus 212 (2011) 682–696 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus IRTF spectra for 17 asteroids from the C and X complexes: A discussion of continuum slopes and their relationships to C chondrites and phyllosilicates ⇑ Daniel R. Ostrowski a, Claud H.S. Lacy a,b, Katherine M. Gietzen a, Derek W.G. Sears a,c, a Arkansas Center for Space and Planetary Sciences, University of Arkansas, Fayetteville, AR 72701, United States b Department of Physics, University of Arkansas, Fayetteville, AR 72701, United States c Department of Chemistry and Biochemistry, University of Arkansas, Fayetteville, AR 72701, United States article info abstract Article history: In order to gain further insight into their surface compositions and relationships with meteorites, we Received 23 April 2009 have obtained spectra for 17 C and X complex asteroids using NASA’s Infrared Telescope Facility and SpeX Revised 20 January 2011 infrared spectrometer. We augment these spectra with data in the visible region taken from the on-line Accepted 25 January 2011 databases. Only one of the 17 asteroids showed the three features usually associated with water, the UV Available online 1 February 2011 slope, a 0.7 lm feature and a 3 lm feature, while five show no evidence for water and 11 had one or two of these features. According to DeMeo et al. (2009), whose asteroid classification scheme we use here, 88% Keywords: of the variance in asteroid spectra is explained by continuum slope so that asteroids can also be charac- Asteroids, composition terized by the slopes of their continua. -
(2000) Forging Asteroid-Meteorite Relationships Through Reflectance
Forging Asteroid-Meteorite Relationships through Reflectance Spectroscopy by Thomas H. Burbine Jr. B.S. Physics Rensselaer Polytechnic Institute, 1988 M.S. Geology and Planetary Science University of Pittsburgh, 1991 SUBMITTED TO THE DEPARTMENT OF EARTH, ATMOSPHERIC, AND PLANETARY SCIENCES IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY IN PLANETARY SCIENCES AT THE MASSACHUSETTS INSTITUTE OF TECHNOLOGY FEBRUARY 2000 © 2000 Massachusetts Institute of Technology. All rights reserved. Signature of Author: Department of Earth, Atmospheric, and Planetary Sciences December 30, 1999 Certified by: Richard P. Binzel Professor of Earth, Atmospheric, and Planetary Sciences Thesis Supervisor Accepted by: Ronald G. Prinn MASSACHUSES INSTMUTE Professor of Earth, Atmospheric, and Planetary Sciences Department Head JA N 0 1 2000 ARCHIVES LIBRARIES I 3 Forging Asteroid-Meteorite Relationships through Reflectance Spectroscopy by Thomas H. Burbine Jr. Submitted to the Department of Earth, Atmospheric, and Planetary Sciences on December 30, 1999 in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy in Planetary Sciences ABSTRACT Near-infrared spectra (-0.90 to ~1.65 microns) were obtained for 196 main-belt and near-Earth asteroids to determine plausible meteorite parent bodies. These spectra, when coupled with previously obtained visible data, allow for a better determination of asteroid mineralogies. Over half of the observed objects have estimated diameters less than 20 k-m. Many important results were obtained concerning the compositional structure of the asteroid belt. A number of small objects near asteroid 4 Vesta were found to have near-infrared spectra similar to the eucrite and howardite meteorites, which are believed to be derived from Vesta. -
Astronomical Observations of Volatiles on Asteroids
Astronomical Observations of Volatiles on Asteroids Andrew S. Rivkin The Johns Hopkins University Applied Physics Laboratory Humberto Campins University of Central Florida Joshua P. Emery University of Tennessee Ellen S. Howell Arecibo Observatory/USRA Javier Licandro Instituto Astrofisica de Canarias Driss Takir Ithaca College and Planetary Science Institute Faith Vilas Planetary Science Institute We have long known that water and hydroxyl are important components in meteorites and asteroids. However, in the time since the publication of Asteroids III, evolution of astronomical instrumentation, laboratory capabilities, and theoretical models have led to great advances in our understanding of H2O/OH on small bodies, and spacecraft observations of the Moon and Vesta have important implications for our interpretations of the asteroidal population. We begin this chapter with the importance of water/OH in asteroids, after which we will discuss their spectral features throughout the visible and near-infrared. We continue with an overview of the findings in meteorites and asteroids, closing with a discussion of future opportunities, the results from which we can anticipate finding in Asteroids V. Because this topic is of broad importance to asteroids, we also point to relevant in-depth discussions elsewhere in this volume. 1 Water ice sublimation and processes that create, incorporate, or deliver volatiles to the asteroid belt 1.1 Accretion/Solar system formation The concept of the “snow line” (also known as “water-frost line”) is often used in discussing the water inventory of small bodies in our solar system. The snow line is the heliocentric distance at which water ice is stable enough to be accreted into planetesimals. -
The V-Band Photometry of Asteroids from ASAS-SN
