An Automatic Approach to Exclude Interlopers from Asteroid Families
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I Corpi Minori Del Sistema Solare
UNIVERSITA' DEGLI STUDI DI BOLOGNA FACOLTA' DI SCIENZE MATEMATICHE, FISICHE E NATURALI Dipartimento di Astronomia Corso di Laurea in Astronomia Materia di Tesi: Astronomia I CORPI MINORI DEL SISTEMA SOLARE Tesi di Laurea di: Relatore: CLAUDIO ELIDORO Chiar.mo Prof. CORRADO BARTOLINI Sessione Autunnale Anno Accademico 1995 - 1996 INDICE INTRODUZIONE 1. UNA VISIONE D'INSIEME 3 2. L'ORIGINE DEL SISTEMA SOLARE 7 3. METODOLOGIE OSSERVATIVE DEI CORPI MINORI 14 PARTE PRIMA: GLI ASTEROIDI 1. NOTA STORICA 17 2. ORIGINE DEGLI ASTEROIDI 19 3. IL RUOLO DEGLI IMPATTI 25 4. FAMIGLIE DINAMICHE 31 5. CLASSIFICAZIONE 39 6. "INCONTRI RAVVICINATI" 48 951 GASPRA 49 243 IDA 52 433 EROS ED I N.E.A. 54 4179 TOUTATIS 61 7. LA TERRA COME BERSAGLIO 65 PARTE SECONDA: LE COMETE 1. NOTA STORICA 81 2. ORIGINE ED EVOLUZIONE 2.1 LA NUBE DI OORT E LA FASCIA DI KUIPER 82 2.2 LE COMETE A CORTO PERIODO 88 2.3 FASI EVOLUTIVE FINALI 94 3. MORFOLOGIA E FENOMENI FISICI CONNESSI 3.1 IL MODELLO DI WHIPPLE 100 3.2 IL NUCLEO 107 3.3 LA CHIOMA 111 3.4 LA CODA 116 PARTE TERZA: KUIPER-BELT OBJECTS 1. NOTA STORICA 119 2. IL SISTEMA PLUTONE - CARONTE 124 3. CHIRONE ED I CENTAURI 128 4. UNA POPOLAZIONE TUTTA DA SCOPRIRE 134 BIBLIOGRAFIA 139 - 2 - INTRODUZIONE 1. UNA VISIONE D'INSIEME Scorrendo le tappe fondamentali della Storia dell'Astronomia, appare evidente come il quadro complessivo del Sistema Solare si sia gradualmente modificato e ampliato man mano che la ricerca e la tecnologia mettevano a disposizione strumenti di indagine più adeguati. -
Asteroid Family Ages. 2015. Icarus 257, 275-289
Icarus 257 (2015) 275–289 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Asteroid family ages ⇑ Federica Spoto a,c, , Andrea Milani a, Zoran Knezˇevic´ b a Dipartimento di Matematica, Università di Pisa, Largo Pontecorvo 5, 56127 Pisa, Italy b Astronomical Observatory, Volgina 7, 11060 Belgrade 38, Serbia c SpaceDyS srl, Via Mario Giuntini 63, 56023 Navacchio di Cascina, Italy article info abstract Article history: A new family classification, based on a catalog of proper elements with 384,000 numbered asteroids Received 6 December 2014 and on new methods is available. For the 45 dynamical families with >250 members identified in this Revised 27 April 2015 classification, we present an attempt to obtain statistically significant ages: we succeeded in computing Accepted 30 April 2015 ages for 37 collisional families. Available online 14 May 2015 We used a rigorous method, including a least squares fit of the two sides of a V-shape plot in the proper semimajor axis, inverse diameter plane to determine the corresponding slopes, an advanced error model Keywords: for the uncertainties of asteroid diameters, an iterative outlier rejection scheme and quality control. The Asteroids best available Yarkovsky measurement was used to estimate a calibration of the Yarkovsky effect for each Asteroids, dynamics Impact processes family. The results are presented separately for the families originated in fragmentation or cratering events, for the young, compact families and for the truncated, one-sided families. For all the computed ages the corresponding uncertainties are provided, and the results are discussed and compared with the literature. The ages of several families have been estimated for the first time, in other cases the accu- racy has been improved. -
1950 Da, 205, 269 1979 Va, 230 1991 Ry16, 183 1992 Kd, 61 1992
Cambridge University Press 978-1-107-09684-4 — Asteroids Thomas H. Burbine Index More Information 356 Index 1950 DA, 205, 269 single scattering, 142, 143, 144, 145 1979 VA, 230 visual Bond, 7 1991 RY16, 183 visual geometric, 7, 27, 28, 163, 185, 189, 190, 1992 KD, 61 191, 192, 192, 253 1992 QB1, 233, 234 Alexandra, 59 1993 FW, 234 altitude, 49 1994 JR1, 239, 275 Alvarez, Luis, 258 1999 JU3, 61 Alvarez, Walter, 258 1999 RL95, 183 amino acid, 81 1999 RQ36, 61 ammonia, 223, 301 2000 DP107, 274, 304 amoeboid olivine aggregate, 83 2000 GD65, 205 Amor, 251 2001 QR322, 232 Amor group, 251 2003 EH1, 107 Anacostia, 179 2007 PA8, 207 Anand, Viswanathan, 62 2008 TC3, 264, 265 Angelina, 175 2010 JL88, 205 angrite, 87, 101, 110, 126, 168 2010 TK7, 231 Annefrank, 274, 275, 289 2011 QF99, 232 Antarctic Search for Meteorites (ANSMET), 71 2012 DA14, 108 Antarctica, 69–71 2012 VP113, 233, 244 aphelion, 30, 251 2013 TX68, 64 APL, 275, 292 2014 AA, 264, 265 Apohele group, 251 2014 RC, 205 Apollo, 179, 180, 251 Apollo group, 230, 251 absorption band, 135–6, 137–40, 145–50, Apollo mission, 129, 262, 299 163, 184 Apophis, 20, 269, 270 acapulcoite/ lodranite, 87, 90, 103, 110, 168, 285 Aquitania, 179 Achilles, 232 Arecibo Observatory, 206 achondrite, 84, 86, 116, 187 Aristarchus, 29 primitive, 84, 86, 103–4, 287 Asporina, 177 Adamcarolla, 62 asteroid chronology function, 262 Adeona family, 198 Asteroid Zoo, 54 Aeternitas, 177 Astraea, 53 Agnia family, 170, 198 Astronautica, 61 AKARI satellite, 192 Aten, 251 alabandite, 76, 101 Aten group, 251 Alauda family, 198 Atira, 251 albedo, 7, 21, 27, 185–6 Atira group, 251 Bond, 7, 8, 9, 28, 189 atmosphere, 1, 3, 8, 43, 66, 68, 265 geometric, 7 A- type, 163, 165, 167, 169, 170, 177–8, 192 356 © in this web service Cambridge University Press www.cambridge.org Cambridge University Press 978-1-107-09684-4 — Asteroids Thomas H. -
Size–Frequency Distributions of Fragments from SPH/N-Body Simulations of Asteroid Impacts: Comparison with Observed Asteroid Families
Icarus 186 (2007) 498–516 www.elsevier.com/locate/icarus Size–frequency distributions of fragments from SPH/N-body simulations of asteroid impacts: Comparison with observed asteroid families Daniel D. Durda a,∗, William F. Bottke Jr. a, David Nesvorný a, Brian L. Enke a, William J. Merline a, Erik Asphaug b, Derek C. Richardson c a Southwest Research Institute, 1050 Walnut Street, Suite 400, Boulder, CO 80302, USA b Earth Sciences Department, University of California Santa Cruz, Santa Cruz, CA 95064, USA c Department of Astronomy, University of Maryland, College Park, MD 20742, USA Received 12 May 2006; revised 1 September 2006 Available online 28 November 2006 Abstract We investigate the morphology of size–frequency distributions (SFDs) resulting from impacts into 100-km-diameter parent asteroids, repre- sented by a suite of 161 SPH/N-body simulations conducted to study asteroid satellite formation [Durda, D.D., Bottke, W.F., Enke, B.L., Merline, W.J., Asphaug, E., Richardson, D.C., Leinhardt, Z.M., 2004. Icarus 170, 243–257]. The spherical basalt projectiles range in diameter from 10 to 46 km (in equally spaced mass increments in logarithmic space, covering six discrete sizes), impact speeds range from 2.5 to 7 km/s (generally in ◦ ◦ ◦ 1km/s increments), and impact angles range from 15 to 75 (nearly head-on to very oblique) in 15 increments. These modeled SFD morpholo- gies match very well the observed SFDs of many known asteroid families. We use these modeled SFDs to scale to targets both larger and smaller than 100 km in order to gain insights into the circumstances of the impacts that formed these families. -
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. -
Size-Dependent Modification of Asteroid Family Yarkovsky V-Shapes
