Resorting Query Results

Minor Planet Publications Used in Preparing the 2005 Triennial Report

The ADS abstract service (http://adsabs.harvard.edu/abstract_service.html) was searched for papers appearing in refereed publications during the period between July 2002 and June 2005, inclusive, on the terms ` “asteroid” OR “minor planet” ‘. This returned 665 abstracts from which we selected 339 as falling under the purview of the Physical Studies of Minor Planets Working Group. That is, no purely meteoritical, theoretical, dynamical, or astrometric studies were included. However, papers on these topics from which physical properties such as Yarkovsky effect, size-frequency distributions, masses, etc., were included.

The 339 relevant papers were sorted into twelve categories and a brief description of the scientific results in each category was written citing a subset of them. The titles and abstracts for the entire list of 339 papers appear below. The order of this list is that returned by the ADS search engine, i.e., it is not in alphabetical or chronological order. A paper cited in the IAU Triennial Report can be located using the browser or PDF reader’s “Find” function.

This list was prepared by A. Cellino and E. Tedesco on 12 September 2005

Title:		Widespread magma oceans on asteroidal bodies in the early Solar System
Authors:		Greenwood, Richard C.; Franchi, Ian A.; Jambon, Albert; Buchanan, Paul C.
Journal:		Nature, Volume 435, Issue 7044, pp. 916-918 (2005). (Nature Homepage)
Publication Date:		06/2005
Origin:		NATURE
Abstract Copyright:		(c) 2005: Nature
DOI:		10.1038/nature03612
Bibliographic Code:		2005Natur.435..916G

Abstract

Immediately following the formation of the Solar System, small planetary bodies accreted, some of which melted to produce igneous rocks. Over a longer timescale (15-33Myr), the inner planets grew by incorporation of these smaller objects through collisions. Processes operating on such asteroids strongly influenced the final composition of these planets, including Earth. Currently there is little agreement about the nature of asteroidal igneous activity: proposals range from small-scale melting, to near total fusion and the formation of deep magma oceans. Here we report a study of oxygen isotopes in two basaltic meteorite suites, the HEDs (howardites, eucrites and diogenites, which are thought to sample the asteroid 4 Vesta) and the angrites (from an unidentified asteroidal source). Our results demonstrate that these meteorite suites formed during early, global-scale melting (>= 50 per cent) events. We show that magma oceans were present on all the differentiated Solar System bodies so far sampled. Magma oceans produced compositionally layered planetesimals; the modification of such bodies before incorporation into larger objects can explain some anomalous planetary features, such as Earth's high Mg/Si ratio.

Title:		Yarkovsky origin of the unstable asteroids in the 2/1 mean motion resonance with Jupiter
Authors:		Brož, M.; Vokrouhlický, D.; Roig, F.; Nesvorný, D.; Bottke, W. F.; Morbidelli, A.
Affiliation:		AA(Institute of Astronomy, Charles University, Prague, V Holešovičkách 2, 18000 Prague 8, Czech Republic), AB(Institute of Astronomy, Charles University, Prague, V Holešovičkách 2, 18000 Prague 8, Czech Republic), AC(Observatório Nacional - MCT, Rua Gal. José Cristino 77, Rio de Janeiro, 20921-400 RJ, Brazil), AD(Department of Space Studies, Southwest Research Institute, 1050 Walnut St., Suite 400, Boulder, CO 80302, USA), AE(Department of Space Studies, Southwest Research Institute, 1050 Walnut St., Suite 400, Boulder, CO 80302, USA), AF(Observatoire de la Côte d'Azur, Dept. Cassiopee, BP 4224, 06304 Nice Cedex 4, France)
Journal:		Monthly Notices of the Royal Astronomical Society, Volume 359, Issue 4, pp. 1437-1455. (MNRAS Homepage)
Publication Date:		06/2005
Origin:		MNRAS
Abstract Copyright:		(c) 2005 RAS
DOI:		10.1111/j.1365-2966.2005.08995.x
Bibliographic Code:		2005MNRAS.359.1437B