Astronomy & Astrophysics manuscript no. 40759˙ArXiV © ESO 2021 July 22, 2021 V-band photometry of asteroids from ASAS-SN Finding asteroids with slow spin ? J. Hanusˇ1, O. Pejcha2, B. J. Shappee3, C. S. Kochanek4;5, K. Z. Stanek4;5, and T. W.-S. Holoien6;?? 1 Institute of Astronomy, Faculty of Mathematics and Physics, Charles University, V Holesoviˇ ckˇ ach´ 2, 18000 Prague, Czech Republic 2 Institute of Theoretical Physics, Faculty of Mathematics and Physics, Charles University, V Holesoviˇ ckˇ ach´ 2, 18000 Prague, Czech Republic 3 Institute for Astronomy, University of Hawai’i, 2680 Woodlawn Drive, Honolulu, HI 96822, USA 4 Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA 5 Center for Cosmology and Astroparticle Physics, The Ohio State University, 191 W. Woodruff Avenue, Columbus, OH 43210, USA 6 The Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USA Received x-x-2021 / Accepted x-x-2021 ABSTRACT We present V-band photometry of the 20,000 brightest asteroids using data from the All-Sky Automated Survey for Supernovae (ASAS-SN) between 2012 and 2018. We were able to apply the convex inversion method to more than 5,000 asteroids with more than 60 good measurements in order to derive their sidereal rotation periods, spin axis orientations, and shape models. We derive unique spin state and shape solutions for 760 asteroids, including 163 new determinations. This corresponds to a success rate of about 15%, which is significantly higher than the success rate previously achieved using photometry from surveys. -
140 Siwa and 4979 Otawara
A&A 379, 660–663 (2001) Astronomy DOI: 10.1051/0004-6361:20011327 & c ESO 2001 Astrophysics The 2000 Rosetta asteroid targets observational campaign: 140 Siwa and 4979 Otawara A. Le Bras1;4, E. Dotto3, M. Fulchignoni1;2, A. Doressoundiram1,M.A.Barucci1,S.LeMou´elic4, O. Forni4, and E. Quirico4 1 DESPA, Observatoire de Paris, 5 place Jules Janssen, 92195 Meudon, France 2 UFR de Physique Universit´e Denis Diderot { Paris 7, 2 place Jussieu 75005 Paris, France 3 Osservatorio Astronomico di Torino, 10025 Pino Torinese, Italy 4 Institut d'Astrophysique Spatiale, B^at. 121, Universit´e Paris-Sud, 91405 Orsay, France Received 11 July 2001 / Accepted 18 September 2001 Abstract. Photometric and spectroscopic observations of 140 Siwa and 4979 Otawara, targets of the Rosetta mission, have been carried out at the European Southern Observatory (ESO, Chile). The complete lightcurves in V and R of both asteroids and the Siwa spectrum in the range 0.95{2.52 µm have been obtained. We determined the precise synodic rotational period of 140 Siwa (18.495 h 0.005 h) and we confirmed the synodic rotational period of 4979 Otawara (2.707 h 0.005 h). The phase function has been obtained for both asteroids, allowing the determination of the HV and GV parameters: for 4979 Otawara HV =14:62 mag, GV =0:34; for 140 Siwa HV =8:34 mag, GV =0:17. The near infrared spectrum of Siwa does not show any spectral feature, which is consistent with a C/P type object. Key words. minor planets, asteroids { solar system: general 1. -
Planetary Penetrators: Their Origins, History and Future
Author's personal copy Available online at www.sciencedirect.com Advances in Space Research 48 (2011) 403–431 www.elsevier.com/locate/asr Planetary penetrators: Their origins, history and future Ralph D. Lorenz ⇑ Johns Hopkins University, Applied Physics Laboratory, Laurel, MD 20723, USA Received 6 January 2011; received in revised form 19 March 2011; accepted 24 March 2011 Available online 30 March 2011 Abstract Penetrators, which emplace scientific instrumentation by high-speed impact into a planetary surface, have been advocated as an alter- native to soft-landers for some four decades. However, such vehicles have yet to fly successfully. This paper reviews in detail, the origins of penetrators in the military arena, and the various planetary penetrator mission concepts that have been proposed, built and flown. From the very limited data available, penetrator developments alone (without delivery to the planet) have required $30M: extensive analytical instrumentation may easily double this. Because the success of emplacement and operation depends inevitably on uncontrol- lable aspects of the target environment, unattractive failure probabilities for individual vehicles must be tolerated that are higher than the typical ‘3-sigma’ (99.5%) values typical for spacecraft. The two pathways to programmatic success, neither of which are likely in an aus- tere financial environment, are a lucky flight as a ‘piggyback’ mission or technology demonstration, or with a substantial and unprec- edented investment to launch a scientific (e.g. seismic) network mission with a large number of vehicles such that a number of terrain- induced failures can be tolerated. Ó 2011 COSPAR. Published by Elsevier Ltd. All rights reserved. -
EPSC2010-864, 2010 European Planetary Science Congress 2010 C Author(S) 2010
EPSC Abstracts Vol. 5, EPSC2010-864, 2010 European Planetary Science Congress 2010 c Author(s) 2010 Why Steins and Lutetia ? M. Fulchignoni (1,2) and M.A. Barucci (2) (1) Université Paris-Diderot, Paris 7, France, (2) LESIA, Observatoire de Paris, Meudon, France, ([email protected] / Fax: +33-145077144) Abstract Few weeks before the scheduled launch date, due to some problem of the launcher, ESA decided to The criteria in choosing the asteroid fly-by targets of postpone the launch of at least one year to allow the Rosetta mission, 2786 Steins and 21 Lutetia, are Ariane to fix the problem. This decision implied a recalled and discussed. global revision of the mission targets. The new target The ratio (discoveries)/(confirmed information) is comet, P/67 Churimov-Gerasimenko, was chosen analyzed on the light of the results obtained during during 2003, and the new trajectory was more each fly-by. expensive, in terms of ΔV, than the that toward The role of the new close observations of these small Wirtanen. So, the decision concerning the asteroid bodies in providing valuable “ground truth” for the targets was postponed after the completion of the interpretation of data on a large sample of asteroids manoeuvre of interplanetary orbit insertion of the obtained from both the Earth surface and in orbit Rosetta probe, in order to check if some hydrazine observatories is also outlined. would have been still available for the one or two fly- bys. We ware starting another campaign of ground based observations of a group of asteroids that the 1.