Physical Properties of B-Type Asteroids from WISE Data⋆
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ESO's VLT Sphere and DAMIT
ESO’s VLT Sphere and DAMIT ESO’s VLT SPHERE (using adaptive optics) and Joseph Durech (DAMIT) have a program to observe asteroids and collect light curve data to develop rotating 3D models with respect to time. Up till now, due to the limitations of modelling software, only convex profiles were produced. The aim is to reconstruct reliable nonconvex models of about 40 asteroids. Below is a list of targets that will be observed by SPHERE, for which detailed nonconvex shapes will be constructed. Special request by Joseph Durech: “If some of these asteroids have in next let's say two years some favourable occultations, it would be nice to combine the occultation chords with AO and light curves to improve the models.” 2 Pallas, 7 Iris, 8 Flora, 10 Hygiea, 11 Parthenope, 13 Egeria, 15 Eunomia, 16 Psyche, 18 Melpomene, 19 Fortuna, 20 Massalia, 22 Kalliope, 24 Themis, 29 Amphitrite, 31 Euphrosyne, 40 Harmonia, 41 Daphne, 51 Nemausa, 52 Europa, 59 Elpis, 65 Cybele, 87 Sylvia, 88 Thisbe, 89 Julia, 96 Aegle, 105 Artemis, 128 Nemesis, 145 Adeona, 187 Lamberta, 211 Isolda, 324 Bamberga, 354 Eleonora, 451 Patientia, 476 Hedwig, 511 Davida, 532 Herculina, 596 Scheila, 704 Interamnia Occultation Event: Asteroid 10 Hygiea – Sun 26th Feb 16h37m UT The magnitude 11 asteroid 10 Hygiea is expected to occult the magnitude 12.5 star 2UCAC 21608371 on Sunday 26th Feb 16h37m UT (= Mon 3:37am). Magnitude drop of 0.24 will require video. DAMIT asteroid model of 10 Hygiea - Astronomy Institute of the Charles University: Josef Ďurech, Vojtěch Sidorin Hygiea is the fourth-largest asteroid (largest is Ceres ~ 945kms) in the Solar System by volume and mass, and it is located in the asteroid belt about 400 million kms away. -
The Impact Crater at the Origin of the Julia Family Detected with VLT/SPHERE??,?? P
A&A 618, A154 (2018) Astronomy https://doi.org/10.1051/0004-6361/201833477 & © ESO 2018 Astrophysics The impact crater at the origin of the Julia family detected with VLT/SPHERE??,?? P. Vernazza1, M. Brož2, A. Drouard1, J. Hanuš2, M. Viikinkoski3, M. Marsset4, L. Jorda1, R. Fetick1, B. Carry5, F. Marchis6, M. Birlan7, T. Fusco1, T. Santana-Ros8, E. Podlewska-Gaca8,9, E. Jehin10, M. Ferrais10, P. Bartczak8, G. Dudzinski´ 8, J. Berthier7, J. Castillo-Rogez11, F. Cipriani12, F. Colas7, C. Dumas13, J. Durechˇ 2, M. Kaasalainen3, A. Kryszczynska8, P. Lamy1, H. Le Coroller1, A. Marciniak8, T. Michalowski8, P. Michel5, M. Pajuelo7,14, P. Tanga5, F. Vachier7, A. Vigan1, B. Warner15, O. Witasse12, B. Yang16, E. Asphaug17, D. C. Richardson18, P. Ševecekˇ 2, M. Gillon10, and Z. Benkhaldoun19 1 Aix-Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille), Marseille, France e-mail: [email protected] 2 Institute of Astronomy, Charles University, Prague, V Holešovickᡠch 2, 18000, Prague 8, Czech Republic 3 Department of Mathematics, Tampere University of Technology, PO Box 553, 33101 Tampere, Finland 4 Astrophysics Research Centre, Queen’s University Belfast, BT7 1NN, UK 5 Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, 06304 Nice Cedex 4, France 6 SETI Institute, Carl Sagan Center, 189 Bernado Avenue, Mountain View CA 94043, USA 7 IMCCE, Observatoire de Paris, 77 avenue Denfert-Rochereau, 75014 Paris Cedex, France 8 Astronomical Observatory Institute, Faculty of Physics, Adam Mickiewicz University, -
The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 36, NUMBER 3, A.D. 2009 JULY-SEPTEMBER 77. PHOTOMETRIC MEASUREMENTS OF 343 OSTARA Our data can be obtained from http://www.uwec.edu/physics/ AND OTHER ASTEROIDS AT HOBBS OBSERVATORY asteroid/. Lyle Ford, George Stecher, Kayla Lorenzen, and Cole Cook Acknowledgements Department of Physics and Astronomy University of Wisconsin-Eau Claire We thank the Theodore Dunham Fund for Astrophysics, the Eau Claire, WI 54702-4004 National Science Foundation (award number 0519006), the [email protected] University of Wisconsin-Eau Claire Office of Research and Sponsored Programs, and the University of Wisconsin-Eau Claire (Received: 2009 Feb 11) Blugold Fellow and McNair programs for financial support. References We observed 343 Ostara on 2008 October 4 and obtained R and V standard magnitudes. The period was Binzel, R.P. (1987). “A Photoelectric Survey of 130 Asteroids”, found to be significantly greater than the previously Icarus 72, 135-208. reported value of 6.42 hours. Measurements of 2660 Wasserman and (17010) 1999 CQ72 made on 2008 Stecher, G.J., Ford, L.A., and Elbert, J.D. (1999). “Equipping a March 25 are also reported. 