Abstract

The 2/1 mean motion resonance with Jupiter, intersecting the main asteroid belt at ~3.27 au, contains a small population of objects. Numerical investigations have classified three groups within this population: asteroids residing on stable orbits (i.e. Zhongguos), those on marginally stable orbits with dynamical lifetimes of the order of 100 Myr (i.e. Griquas), and those on unstable orbits. In this paper, we reexamine the origin, evolution and survivability of objects in the 2/1 population. Using recent asteroid survey data, we have identified 100 new members since the last search, which increases the resonant population to 153. The most interesting new asteroids are those located in the theoretically predicted stable island A, which until now had been thought to be empty. We also investigate whether the population of objects residing on the unstable orbits could be resupplied by material from the edges of the 2/1 resonance by the thermal drag force known as the Yarkovsky effect (and by the YORP effect, which is related to the rotational dynamics). Using N-body simulations, we show that test particles pushed into the 2/1 resonance by the Yarkovsky effect visit the regions occupied by the unstable asteroids. We also find that our test bodies have dynamical lifetimes consistent with the integrated orbits of the unstable population. Using a semi-analytical Monte Carlo model, we compute the steady-state size distribution of magnitude H < 14 asteroids on unstable orbits within the resonance. Our results provide a good match with the available observational data. Finally, we discuss whether some 2/1 objects may be temporarily captured Jupiter-family comets or near-Earth asteroids.

Title:		Spectral study of the Eunomia asteroid family
Authors:		Nathues, Andreas; Mottola, Stefano; Kaasalainen, Mikko; Neukum, Gerhard
Affiliation:		AA(Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Straße 2, 37191 Katlenburg-Lindau, Germany), AB(DLR, Institute of Space Sensor Technology and Planetary Exploration, Rutherfordstrasse 2, 12489 Berlin, Germany), AC(Rolf Nevanlinna Institute, Department of Mathematics and Statistics, P.O. Box 68, 00014 University of Helsinki, Finland), AD(Freie Universität Berlin, Institut für Geologie, Geophysik und Geoinformatik, Malteserstraße 74-100, D-12249 Berlin, Germany)
Journal:		Icarus, Volume 175, Issue 2, p. 452-463. (Icarus Homepage)
Publication Date:		06/2005
Origin:		ELSEVIER
Abstract Copyright:		(c) 2005 Elsevier Science B.V. All rights reserved.
DOI:		10.1016/j.icarus.2004.12.013
Bibliographic Code:		2005Icar..175..452N

Abstract

We present color ratio curves of the S-Asteroid 15 Eunomia, which have been extracted from high-precision photometric lightcurves obtained in three different VNIR wavelength bands at the Bochum Telescope, La Silla. The measured color ratio curves and near infrared spectra were used to derive a detailed surface composition model whose shape has been computed by V-lightcurve inversions. According to this analysis, the asteroid shows on one hemisphere a higher concentration of pyroxene, which causes an increased 440/700 nm and a reduced 940/700 nm reflectance ratio as well as a pronounced 2-μm absorption band. The remaining surface shows a higher concentration of olivine, leading to a reduced 440/700 nm and slightly increased 940/700 nm color ratio. In addition, we found that the maximum of the 440/700 nm color ratio curve coincide with the minimum of the 940/700 nm color ratio curve and vice versa. We demonstrate on the basis of USGS laboratory spectra that this anti-cyclical behavior can be explained by choosing Fe-rich olivine and a pyroxene with moderate Fe content as varying mineral phases. Furthermore, our observations confirm that 15 Eunomia is an irregular elongated and at least partially differentiated body. Previous spectral investigations of several smaller fragments of the Eunomia asteroid family revealed that the amount of fragments showing an increased pyroxene content exceeds the amount of pyroxene-poor fragments (Nathues, 2000, DLR Forschungsbericht, ISSN 1434-8454). This finding together with the observation that the major fraction of Eunomia's surface is enriched in olivine let us claim that a large fraction of the original pyroxene-enriched crust layer has been lost due to a major collision that created the Eunomia asteroid family. Significant spectral evidences, consistent with high concentrations of metals have been found neither in the rotational resolved spectra of 15 Eunomia nor in its fragments. This led to the conclusion that either no core consisting mainly of metals exists or that an eventual one has not been unearthed by the impact.

Title:		The spin state of 433 Eros and its possible implications
Authors:		Vokrouhlický, D.; Bottke, W. F.; Nesvorný, D.
Affiliation:		AA(Institute of Astronomy, Charles University, V Holešovičkách 2, CZ-18000 Prague 8, Czech Republic), AB(Southwest Research Institute, 1050 Walnut St, Suite 400, Boulder, CO 80302, USA), AC(Southwest Research Institute, 1050 Walnut St, Suite 400, Boulder, CO 80302, USA)
Journal:		Icarus, Volume 175, Issue 2, p. 419-434. (Icarus Homepage)
Publication Date:		06/2005
Origin:		ELSEVIER
DOI:		10.1016/j.icarus.2004.11.017
Bibliographic Code:		2005Icar..175..419V

Abstract

In this paper, we show that Asteroid (433) Eros is currently residing in a spin orbit resonance, with its spin axis undergoing a small-amplitude libration about the Cassini state 2 of the proper mode in the nonsingular orbital element sinI/2exp(ıΩ), where I the orbital inclination and Ω the longitude of the node. The period of this libration is &simeq;53.4 kyr. By excluding these libration wiggles, we find that Eros' pole precesses with the proper orbital plane in inertial space with a period of &simeq;61.4 kyr. Eros' resonant state forces its obliquity to oscillate with a period of &simeq;53.4 kyr between &simeq;76° and &simeq;89.5°. The observed value of &simeq;89° places it near the latter extreme of this cycle. We have used these results to probe Eros' past orbit and spin evolution. Our computations suggest that Eros is unlikely to have achieved its current spin state by solar and planetary gravitational perturbations alone. We hypothesize that some dissipative process such as thermal torques (e.g., the so-called YORP effect) may be needed in our model to obtain a more satisfactory match with data. A detailed study of this problem is left for future work.

Title:		An equal-area map projection for irregular objects
Authors:		Berthoud, M. G.
Affiliation:		Center for Radiophysics and Space Research, 306 Space Sciences, Cornell University, Ithaca, NY 14850, USA
Journal:		Icarus, Volume 175, Issue 2, p. 382-389. (Icarus Homepage)
Publication Date:		06/2005
Origin:		ELSEVIER
Abstract Copyright:		(c) 2005 Elsevier Science B.V. All rights reserved.
DOI:		10.1016/j.icarus.2004.11.021
Bibliographic Code:		2005Icar..175..382B

Abstract

An increasing number of objects discovered in the Solar System have irregular shapes which require unconventional mapping techniques. Here we present a technique that produces equivalent maps of such objects. As such maps preserve surface area they are especially useful for mapping the distribution of geological features on irregular objects. Maps of blocks and craters on the Asteroid 433 Eros are used to illustrate the potential use of the technique. Two equal-area maps are adequate to cover the entire asteroid and convincingly demonstrate variations in surface density of mapped features. Similar coverage by orthographic views requires 4 to 6 plots. The distortion of the maps are comparable to the distortions of maps created by other techniques.

Title:		The Statistical Asteroid Model. I. The Main-Belt Population for Diameters Greater than 1 Kilometer
Authors:		Tedesco, Edward F.; Cellino, Alberto; Zappalá, Vincenzo
Affiliation:		AA(Space Science Center, University of New Hampshire, Durham, NH 03824; ), AB(INAF - Osservatorio Astronomico di Torino, 10025 Pino Torinese, Torino, Italy; , ), AC(INAF - Osservatorio Astronomico di Torino, 10025 Pino Torinese, Torino, Italy; , )
Journal:		The Astronomical Journal, Volume 129, Issue 6, pp. 2869-2886. (AJ Homepage)
Publication Date:		06/2005
Origin:		UCP
AJ Keywords:		Infrared: Solar System, Minor Planets, Asteroids, Solar System: General
Abstract Copyright:		(c) 2005: The American Astronomical Society
DOI:		10.1086/429734
Bibliographic Code:		2005AJ....129.2869T

Abstract

We describe the creation of a model of the main asteroid belt whose purpose is to describe the main-belt asteroid size frequency distribution and simulate the number of main-belt asteroids and their fluxes at visual through mid-infrared (~0.3-70 μm) wavelengths in any area of sky for an arbitrary date. This model is based on a population of ~1.9×10⁶ asteroids obtained from the complete known asteroid sample, plus extrapolation of the size-frequency distributions of 15 asteroid dynamical families and three background populations, to a diameter limit of 1 km. The model is compared with data and other models, example applications are given, planned refinements and extensions to the model are presented, and some implications of the resulting size frequency distribution are discussed.

Title:		Analysis of near-IR spectra of 1 Ceres and 4 Vesta, targets of the Dawn mission
Authors:		Vernazza, P.; Mothé-Diniz, T.; Barucci, M. A.; Birlan, M.; Carvano, J. M.; Strazzulla, G.; Fulchignoni, M.; Migliorini, A.
Affiliation:		AA(LESIA, Observatoire de Paris, 92195 Meudon Principal Cedex, France ), AB(LESIA, Observatoire de Paris, 92195 Meudon Principal Cedex, France), AC(LESIA, Observatoire de Paris, 92195 Meudon Principal Cedex, France), AD(IMCCE, Observatoire de Paris, 77 Av. Denfert Rochereau, 75014 Paris Cedex, France), AE(LESIA, Observatoire de Paris, 92195 Meudon Principal Cedex, France), AF(INAF-Osservatorio Astrofisico di Catania, via Santa Sofia 78, 95123 Catania, Italy), AG(LESIA, