The Resolved Asteroid Program
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(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. -
CURRICULUM VITAE, ALAN W. HARRIS Personal: Born
CURRICULUM VITAE, ALAN W. HARRIS Personal: Born: August 3, 1944, Portland, OR Married: August 22, 1970, Rose Marie Children: W. Donald (b. 1974), David (b. 1976), Catherine (b 1981) Education: B.S. (1966) Caltech, Geophysics M.S. (1967) UCLA, Earth and Space Science PhD. (1975) UCLA, Earth and Space Science Dissertation: Dynamical Studies of Satellite Origin. Advisor: W.M. Kaula Employment: 1966-1967 Graduate Research Assistant, UCLA 1968-1970 Member of Tech. Staff, Space Division Rockwell International 1970-1971 Physics instructor, Santa Monica College 1970-1973 Physics Teacher, Immaculate Heart High School, Hollywood, CA 1973-1975 Graduate Research Assistant, UCLA 1974-1991 Member of Technical Staff, Jet Propulsion Laboratory 1991-1998 Senior Member of Technical Staff, Jet Propulsion Laboratory 1998-2002 Senior Research Scientist, Jet Propulsion Laboratory 2002-present Senior Research Scientist, Space Science Institute Appointments: 1976 Member of Faculty of NATO Advanced Study Institute on Origin of the Solar System, Newcastle upon Tyne 1977-1978 Guest Investigator, Hale Observatories 1978 Visiting Assoc. Prof. of Physics, University of Calif. at Santa Barbara 1978-1980 Executive Committee, Division on Dynamical Astronomy of AAS 1979 Visiting Assoc. Prof. of Earth and Space Science, UCLA 1980 Guest Investigator, Hale Observatories 1983-1984 Guest Investigator, Lowell Observatory 1983-1985 Lunar and Planetary Review Panel (NASA) 1983-1992 Supervisor, Earth and Planetary Physics Group, JPL 1984 Science W.G. for Voyager II Uranus/Neptune Encounters (JPL/NASA) 1984-present Advisor of students in Caltech Summer Undergraduate Research Fellowship Program 1984-1985 ESA/NASA Science Advisory Group for Primitive Bodies Missions 1985-1993 ESA/NASA Comet Nucleus Sample Return Science Definition Team (Deputy Chairman, U.S. -
Asteroid Regolith Weathering: a Large-Scale Observational Investigation
University of Tennessee, Knoxville TRACE: Tennessee Research and Creative Exchange Doctoral Dissertations Graduate School 5-2019 Asteroid Regolith Weathering: A Large-Scale Observational Investigation Eric Michael MacLennan University of Tennessee, [email protected] Follow this and additional works at: https://trace.tennessee.edu/utk_graddiss Recommended Citation MacLennan, Eric Michael, "Asteroid Regolith Weathering: A Large-Scale Observational Investigation. " PhD diss., University of Tennessee, 2019. https://trace.tennessee.edu/utk_graddiss/5467 This Dissertation is brought to you for free and open access by the Graduate School at TRACE: Tennessee Research and Creative Exchange. It has been accepted for inclusion in Doctoral Dissertations by an authorized administrator of TRACE: Tennessee Research and Creative Exchange. For more information, please contact [email protected]. To the Graduate Council: I am submitting herewith a dissertation written by Eric Michael MacLennan entitled "Asteroid Regolith Weathering: A Large-Scale Observational Investigation." I have examined the final electronic copy of this dissertation for form and content and recommend that it be accepted in partial fulfillment of the equirr ements for the degree of Doctor of Philosophy, with a major in Geology. Joshua P. Emery, Major Professor We have read this dissertation and recommend its acceptance: Jeffrey E. Moersch, Harry Y. McSween Jr., Liem T. Tran Accepted for the Council: Dixie L. Thompson Vice Provost and Dean of the Graduate School (Original signatures are on file with official studentecor r ds.) Asteroid Regolith Weathering: A Large-Scale Observational Investigation A Dissertation Presented for the Doctor of Philosophy Degree The University of Tennessee, Knoxville Eric Michael MacLennan May 2019 © by Eric Michael MacLennan, 2019 All Rights Reserved. -
Iso and Asteroids
r bulletin 108 Figure 1. Asteroid Ida and its moon Dactyl in enhanced colour. This colour picture is made from images taken by the Galileo spacecraft just before its closest approach to asteroid 243 Ida on 28 August 1993. The moon Dactyl is visible to the right of the asteroid. The colour is ‘enhanced’ in the sense that the CCD camera is sensitive to near-infrared wavelengths of light beyond human vision; a ‘natural’ colour picture of this asteroid would appear mostly grey. Shadings in the image indicate changes in illumination angle on the many steep slopes of this irregular body, as well as subtle colour variations due to differences in the physical state and composition of the soil (regolith). There are brighter areas, appearing bluish in the picture, around craters on the upper left end of Ida, around the small bright crater near the centre of the asteroid, and near the upper right-hand edge (the limb). This is a combination of more reflected blue light and greater absorption of near-infrared light, suggesting a difference Figure 2. This image mosaic of asteroid 253 Mathilde is in the abundance or constructed from four images acquired by the NEAR spacecraft composition of iron-bearing on 27 June 1997. The part of the asteroid shown is about 59 km minerals in these areas. Ida’s by 47 km. Details as small as 380 m can be discerned. The moon also has a deeper near- surface exhibits many large craters, including the deeply infrared absorption and a shadowed one at the centre, which is estimated to be more than different colour in the violet than any 10 km deep. -
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. -
IRAS LOW RESOLUTION SPECTRA of ASTEROIDS Russell G. Walker
IRAS LOW RESOLUTION SPECTRA OF ASTEROIDS Russell G. Walker and Martin Cohen Astronomy and Astrophysics Vanguard Research, Inc. Scotts Valley, California Final Technical Report on Contract NASW-99025 April 16, 2002 Vanguard Research, Inc. 5321 Scotts Valley Drive Suite 204 Scotts Valley, California 95066 UNCLASSIFIED Abstract Optical/near-infrared studies of asteroids are based on reflected sunlight and surface albedo variations create broad spectral features, suggestive of families of materials. There is a significant literature on these features, but there is very little work in the thermal infrared that directly probes the materials emitting on the surfaces of asteroids. We have searched for and extracted 534 thermal spectra of 245 asteroids from the original Dutch (Groningen) archive of spectra observed by the IRAS Low Resolution Spectrometer (LRS). We find that, in general, the observed shapes of the spectral continua are inconsistent with that predicted by the standard thermal model used by IRAS (Lebofsky et al., 1986). Thermal models such as proposed by Harris (1998) and Harris et a1.(1998) for the near-earth asteroids with the "beaming parameter" in the range of 1.0 to 1.2 best represent the observed spectral shapes. This implies that the IRAS Minor Planet Survey (IMPS, Tedesco, 1992) and the Supplementary IMPS (SIMPS, Tedesco, et al., 2002) derived asteroid diameters are systematically underestimated, and the albedos are overestimated. We have tentatively identified several spectral features that appear to be diagnostic of at least families of materials. The variation of spectral features with taxonomic class hints that thermal infrared spectra can be a valuable tool for taxonomic classification of asteroids. -
(52) Europa Q ⇑ W.J
Icarus 225 (2013) 794–805 Contents lists available at SciVerse ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus The Resolved Asteroid Program – Size, shape, and pole of (52) Europa q ⇑ W.J. Merline a, , J.D. Drummond b, B. Carry c,d, A. Conrad e,f, P.M. Tamblyn a, C. Dumas g, M. Kaasalainen h, A. Erikson i, S. Mottola i,J.Dˇ urech j, G. Rousseau k, R. Behrend k,l, G.B. Casalnuovo k,m, B. Chinaglia k,m, J.C. Christou n, C.R. Chapman a, C. Neyman f a Southwest Research Institute, 1050 Walnut St., #300, Boulder, CO 80302, USA b Starfire Optical Range, Directed Energy Directorate, Air Force Research Laboratory, Kirtland AFB, NM 87117, USA c IMCCE, Observatoire de Paris, CNRS, 77 Av. Denfert Rochereau, 75014 Paris, France d European Space Astronomy Centre, ESA, P.O. Box 78, 28691 Villanueva de la Cañada, Madrid, Spain e Max-Planck-Institut für Astronomie, Königstuhl, 17 Heidelberg, Germany f W.M. Keck Observatory, 65-1120 Mamalahoa Highway, Kamuela, HI 96743, USA g ESO, Alonso de Córdova 3107, Vitacura, Casilla 19001, Santiago de Chile, Chile h Tampere University of Technology, P.O. Box 553, 33101 Tampere, Finland i Institute of Planetary Research, DLR, Rutherfordstrasse 2, 12489 Berlin, Germany j Astronomical Institute, Faculty of Mathematics and Physics, Charles University in Prague, V Holešovicˇkách 2, 18000 Prague, Czech Republic k CdR & CdL Group: Lightcurves of Minor Planets and Variable Stars, Switzerland l Geneva Observatory, 1290 Sauverny, Switzerland m Eurac Observatory, Bolzano, Italy n Gemini Observatory, 670 N. Aohoku Place, Hilo, HI 96720, USA article info abstract Article history: With the adaptive optics (AO) system on the 10 m Keck-II telescope, we acquired a high quality set of 84 Received 1 June 2012 images at 14 epochs of asteroid (52) Europa on 2005 January 20, when it was near opposition. -
Large Low-Albedo Asteroids: Thermal and Dynamical Context
52nd Lunar and Planetary Science Conference 2021 (LPI Contrib. No. 2548) 1364.pdf LARGE LOW-ALBEDO ASTEROIDS: DYNAMICAL AND THERMAL CONTEXT. D. Takir1, W. Neu- mann2,3 S.N. Raymond4, J.P. Emery5, M. Trieloff3. 1Jacobs, NASA Johnson Space Center, Houston ([email protected]), TX 77058, USA, 2German Aerospace Center, Institute of Planetary Research, Berlin, Ger- many, 2Institut für Geowissenschaften, Universität Heidelberg, 69120 Heidelberg, Germany. 4Laboratoire d'Astro- physique de Bordeaux, Pessac, France, 5Northern Arizona University, Flagstaff, AZ 86011, USA. Introduction: Low-albedo asteroids, most of 10]. Jupiter’s rapid increase in mass destabilized the which are located in the outer belt and Jupiter’s Trojan orbits of nearby planetesimals and gravitationally scat- clouds, provide information related to the origin and tered them in all directions. Under the action of gas evolution of the solar system and the conditions in drag, a fraction of planetesimals was implanted onto which the solar nebula was formed. These asteroids are stable orbits, preferentially in the outer main belt ([11], widely thought to be the source of the primitive carbo- [12]). This same process was repeated during Saturn’s naceous chondrites and allow us to put crucial con- rapid gas accretion. Primitive planetesimals were likely straints on the current dynamical and thermal theories implanted from across the outer solar system and in of the formation and evolution of the early solar sys- multiple episodes (Fig. 2). The narrowest possible tem. source region assuming that Jupiter and Saturn grew The nature of surface composition of large and in-situ with no migration – is still ~5 AU wide, extend- low-albedo asteroids, like (1) Ceres, (10) Hygiea and ing from roughly 4-9 AU [11]. -
(704) Interamnia: a Transitional Object Between a Dwarf Planet and a Typical Irregular-Shaped Minor Body G
(704) Interamnia: a transitional object between a dwarf planet and a typical irregular-shaped minor body G. Dudziński, E. Podlewska-Gaca, P. Bartczak, S Benseguane, M. Ferrais, L. Jorda, J. Hanuš, P. Vernazza, N. Rambaux, B. Carry, et al. To cite this version: G. Dudziński, E. Podlewska-Gaca, P. Bartczak, S Benseguane, M. Ferrais, et al.. (704) Interamnia: a transitional object between a dwarf planet and a typical irregular-shaped minor body. Astronomy and Astrophysics - A&A, EDP Sciences, 2020, 633 (2), pp.A65. 10.1051/0004-6361/201936639. hal- 02996661 HAL Id: hal-02996661 https://hal.archives-ouvertes.fr/hal-02996661 Submitted on 15 Apr 2021 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. A&A 633, A65 (2020) Astronomy https://doi.org/10.1051/0004-6361/201936639 & © ESO 2020 Astrophysics (704) Interamnia: a transitional object between a dwarf planet and a typical irregular-shaped minor body?,?? J. Hanuš1, P. Vernazza2, M. Viikinkoski3, M. Ferrais4,2, N. Rambaux5, E. Podlewska-Gaca6, A. Drouard2, L. Jorda2, E. Jehin4, B. Carry7, M. Marsset8, F. Marchis9, B. Warner10, R. Behrend11, V. Asenjo12, N. Berger13, M. Bronikowska14, T. -