0.6 Meter Alt-Azimuth Telescope for Photometry”, IAPPP Comm, 76, 68-74. We made R band and V band photometric measurements of 343 Warner, B.D. (2006). A Practical Guide to Lightcurve Photometry Ostara on 2008 October 4 using the 0.6 m “Air Force” Telescope and Analysis. Springer, New York, NY. located at Hobbs Observatory (MPC code 750) near Fall Creek, Wisconsin. -
Near-Infrared Observations of Active Asteroid (3200) Phaethon Reveal No Evidence for Hydration ✉ Driss Takir 1,7 , Theodore Kareta 2, Joshua P
ARTICLE https://doi.org/10.1038/s41467-020-15637-7 OPEN Near-infrared observations of active asteroid (3200) Phaethon reveal no evidence for hydration ✉ Driss Takir 1,7 , Theodore Kareta 2, Joshua P. Emery3, Josef Hanuš 4, Vishnu Reddy2, Ellen S. Howell2, Andrew S. Rivkin5 & Tomoko Arai6 Asteroid (3200) Phaethon is an active near-Earth asteroid and the parent body of the Geminid Meteor Shower. Because of its small perihelion distance, Phaethon’s surface reaches 1234567890():,; temperatures sufficient to destabilize hydrated materials. We conducted rotationally resolved spectroscopic observations of this asteroid, mostly covering the northern hemisphere and the equatorial region, beyond 2.5-µm to search for evidence of hydration on its surface. Here we show that the observed part of Phaethon does not exhibit the 3-µm hydrated mineral absorption (within 2σ). These observations suggest that Phaethon’s modern activity is not due to volatile sublimation or devolatilization of phyllosilicates on its surface. It is possible that the observed part of Phaethon was originally hydrated and has since lost volatiles from its surface via dehydration, supporting its connection to the Pallas family, or it was formed from anhydrous material. 1 JETS/ARES, NASA Johnson Space Center, Houston, TX 77058-3696, USA. 2 Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721- 0092, USA. 3 Department of Astronomy and Planetary Sciences, Northern Arizona University, Flagstaff, AZ 86011, USA. 4 Institute of Astronomy, Charles University, CZ-18000 Prague 8, Czech Republic. 5 Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20273, USA. 6 Planetary Exploration Research Center, Chiba Institute of Technology, Narashino, Japan. -
(704) Interamnia from Its Occultations and Lightcurves
International Journal of Astronomy and Astrophysics, 2014, 4, 91-118 Published Online March 2014 in SciRes. http://www.scirp.org/journal/ijaa http://dx.doi.org/10.4236/ijaa.2014.41010 A 3-D Shape Model of (704) Interamnia from Its Occultations and Lightcurves Isao Satō1*, Marc Buie2, Paul D. Maley3, Hiromi Hamanowa4, Akira Tsuchikawa5, David W. Dunham6 1Astronomical Society of Japan, Yamagata, Japan 2Southwest Research Institute, Boulder, USA 3International Occultation Timing Association, Houston, USA 4Hamanowa Astronomical Observatory, Fukushima, Japan 5Yanagida Astronomical Observatory, Ishikawa, Japan 6International Occultation Timing Association, Greenbelt, USA Email: *[email protected], [email protected], [email protected], [email protected], [email protected], [email protected] Received 9 November 2013; revised 9 December 2013; accepted 17 December 2013 Copyright © 2014 by authors and Scientific Research Publishing Inc. This work is licensed under the Creative Commons Attribution International License (CC BY). http://creativecommons.org/licenses/by/4.0/ Abstract A 3-D shape model of the sixth largest of the main belt asteroids, (704) Interamnia, is presented. The model is reproduced from its two stellar occultation observations and six lightcurves between 1969 and 2011. The first stellar occultation was the occultation of TYC 234500183 on 1996 De- cember 17 observed from 13 sites in the USA. An elliptical cross section of (344.6 ± 9.6 km) × (306.2 ± 9.1 km), for position angle P = 73.4 ± 12.5˚ was fitted. The lightcurve around the occulta- tion shows that the peak-to-peak amplitude was 0.04 mag. and the occultation phase was just be- fore the minimum. -
Observations from Orbiting Platforms 219
Dotto et al.: Observations from Orbiting Platforms 219 Observations from Orbiting Platforms E. Dotto Istituto Nazionale di Astrofisica Osservatorio Astronomico di Torino M. A. Barucci Observatoire de Paris T. G. Müller Max-Planck-Institut für Extraterrestrische Physik and ISO Data Centre A. D. Storrs Towson University P. Tanga Istituto Nazionale di Astrofisica Osservatorio Astronomico di Torino and Observatoire de Nice Orbiting platforms provide the opportunity to observe asteroids without limitation by Earth’s atmosphere. Several Earth-orbiting observatories have been successfully operated in the last decade, obtaining unique results on asteroid physical properties. These include the high-resolu- tion mapping of the surface of 4 Vesta and the first spectra of asteroids in the far-infrared wave- length range. In the near future other space platforms and orbiting observatories are planned. Some of them are particularly promising for asteroid science and should considerably improve our knowledge of the dynamical and physical properties of asteroids. 1. INTRODUCTION 1800 asteroids. The results have been widely presented and discussed in the IRAS Minor Planet Survey (Tedesco et al., In the last few decades the use of space platforms has 1992) and the Supplemental IRAS Minor Planet Survey opened up new frontiers in the study of physical properties (Tedesco et al., 2002). This survey has been very important of asteroids by overcoming the limits imposed by Earth’s in the new assessment of the asteroid population: The aster- atmosphere and taking advantage of the use of new tech- oid taxonomy by Barucci et al. (1987), its recent extension nologies. (Fulchignoni et al., 2000), and an extended study of the size Earth-orbiting satellites have the advantage of observing distribution of main-belt asteroids (Cellino et al., 1991) are out of the terrestrial atmosphere; this allows them to be in just a few examples of the impact factor of this survey. -
Color Study of Asteroid Families Within the MOVIS Catalog David Morate1,2, Javier Licandro1,2, Marcel Popescu1,2,3, and Julia De León1,2
A&A 617, A72 (2018) Astronomy https://doi.org/10.1051/0004-6361/201832780 & © ESO 2018 Astrophysics Color study of asteroid families within the MOVIS catalog David Morate1,2, Javier Licandro1,2, Marcel Popescu1,2,3, and Julia de León1,2 1 Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea s/n, 38205 La Laguna, Tenerife, Spain e-mail: [email protected] 2 Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain 3 Astronomical Institute of the Romanian Academy, 5 Cu¸titulde Argint, 040557 Bucharest, Romania Received 6 February 2018 / Accepted 13 March 2018 ABSTRACT The aim of this work is to study the compositional diversity of asteroid families based on their near-infrared colors, using the data within the MOVIS catalog. As of 2017, this catalog presents data for 53 436 asteroids observed in at least two near-infrared filters (Y, J, H, or Ks). Among these asteroids, we find information for 6299 belonging to collisional families with both Y J and J Ks colors defined. The work presented here complements the data from SDSS and NEOWISE, and allows a detailed description− of− the overall composition of asteroid families. We derived a near-infrared parameter, the ML∗, that allows us to distinguish between four generic compositions: two different primitive groups (P1 and P2), a rocky population, and basaltic asteroids. We conducted statistical tests comparing the families in the MOVIS catalog with the theoretical distributions derived from our ML∗ in order to classify them according to the above-mentioned groups. We also studied the background populations in order to check how similar they are to their associated families. -
Surface Composition of Icy Asteroids and the Special Case of Ceres
Surface composition of icy asteroids and the special case of Ceres P. Vernazza (Laboratoire d’Astrophysique de Marseille) March 15, 2017 SOFIA Tele-Talk Examples of asteroids with Compositional links between asteroids and meteorites meteoritic analogues Falls Mass in the asteroid belt 6.2% 9.6% 80.0% 8.4% 1.9% 1.0% 1.1% 0.4% 2.5% 0.1% 1.5% 7.0% 4.6% 3.3% Total Total ~98% ~30% Vernazza & Beck 2016 ~2/3 of the mass of the asteroid belt seems absent from our meteorite collections 6 asteroid types, representing ~2/3 of the main belt mass (DeMeo & Carry 2013), are presently unconnected to meteorites. Asteroid spectral properties (DeMeo et al. 2009) Metamorphosed CI/CM chondrites as analogues of most B, C, Cb, Cg types? (1) Metamorphosed CI/CM chondrites as analogues of most B, C, Cb, Cg types? (2) This is very unlikely because: a) Metamorphosed CI/CM chondrites represent 0.2% of the falls whereas B, C, Cb and Cg type represent ~50% of the mass of the belt b) Metamorphosed CI/CM chondrites possess a significantly higher density (2.5-3 g/cm3) than those asteroid types (0.8-1.5 g/cm3) c) Metamorphosed CI/CM chondrites possess different spectral properties in the mid-infrared with respect to those asteroid types Why are most B, C, Cb, Cg, P and D types unsampled by our meteorite collections? The lack of samples for these objects within our collections may stem from the fact that they are volatile-rich as implied by their low density (0.8-2 g/cm3) and their comet-like activity in some cases. -
Asteroid Family Identification 613
Bendjoya and Zappalà: Asteroid Family Identification 613 Asteroid Family Identification Ph. Bendjoya University of Nice V. Zappalà Astronomical Observatory of Torino Asteroid families have long been known to exist, although only recently has the availability of new reliable statistical techniques made it possible to identify a number of very “robust” groupings. These results have laid the foundation for modern physical studies of families, thought to be the direct result of energetic collisional events. A short summary of the current state of affairs in the field of family identification is given, including a list of the most reliable families currently known. Some likely future developments are also discussed. 1. INTRODUCTION calibrate new identification methods. According to the origi- nal papers published in the literature, Brouwer (1951) used The term “asteroid families” is historically linked to the a fairly subjective criterion to subdivide the Flora family name of the Japanese researcher Kiyotsugu Hirayama, who delineated by Hirayama. Arnold (1969) assumed that the was the first to use the concept of orbital proper elements to asteroids are dispersed in the proper-element space in a identify groupings of asteroids characterized by nearly iden- Poisson distribution. Lindblad and Southworth (1971) cali- tical orbits (Hirayama, 1918, 1928, 1933). In interpreting brated their method in such a way as to find good agree- these results, Hirayama made the hypothesis that such a ment with Brouwer’s results. Carusi and Massaro (1978) proximity could not be due to chance and proposed a com- adjusted their method in order to again find the classical mon origin for the members of these groupings. -
Aas 14-267 Design of End-To-End Trojan Asteroid
AAS 14-267 DESIGN OF END-TO-END TROJAN ASTEROID RENDEZVOUS TOURS INCORPORATING POTENTIAL SCIENTIFIC VALUE Jeffrey Stuart,∗ Kathleen Howell,y and Roby Wilsonz The Sun-Jupiter Trojan asteroids are celestial bodies of great scientific interest as well as potential natural assets offering mineral resources for long-term human exploration of the solar system. Previous investigations have addressed the auto- mated design of tours within the asteroid swarm and the transition of prospective tours to higher-fidelity, end-to-end trajectories. The current development incorpo- rates the route-finding Ant Colony Optimization (ACO) algorithm into the auto- mated tour generation procedure. Furthermore, the potential scientific merit of the target asteroids is incorporated such that encounters with higher value asteroids are preferentially incorporated during sequence creation. INTRODUCTION Near Earth Objects (NEOs) are currently under consideration for manned sample return mis- sions,1 while a recent NASA feasibility assessment concludes that a mission to the Trojan asteroids can be accomplished at a projected cost of less than $900M in fiscal year 2015 dollars.2 Tour concepts within asteroid swarms allow for a broad sampling of interesting target bodies either for scientific investigation or as potential resources to support deep-space human missions. However, the multitude of asteroids within the swarms necessitates the use of automated design algorithms if a large number of potential mission options are to be surveyed. Previously, a process to automatically and rapidly generate sample tours within the Sun-Jupiter L4 Trojan asteroid swarm with a mini- mum of human interaction has been developed.3 This scheme also enables the automated transition of tours of interest into fully optimized, end-to-end trajectories using a variety of electrical power sources.4,5 This investigation extends the automated algorithm to use ant colony optimization, a heuristic search algorithm, while simultaneously incorporating a relative ‘scientific importance’ ranking into tour construction and analysis. -
Chaotic Diffusion of the Vesta Family Induced by Close Encounters with Massive Asteroids
A&A 540, A118 (2012) Astronomy DOI: 10.1051/0004-6361/201118339 & c ESO 2012 Astrophysics Chaotic diffusion of the Vesta family induced by close encounters with massive asteroids J.-B. Delisle and J. Laskar ASD, IMCCE-CNRS UMR8028, Observatoire de Paris, UPMC, 77 Av. Denfert-Rochereau, 75014 Paris, France e-mail: [email protected] Received 26 October 2011 / Accepted 1 March 2012 ABSTRACT We numerically estimate the semi-major axis chaotic diffusion of the Vesta family asteroids induced by close encounters with 11 mas- sive main-belt asteroids: (1) Ceres, (2) Pallas, (3) Juno, (4) Vesta, (7) Iris, (10) Hygiea, (15) Eunomia, (19) Fortuna, (324) Bamberga, (532) Herculina, (704) Interamnia. We find that most of the diffusion is caused by Ceres and Vesta. By extrapolating our results, we are able to constrain the global effect of close encounters with all main-belt asteroids. A comparison of this drift estimate with the one expected for the Yarkovsky effect shows that for asteroids whose diameter is larger than about 40 km, close encounters dominate the Yarkovsky effect. Overall, our findings confirm the standard scenario for the history of the Vesta family. Key words. celestial mechanics – minor planets, asteroids: general – chaos – methods: numerical 1. Introduction (in terms of the number of asteroids taken into account) con- cerned the Gefion and Adeona families and was conducted by It is now common consent that most of the V-type near-Earth as- Carruba et al. (2003). The authors considered all 682 asteroids teroids (NEAs) and howardite, eucrite, and diogenite (HED) me- of radius larger than 50 km for encounters with members of teorites are fragments of a collision between Vesta and another the families. -
Origin of the Near-Earth Asteroid Phaethon and the Geminids Meteor Shower
University of Central Florida STARS Faculty Bibliography 2010s Faculty Bibliography 1-1-2010 Origin of the near-Earth asteroid Phaethon and the Geminids meteor shower J. de León H. Campins University of Central Florida K. Tsiganis A. Morbidelli J. Licandro Find similar works at: https://stars.library.ucf.edu/facultybib2010 University of Central Florida Libraries http://library.ucf.edu This Article is brought to you for free and open access by the Faculty Bibliography at STARS. It has been accepted for inclusion in Faculty Bibliography 2010s by an authorized administrator of STARS. For more information, please contact [email protected]. Recommended Citation de León, J.; Campins, H.; Tsiganis, K.; Morbidelli, A.; and Licandro, J., "Origin of the near-Earth asteroid Phaethon and the Geminids meteor shower" (2010). Faculty Bibliography 2010s. 92. https://stars.library.ucf.edu/facultybib2010/92 A&A 513, A26 (2010) Astronomy DOI: 10.1051/0004-6361/200913609 & c ESO 2010 Astrophysics Origin of the near-Earth asteroid Phaethon and the Geminids meteor shower J. de León1,H.Campins2,K.Tsiganis3, A. Morbidelli4, and J. Licandro5,6 1 Instituto de Astrofísica de Andalucía-CSIC, Camino Bajo de Huétor 50, 18008 Granada, Spain e-mail: [email protected] 2 University of Central Florida, PO Box 162385, Orlando, FL 32816.2385, USA e-mail: [email protected] 3 Department of Physics, Aristotle University of Thessaloniki, 54 124 Thessaloniki, Greece 4 Departement Casiopée: Universite de Nice - Sophia Antipolis, Observatoire de la Cˆote d’Azur, CNRS 4, 06304 Nice, France 5 Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea s/n, 38205 La Laguna, Spain 6 Department of Astrophysics, University of La Laguna, 38205 La Laguna, Tenerife, Spain Received 5 November 2009 / Accepted 26 January 2010 ABSTRACT Aims.