Astronomy & Astrophysics manuscript no. ModifiedVshape˙v7˙revised c ESO 2018 March 6, 2018 Size-dependent modification of asteroid family Yarkovsky V-shapes B. T. Bolin1;2;3, A. Morbidelli1, and K. J. Walsh4 1 Laboratoire Lagrange, Universite´ Coteˆ d’Azur, Observatoire de la Coteˆ d’Azur, CNRS, Blvd. de l’Observatoire, CS 34229, 06304 Nice cedex 4, France e-mail: [bryce.bolin;morby;marco.delbo]@oca.eu 2 Department of Astronomy, University of Washington, 3910 15th Ave NE, Seattle, WA 98195 3 B612 Asteroid Institute, 20 Sunnyside Ave, Suite 427, Mill Valley, CA, 94941, United States 4 Southwest Research Institute, 1050 Walnut St. Suite 300, Boulder, CO 80302, United States e-mail: [email protected] Preprint online version: March 6, 2018 ABSTRACT Context. The thermal properties of the surfaces of asteroids determine the magnitude of the drift rate cause by the Yarkovsky force. In the general case of Main Belt asteroids, the Yarkovsky force is indirectly proportional to the thermal inertia, Γ. Aims. Following the proposed relationship between Γ and asteroid diameter D, we find that asteroids’ Yarkovsky drift rates might have a more complex size dependence than previous thought, leading to a curved family V-shape boundary in semi-major axis, a, vs. 1/D space. This implies that asteroids are drifting faster at larger sizes than previously considered decreasing on average the known ages of asteroid families. Methods. The V-Shape curvature is determined for >25 families located throughout the Main Belt to quantify the Yarkovsky size- dependent drift rate. Results. We find that there is no correlation between family age and V-shape curvature. -
Asteroidal Source of L Chondrite Meteorites ∗ David Nesvorný A, , David Vokrouhlický A,B, Alessandro Morbidelli A,C, William F
ARTICLE IN PRESS YICAR:8854 JID:YICAR AID:8854 /SCO [m5G; v 1.79; Prn:12/02/2009; 11:10] P.1 (1-4) Icarus ••• (••••) •••–••• Contents lists available at ScienceDirect Icarus www.elsevier.com/locate/icarus Note Asteroidal source of L chondrite meteorites ∗ David Nesvorný a, , David Vokrouhlický a,b, Alessandro Morbidelli a,c, William F. Bottke a a Department of Space Studies, Southwest Research Institute, 1050 Walnut St., Suite 300, Boulder, CO 80302, USA b Institute of Astronomy, Charles University, V Holešoviˇckách2,CZ-18000,Prague8,CzechRepublic c Observatoire de la Côte d’Azur, Boulevard de l’Observatoire, B.P. 4229, 06304 Nice Cedex 4, France article info abstract Article history: Establishing connections between meteorites and their parent asteroids is an important goal of planetary science. Received 28 July 2008 Several links have been proposed in the past, including a spectroscopic match between basaltic meteorites and (4) Revised 19 November 2008 Vesta, that are helping scientists understand the formation and evolution of the Solar System bodies. Here we show Accepted 11 December 2008 that the shocked L chondrite meteorites, which represent about two thirds of all L chondrite falls, may be fragments Available online xxxx of a disrupted asteroid with orbital semimajor axis a = 2.8 AU. This breakup left behind thousands of identified 1– 15 km asteroid fragments known as the Gefion family. Fossil L chondrite meteorites and iridium enrichment found Keywords: in an ≈467 Ma old marine limestone quarry in southern Sweden, and perhaps also ∼5 large terrestrial craters Meteorites with corresponding radiometric ages, may be tracing the immediate aftermath of the family-forming collision when Asteroids numerous Gefion fragments evolved into the Earth-crossing orbits by the 5:2 resonance with Jupiter. -
Pairs and Groups of Asteroids with Nearest Orbits in Known Families
Pairs and groups of asteroids with nearest orbits in known families Rosaev A.E. NPC Nedra, Yaroslavl, Russia Abstract: The problem of origin and age of asteroid families studied very intensively. First of all youngest families are interesting due to possibility of the reconstruction collisional history. But in oldest families present objects with very close orbits some of them are products of recent collisions. The search for and studying of dynamics of such pairs of orbits is a main aim of the present paper. In result, two new young groups of minor planets are detected as well as some new members of known families. The problem of origin and age of asteroid families studied in many publications. First of all youngest and compact minor planets clusters are interesting due to possibility of the reconstruction collisional history. The search for of such pairs or groups of orbits is a main aim of the present paper. The list of orbital elements of 415000 asteroids with permanent numbers from the catalogue [1] on data 15 Dec 2014 is used. The method of selection of nearest orbits is similar to used in [2]. Due to very high sensitivity to variation of angular elements, this method has an advantage in detecting first of all low velocity and most recent breakups. We use osculating orbital elements instead proper elements by similar reason – our target is search for low velocity and most recent breakups The clusters of close orbits with 3 or more members have a particular interest. In this case, we can say about new compact young family, was born in a low-velocity breakup. -
A Taxonomic Study of Asteroid Families from Kmtnet-Saao Multi-Band Photometry
Draft version March 20, 2019 Typeset using LATEX default style in AASTeX61 A TAXONOMIC STUDY OF ASTEROID FAMILIES FROM KMTNET-SAAO MULTI-BAND PHOTOMETRY N. Erasmus,1 A. McNeill,2 M. Mommert,3 D. E. Trilling,2, 1 A. A. Sickafoose,1, 4 and K. Paterson5 1South African Astronomical Observatory, Cape Town, 7925, South Africa. 2Department of Physics and Astronomy, Northern Arizona University, Flagstaff, AZ 86001, USA. 3Lowell Observatory, 1400 W. Mars Hill Rd., Flagstaff, AZ, 86001, USA 4Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139-4307, USA. 5Department of Astronomy, University of Cape Town, Cape Town, 7701, South Africa ABSTRACT We present here multi-band photometry for over 2000 Main-belt asteroids. For each target we report the probabilistic taxonomy using the measured V-R and V-I colors in combination with a machine-learning generated decision surface in color-color space. Through this method we classify >85% of our targets as one the four main Bus-DeMeo complexes: S-, C-, X-, or D-type. Roughly one third of our targets have a known associated dynamic family with 69 families represented in our data. Within uncertainty our results show no discernible difference in taxonomic distribution between family members and non-family members. Nine of the 69 families represented in our observed sample had 20 or more members present and therefore we investigate the taxonomy of these families in more detail and find excellent agreement with literature. Out of these 9 well-sampled families, our data show that the Themis, Koronis, Hygiea, Massalia, and Eunomia families display a high degree of taxonomic homogeneity and that the Vesta, Flora, Nysa-Polana, and Eos families show a significant level of mixture in taxonomies. -
Satellite Dynamics and Space Missions: Theory and Applications of Celestial Mechanics S
Satellite Dynamics and Space Missions: Theory and Applications of Celestial Mechanics S. Martino al Cimino, 27 August - 2 September 2017 Space missions for minor-body science Andrea Milani Department of Mathematics, University of Pisa PLAN of LECTURES 1. Self presentation and method 2. Mission design and implementation: a difficult process 3. Case A: ROSETTA, cometary mission 4. Case B: MORO, a proposed lunar mission 5. Why so many asteroid missions? 6. Case C: DON QUIXOTE, a proposed deflection experiment 7. Asteroid families, proper elements, and asteroid ground truth 8. Case D: DAWN, rendez-vous asteroids mission 9. Next asteroid missions: LUCY, PSYCHE 1 1.1 Self presentation Old persons have plenty of memories. The challenge is to select the important ones, not just for the old, but for the next generations. The challenge for the young listeners is to be receptive, but critical: do not do as we did in our times, but learn lessons to apply in innovative ways to the new experiences. In the early sixties I was a teenager with some very passionate interests, including exploration of space: these were the times of the first human spaceflights, and of the race for the moon. I also liked computers, not accessible to me, but I did study my first programming language, FORTRAN. In 1976 I was aged 28 and already with a tenured position (Assistant of Mathe- matical Analysis) in the University of Pisa. However, my research career in pure Mathematics was going nowhere. Then, following the advice of A. Nobili and P. Farinella, I attended the lectures by Giuseppe (Bepi) Colombo at SNS. -
Asteroid Family Physical Properties, Numerical Sim- Constraints on the Ages of Families
Asteroid Family Physical Properties Joseph R. Masiero NASA Jet Propulsion Laboratory/Caltech Francesca DeMeo Harvard/Smithsonian Center for Astrophysics Toshihiro Kasuga Planetary Exploration Research Center, Chiba Institute of Technology Alex H. Parker Southwest Research Institute An asteroid family is typically formed when a larger parent body undergoes a catastrophic collisional disruption, and as such family members are expected to show physical properties that closely trace the composition and mineralogical evolution of the parent. Recently a number of new datasets have been released that probe the physical properties of a large number of asteroids, many of which are members of identified families. We review these data sets and the composite properties of asteroid families derived from this plethora of new data. We also discuss the limitations of the current data, and the open questions in the field. 1. INTRODUCTION techniques that rely on simulating the non-gravitational forces that depend on an asteroid’s albedo, diameter, and Asteroid families provide waypoints along the path of density. dynamical evolution of the solar system, as well as labo- In Asteroids III, Zappala` et al. (2002) and Cellino et ratories for studying the massive impacts that were com- al. (2002) reviewed the physical and spectral properties mon during terrestrial planet formation. Catastrophic dis- (respectively) of asteroid families known at that time. Zap- ruptions shattered these asteroids, leaving swarms of bod- pala` et al. (2002) primarily dealt with asteroid size distri- ies behind that evolved dynamically under gravitational per- butions inferred from a combination of observed absolute turbations and the Yarkovsky effect to their present-day lo- H magnitudes and albedo assumptions based on the subset cations, both in the Main Belt and beyond. -
Updated on 1 September 2018
20813 Aakashshah 12608 Aesop 17225 Alanschorn 266 Aline 31901 Amitscheer 30788 Angekauffmann 2341 Aoluta 23325 Arroyo 15838 Auclair 24649 Balaklava 26557 Aakritijain 446 Aeternitas 20341 Alanstack 8651 Alineraynal 39678 Ammannito 11911 Angel 19701 Aomori 33179 Arsenewenger 9117 Aude 16116 Balakrishnan 28698 Aakshi 132 Aethra 21330 Alanwhitman 214136 Alinghi 871 Amneris 28822 Angelabarker 3810 Aoraki 29995 Arshavsky 184535 Audouze 3749 Balam 28828 Aalamiharandi 1064 Aethusa 2500 Alascattalo 108140 Alir 2437 Amnestia 129151 Angelaboggs 4094 Aoshima 404 Arsinoe 4238 Audrey 27381 Balasingam 33181 Aalokpatwa 1142 Aetolia 19148 Alaska 14225 Alisahamilton 32062 Amolpunjabi 274137 Angelaglinos 3400 Aotearoa 7212 Artaxerxes 31677 Audreyglende 20821 Balasridhar 677 Aaltje 22993 Aferrari 200069 Alastor 2526 Alisary 1221 Amor 16132 Angelakim 9886 Aoyagi 113951 Artdavidsen 20004 Audrey-Lucienne 26634 Balasubramanian 2676 Aarhus 15467 Aflorsch 702 Alauda 27091 Alisonbick 58214 Amorim 30031 Angelakong 11258 Aoyama 44455 Artdula 14252 Audreymeyer 2242 Balaton 129100 Aaronammons 1187 Afra 5576 Albanese 7517 Alisondoane 8721 AMOS 22064 Angelalewis 18639 Aoyunzhiyuanzhe 1956 Artek 133007 Audreysimmons 9289 Balau 22656 Aaronburrows 1193 Africa 111468 Alba Regia 21558 Alisonliu 2948 Amosov 9428 Angelalouise 90022 Apache Point 11010 Artemieva 75564 Audubon 214081 Balavoine 25677 Aaronenten 6391 Africano 31468 Albastaki 16023 Alisonyee 198 Ampella 25402 Angelanorse 134130 Apaczai 105 Artemis 9908 Aue 114991 Balazs 11451 Aarongolden 3326 Agafonikov 10051 Albee