Rings Under Close Encounters with the Giant Planets: Chariklo Vs Chiron
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Surface Characteristics of Transneptunian Objects and Centaurs from Photometry and Spectroscopy
Barucci et al.: Surface Characteristics of TNOs and Centaurs 647 Surface Characteristics of Transneptunian Objects and Centaurs from Photometry and Spectroscopy M. A. Barucci and A. Doressoundiram Observatoire de Paris D. P. Cruikshank NASA Ames Research Center The external region of the solar system contains a vast population of small icy bodies, be- lieved to be remnants from the accretion of the planets. The transneptunian objects (TNOs) and Centaurs (located between Jupiter and Neptune) are probably made of the most primitive and thermally unprocessed materials of the known solar system. Although the study of these objects has rapidly evolved in the past few years, especially from dynamical and theoretical points of view, studies of the physical and chemical properties of the TNO population are still limited by the faintness of these objects. The basic properties of these objects, including infor- mation on their dimensions and rotation periods, are presented, with emphasis on their diver- sity and the possible characteristics of their surfaces. 1. INTRODUCTION cally with even the largest telescopes. The physical char- acteristics of Centaurs and TNOs are still in a rather early Transneptunian objects (TNOs), also known as Kuiper stage of investigation. Advances in instrumentation on tele- belt objects (KBOs) and Edgeworth-Kuiper belt objects scopes of 6- to 10-m aperture have enabled spectroscopic (EKBOs), are presumed to be remnants of the solar nebula studies of an increasing number of these objects, and signifi- that have survived over the age of the solar system. The cant progress is slowly being made. connection of the short-period comets (P < 200 yr) of low We describe here photometric and spectroscopic studies orbital inclination and the transneptunian population of pri- of TNOs and the emerging results. -
Distant Ekos: 2011 HL103, 2011 KW48, 2012 VR113, 2013 QO95, 2013 QP95 and 4 New Centaur/SDO Discoveries: 2011 JD32, 2012 VS113, 2013 TV158, 2014 OG392
Issue No. 94 August 2014 r✤✜ s ✓✏ DISTANT EKO ❞✐ ✒✑ The Kuiper Belt Electronic Newsletter ✣✢ Edited by: Joel Wm. Parker [email protected] www.boulder.swri.edu/ekonews CONTENTS News & Announcements ................................. 2 Abstracts of 5 Accepted Papers ......................... 3 Newsletter Information .............................. .....7 1 NEWS & ANNOUNCEMENTS There were 5 new TNO discoveries announced since the previous issue of Distant EKOs: 2011 HL103, 2011 KW48, 2012 VR113, 2013 QO95, 2013 QP95 and 4 new Centaur/SDO discoveries: 2011 JD32, 2012 VS113, 2013 TV158, 2014 OG392 Reclassified objects: 2013 LU28 (Centaur → SDO) Deleted/Re-identified objects: 2014 LJ9 = 2013 LU28 Current number of TNOs: 1277 (including Pluto) Current number of Centaurs/SDOs: 401 Current number of Neptune Trojans: 9 Out of a total of 1687 objects: 646 have measurements from only one opposition 629 of those have had no measurements for more than a year 326 of those have arcs shorter than 10 days (for more details, see: http://www.boulder.swri.edu/ekonews/objects/recov_stats.jpg) 2 PAPERS ACCEPTED TO JOURNALS Photometric and Spectroscopic Evidence for a Dense Ring System around Centaur Chariklo R. Duffard1, N. Pinilla-Alonso2, J.L. Ortiz1, A. Alvarez-Candal3, B. Sicardy4, P. Santos-Sanz1, N. Morales1, C. Colazo5, E. Fern´andez-Valenzuela1, and F. Braga-Ribas1 1 Instituto de Astrofisica de Andalucia - CSIC. Glorieta de la Astronom´ıa s/n. Granada. 18008. Spain 2 Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN, 37996-1410, USA 3 Observatorio Nacional de Rio de Janeiro, Rio de Janeiro, Brazil 4 LESIA-Observatoire de Paris, CNRS, UPMC Univ. Paris 6, Univ. -
The Journey of Typhon-Echidna As a Binary System Through the Planetary