Hydrated Minerals on Asteroids 235
Rivkin et al.: Hydrated Minerals on Asteroids 235 Hydrated Minerals on Asteroids: The Astronomical Record A. S. Rivkin Massachusetts Institute of Technology E. S. Howell Arecibo Observatory F. Vilas NASA Johnson Space Center L. A. Lebofsky University of Arizona Knowledge of the hydrated mineral inventory on the asteroids is important for deducing the origin of Earth’s water, interpreting the meteorite record, and unraveling the processes occurring during the earliest times in solar system history. Reflectance spectroscopy shows absorption features in both the 0.6–0.8 and 2.5–3.5-µm regions, which are diagnostic of or associated with hydrated minerals. Observations in those regions show that hydrated minerals are common in the mid-asteroid belt, and can be found in unexpected spectral groupings as well. Asteroid groups formerly associated with mineralogies assumed to have high-temperature formation, such as M- and E-class asteroids, have been observed to have hydration features in their reflectance spectra. Some asteroids have apparently been heated to several hundred degrees Celsius, enough to destroy some fraction of their phyllosilicates. Others have rotational variation suggesting that heating was uneven. We summarize this work, and present the astronomical evidence for water- and hydroxyl-bearing minerals on asteroids. 1. INTRODUCTION to be common. Indeed, water is found throughout the outer solar system on satellites (Clark and McCord, 1980; Clark Extraterrestrial water and water-bearing minerals are of et al., 1984), Kuiper Belt Objects (KBOs) (Brown et al., great importance both for understanding the formation and 1997), and comets (Bregman et al., 1988; Brooke et al., 1989) evolution of the solar system and for supporting future as ice, and on the planets as vapor (Larson et al., 1975; human activities in space. -
Asteroid Shape Determination: a Comparison of Ao Imaging with Lightcurve Inversion A
Lunar and Planetary Science XXXIX (2008) 2473.pdf ASTEROID SHAPE DETERMINATION: A COMPARISON OF AO IMAGING WITH LIGHTCURVE INVERSION A. R. Conrad1, W. J. Merline3, J. D. Drummond4, B. Carry2, C. Dumas2, P. M. Tamblyn3, R. D. Campbell1, R. W. Goodrich1, D. Le Mignant1, 1W.M. Keck Observatory, 65-1120 Mamalahoa Highway, Kamuela, HI, 96743, 2ESO Very Large Telescope (VLT), European Southern Observatory, Alonso de Cordova 3107, Vi- tacura Casilla 19001, Santiago 19, Chile, 3Southwest Research Institute, 1050 Walnut Street, Ste 300, Boulder, CO 80302, 4Starfire Optical Range, Directed Energy Directorate, Air Force Research Laboratory, Kirtland AFB, NM 87117 Summary: We present imaging data on 3 larger as- model from a single-rotation data set. Additional ob- teroids, taken with adaptive optics (AO) on large tele- servations taken later in time can give powerful lever- scopes, with high spatial and rotational resolution. age to reduce uncertainties [12]. We can identify and The resulting shapes can be compared with previous rotationally confirm large shape features, such as the shape models derived from inversion of lightcurve two facets and the promontory identified on Davida data, and the agreement is generally good. [9]. Further this can lead to geological interpretations Introduction: The physical and statistical study of such as the identification of giant craters, giving in- asteroids requires accurate knowledge of their shape, sight into impact history [9]. Here we extend efforts by size, and pole position. Improved size permits im- our group and others [10,11] to validate earlier shape proved estimates of albedo, in turn allowing better models produced with lightcurve techniques.