MNRAS 476, 5323–5331 (2018) doi:10.1093/mnras/sty583 Advance Access publication 2018 March 6 The journey of Typhon-Echidna as a binary system through the planetary Downloaded from https://academic.oup.com/mnras/article-abstract/476/4/5323/4923085 by Universidade Estadual Paulista J�lio de Mesquita Filho user on 19 June 2019 region R. A. N. Araujo,1 M. A. Galiazzo,2‹ O. C. Winter1 and R. Sfair1 1UNESP-Sao˜ Paulo State University, Grupo de Dinamicaˆ Orbital e Planetologia, CEP 12516-410 Guaratingueta,´ SP, Brazil 2Institute of Astrophysics, University of Vienna, A-1180 Vienna, Austria Accepted 2018 February 23. Received 2018 February 22; in original form 2017 August 20 ABSTRACT Among the current population of the 81 known trans-Neptunian binaries (TNBs), only two are in orbits that cross the orbit of Neptune. These are (42355) Typhon-Echidna and (65489) Ceto-Phorcys. In this work, we focused our analyses on the temporal evolution of the Typhon- Echidna binary system through the outer and inner planetary systems. Using numerical inte- grations of the N-body gravitational problem, we explored the orbital evolutions of 500 clones of Typhon, recording the close encounters of those clones with planets. We then analysed the effects of those encounters on the binary system. It was found that only ≈22 per cent of the encounters with the giant planets were strong enough to disrupt the binary. This binary system has an ≈3.6 per cent probability of reaching the terrestrial planetary region over a time-scale of approximately 5.4 Myr. Close encounters of Typhon-Echidna with Earth and Venus were also registered, but the probabilities of such events occurring are low (≈0.4 per cent). -
Size Distribution of Particles in Saturn's Rings from Aggregation And
Size distribution of particles in Saturn’s rings from aggregation and fragmentation Nikolai Brilliantov ∗, P. L. Krapivsky †, Anna Bodrova ‡§, Frank Spahn § , Hisao Hayakawa ¶, Vladimir Stadnichuk ‡ , and Jurgen¨ Schmidt k § ∗University of Leicester, Leicester, United Kingdom,†Department of Physics, Boston University, Boston, USA,‡Moscow State University, Moscow, Russia,§University of Potsdam, Potsdam, Germany,¶Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto, Japan, and kAstronomy and Space Physics, University of Oulu, Oulu, Finland Submitted to Proceedings of the National Academy of Sciences of the United States of America Saturn’s rings consist of a huge number of water ice particles, as observed in Saturn’s rings, is universal for systems where a with a tiny addition of rocky material. They form a flat disk, as balance between aggregation and disruptive collisions is steadily the result of an interplay of angular momentum conservation and sustained. Hence, the same size distribution is expected for any the steady loss of energy in dissipative inter-particle collisions. ring system where collisions play a role, like the Uranian rings, the For particles in the size range from a few centimeters to a few q recently discovered rings of Chariklo and Chiron, and possibly meters, a power-law distribution of radii, r− with q 3, has been inferred; for larger sizes, the distribution∼ has a steep≈ cutoff. rings around extrasolar objects. It has been suggested that this size distribution may arise from a balance between aggregation and fragmentation of ring particles, yet neither the power-law dependence nor the upper size cutoff Results and Discussion have been established on theoretical grounds. -
A Portrait of Centaur 10199 Chariklo
A&A 501, 777–784 (2009) Astronomy DOI: 10.1051/0004-6361/200911660 & c ESO 2009 Astrophysics A portrait of Centaur 10199 Chariklo A. Guilbert1, M. A. Barucci1, R. Brunetto2, A. Delsanti1, F. Merlin1,3, A. Alvarez-Candal1, S. Fornasier1,4, C. de Bergh1, and G. Sarid5 1 LESIA, Observatoire de Paris - Section Meudon, 2 Place J. Janssen, 92195 Meudon Principal Cedex, France e-mail: [email protected] 2 Institut d’Astrophysique Spatiale, UMR-8617, Université Paris-Sud, bâtiment 121, 91405 Orsay Cedex, France 3 Department of Astronomy, University of Maryland, College Park, MD 20742, USA 4 Université Paris 7 - Denis Diderot, Paris, France 5 Department of Geophysics and Planetary Sciences, Sackler Faculty of Exact Sciences, Tel Aviv University, Ramat Aviv, Israel Received 14 January 2009 / Accepted 14 April 2009 ABSTRACT Context. An ESO Large Program was undertaken in October 2006 (P.I.: M. A. Barucci) to provide as complete observations as possible of about 40 Trans-Neptunian Objects and Centaurs, to investigate their surface properties. Hence, new visible and near- infrared observations of Centaur 10199 Chariklo (1997 CU26)) were performed. Aims. We investigate Chariklo’s surface composition. It has already been suspected of being inhomogeneous. We try to confirm this assumption by comparing our results with previously published works, and find an explanation related the observed variations. Methods. A spectral modeling is applied to the spectra, using different types of mixtures, to place constraints on the amount of water ice present in our new spectrum. Several spectra, obtained at different moments by different groups, are compared by studying the variations in the depth of absorption bands attributable to water ice. -
Colours of Minor Bodies in the Outer Solar System II - a Statistical Analysis, Revisited
Astronomy & Astrophysics manuscript no. MBOSS2 c ESO 2012 April 26, 2012 Colours of Minor Bodies in the Outer Solar System II - A Statistical Analysis, Revisited O. R. Hainaut1, H. Boehnhardt2, and S. Protopapa3 1 European Southern Observatory (ESO), Karl Schwarzschild Straße, 85 748 Garching bei M¨unchen, Germany e-mail: [email protected] 2 Max-Planck-Institut f¨ur Sonnensystemforschung, Max-Planck Straße 2, 37 191 Katlenburg- Lindau, Germany 3 Department of Astronomy, University of Maryland, College Park, MD 20 742-2421, USA Received —; accepted — ABSTRACT We present an update of the visible and near-infrared colour database of Minor Bodies in the outer Solar System (MBOSSes), now including over 2000 measurement epochs of 555 objects, extracted from 100 articles. The list is fairly complete as of December 2011. The database is now large enough that dataset with a high dispersion can be safely identified and rejected from the analysis. The method used is safe for individual outliers. Most of the rejected papers were from the early days of MBOSS photometry. The individual measurements were combined so not to include possible rotational artefacts. The spectral gradient over the visible range is derived from the colours, as well as the R absolute magnitude M(1, 1). The average colours, absolute magnitude, spectral gradient are listed for each object, as well as their physico-dynamical classes using a classification adapted from Gladman et al., 2008. Colour-colour diagrams, histograms and various other plots are presented to illustrate and in- vestigate class characteristics and trends with other parameters, whose significance are evaluated using standard statistical tests. -
Polarimetric Properties of Transneptunian Objects and Centaurs
Polarimetry of Centaurs (2060) Chiron, (5145) Pholus and (10199) Chariklo I. N. Belskaya1,2, S. Bagnulo3, M.A. Barucci2, K. Muinonen4,5, G.P. Tozzi6, S. Fornasier2,7, L. Kolokolova8 1Institute of Astronomy, Kharkiv National University, 35 Sumska str., 61022 Kharkiv, Ukraine, [email protected] 2LESIA, Observatoire de Paris, 5, pl.Jules Janssen, 92195 Meudon cedex, France 3Armagh Observatory, College Hill, Armagh BT61 9DG, Northern Ireland, United Kingdom 4 Department of Physics, University of Helsinki, P.O. Box 64, Gustaf Hällströmin katu 2a, FI-00014, Finland 5Finnish Geodetic Institute, P.O. Box 15, Geodeetinrinne 2, FI-02431 Masala, Finland 6INAF - Oss. Astrofisico di Arcetri, Largo E. Fermi 5, I-50125 Firenze, Italy 7University of Denis Diderot -Paris VII, France 8University of Maryland, College Park, MD, USA Published in Icarus 210, p.472-479, 2010 http://www.sciencedirect.com/science/article/pii/S0019103510002277 * Based on observations made with ESO Very Large Telescope at the La Silla-Paranal Observatory under programme ID 178.C-0036 (PI: A. Barucci) Pages: 18 Tables: 3 Figures: 8 Abstract Results of the first polarimetric observations of Centaurs (5145) Pholus and (10199) Chariklo, and new observations of (2060) Chiron are presented together with the estimates of their absolute magnitudes. Observations were carried out at the 8 m ESO Very Large Telescope in 2007-2008. They revealed noticeable negative polarization in the phase angle range 0.5-4.4 deg with a minimum varying from -1% to -2.1% in the R band. All three objects show diverse polarization phase angle behaviour, each distinctly different from that of transneptunian objects. -
EPSC2017-96, 2017 European Planetary Science Congress 2017 Eeuropeapn Planetarsy Science Ccongress C Author(S) 2017
EPSC Abstracts Vol. 11, EPSC2017-96, 2017 European Planetary Science Congress 2017 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2017 First results from stellar occultations in the “GAIA era” G. Benedetti-Rossi (1,2,3) ([email protected]), R. Vieira-Martins (1,2), B. Sicardy (4), the Rio Group, the “Lucky Star” Occultation Team, and the Granada Occultation Team (1) Observatório Nacional/MCTIC, Brazil (2) Laboratório Interinstitucional de e-Astronomia (LineA), Brazil, (3) INCT do e-Universo/CNPq (4) Observatoire de Paris-Meudon, France Abstract presence of atmosphere, and also about the immediate neighborhoods of distant solar system Stellar occultation is a powerful technique to study bodies. distant solar system bodies. It allows high angular resolution of the occulting body from the analysis of Stellar occultations by Pluto, (10199) Chariklo, a light curve acquired with high temporal resolution. (136108) Haumea, among many other objects are In the past few years, this technique is showing already in the list of the observed objects in the impressive results such as the determination of “GAIA era”. Pluto's atmosphere with uncertainties comparable to the New Horizons probe[1], the discovery of rings 2. Summary and Conclusions around the Centaur object (10199) Chariklo[2], or the detection of a chasm on a Trans-Neptunian Object The GAIA mission (together with other surveys, such (2003 AZ84)[3], among others. After the first release as the LSST) should provide accurate predictions of of the GAIA catalog (in October/2016), stellar stellar occultations by tens of thousands of distant occultations predictions became much more accurate, small solar system bodies in the next years. -
Transneptunian Object Taxonomy 181
Fulchignoni et al.: Transneptunian Object Taxonomy 181 Transneptunian Object Taxonomy Marcello Fulchignoni LESIA, Observatoire de Paris Irina Belskaya Kharkiv National University Maria Antonietta Barucci LESIA, Observatoire de Paris Maria Cristina De Sanctis IASF-INAF, Rome Alain Doressoundiram LESIA, Observatoire de Paris A taxonomic scheme based on multivariate statistics is proposed to distinguish groups of TNOs having the same behavior concerning their BVRIJ colors. As in the case of asteroids, the broadband spectrophotometry provides a first hint about the bulk compositional properties of the TNOs’ surfaces. Principal components (PC) analysis shows that most of the TNOs’ color variability can be accounted for by a single component (i.e., a linear combination of the col- ors): All the studied objects are distributed along a quasicontinuous trend spanning from “gray” (neutral color with respect to those of the Sun) to very “red” (showing a spectacular increase in the reflectance of the I and J bands). A finer structure is superimposed to this trend and four homogeneous “compositional” classes emerge clearly, and independently from the PC analy- sis, if the TNO sample is analyzed with a grouping technique (the G-mode statistics). The first class (designed as BB) contains the objects that are neutral in color with respect to the Sun, while the RR class contains the very red ones. Two intermediate classes are separated by the G mode: the BR and the IR, which are clearly distinguished by the reflectance relative increases in the R and I bands. Some characteristics of the classes are deduced that extend to all the objects of a given class the properties that are common to those members of the class for which more detailed data are available (observed activity, full spectra, albedo). -
Characterization of Asteroids and Tnos Authors: T
Small Bodies Near and Far (SBNAF): Characterization of asteroids and TNOs Authors: T. G. Müller1, A. Marciniak2, Cs. Kiss3, R. Duffard4, V. Alí-Lagoa1, P. Bartczak2, M. Butkiewicz- Bąk2, G. Dudziński2, E. Fernández-Valenzuela4, G. Marton3, N. Morales4, J.-L. Ortiz4, D. Oszkiewicz2, T. Santana-Ros2, P. Santos-Sanz4, R. Szakáts3, A. Takácsné Farkas3, E. Varga-Verebélyi3 1: MPI für Extraterrestrische Physik (MPE), Garching, Germany. 2: Astronomical Observatory Institute (UAM), Poznań, Poland. 3: Konkoly Observatory, Budapest, Hungary. 4: Instituto de Astrofísica de Andalucía (IAA) - CSIC, Granada, Spain. Abstract: We present results from an EU Horizon2020-funded benchmark study (2016-2019) that addresses critical points in reconstructing physical and thermal prop- erties of near-Earth, main-belt, and trans-Neptunian objects. The combination of the visual and thermal data from the ground and from astrophysics space missions is key to improving the scientific understanding of these objects. The development of new tools is crucial for the interpretation of much larger data sets, but also for the operations and scientific exploitation of interplanetary missions. We combine different methods and techniques to get full information on selected bodies: lightcurve inversion, stellar occultations, thermophysical modeling, radiometric methods, radar ranging and adaptive optics imaging. The applications to objects with ground- truth information from interplanetary missions Hayabusa, NEAR-Shoemaker, Rosetta, and DAWN allow us to advance the techniques beyond the current state-of-the- art and to assess the limitations of each method. We present our recently developed tools, services, products, deliverables, and list important SBNAF publications. Results I: Tools & Services • ISAM service (http://isam.astro.amu.edu.pl/) contains shape models for more than 900 asteroids. -
EPSC2010-156, 2010 European Planetary Science Congress 2010 C Author(S) 2010
EPSC Abstracts Vol. 5, EPSC2010-156, 2010 European Planetary Science Congress 2010 c Author(s) 2010 Polarimetric properties of transneptunian objects and Centaurs from the VLT Large Programme I.N. Belskaya (1,2), S. Bagnulo (3), M.A. Barucci (2), K. Muinonen (4,5), G.P. Tozzi (6), S. Fornasier (2,7), L. Kolokolova (8) (1) Institute of Astronomy, Kharkiv National University, Ukraine ([email protected]), (2) LESIA, Observatoire de Paris, France, (3) Armagh Observatory, United Kingdom, (4) Department of Physics, University of Helsinki, Finland, (5) Finnish Geodetic Institute, Masala, Finland, (6) INAF - Oss. Astrofisico di Arcetri, Firenze, Italy, (7) University of Denis Diderot -Paris VII, France, (8) University of Maryland, USA. measure 8 objects selected on the basis of two main Abstract m criteria: (1) R-filter brightness mR<21 to enable Polarimetric observations of 3 Centaurs and 5 polarimetry with observational error ~0.05% in less transneptunian objects (TNOs) carried out within the than 2 hours of telescope time; and (2) diversity of VLT Large Programme (VLT-LP) show that, first, all physical and dynamical properties of the sample objects display negative polarization at small phase objects. Measurements of linear polarization were angles whose minimum values varied from -0.3% to carried out with the FORS1 instrument in the R filter. -2.2%; second, even a single polarization A detailed description of the methods of observations measurement at a phase angle larger than 1º can and reduction can be found in [1]. The objects discriminate between a high-albedo and a low-albedo observed are given in Table 1 together with the surface; third, polarimetric properties of Centaurs are orbital type, taxonomy, and the range of phase angles more diverse than those of TNOs; and, fourth, covered by the observations. -
On the Origin of the Ring System of (10199) Chariklo
On the origin of the ring system of (10199) Chariklo M. D. Melita1, Duffard, R.2, Ortiz J.L.2 [email protected] 1 IAFE (UBA-CONICET) y FCAG (UNLP). 2 Instituto de Astrof´ısica de Andaluc´ıa (CSIC). Granada. Espana.˜ Melita et al. Fof 2016. – p. 1 Layout Astrophysical Background: . (10199) Chariklo . The Centaurs . (10199) Chariklo Ring System Formation scenarios: . Classical Roche limit & Tidal evolution . Material ejected by a collision on the body of the asteoriod . Breakup of a satellite of (10199) Chariklo due to a catastrophic collision . Cometary-like activity (Pan & Wu 2016, arXiv:1602.01769) . Discussion Melita et al. Fof 2016. – p. 2 Centaur asteroids Melita et al. Fof 2016. – p. 3 The Centaurs Features and Peculiarities . It is a transitinal population (Levison & Duncan 1997) with dynamical lifetimes between the planets of ∼ 104 − 105 yr. The observed surface properties are not a simple juxtaposition of the properties of the bodies at the origin (TNOs) or as end-states (JFCs), i.e. The color distribution is bimodal (Tegler & Romanishin 2003, Melita & Licandro 2012), as observed in small TNOs (Peixinho 2014). Cometary-like comas have been observed on some members. e.g. (2060) Chiron, sometimes attributed to phase changes of water-ice (Jewitt 2009). Only class of asteroids where rings have been detected. Melita et al. Fof 2016. – p. 4 (10199) Chariklo . H = 6.6 . mV = 18.5 . p = 4.5 % . a = 15.75 AU . e = 0.15 . i=23deg . R1 = R2 = 122 km . R3 = 117 km . M(ρ = 1g/cm3)= 7 1018 kg . Colors: | B-V | = 0.86 (Grey) Melita et al.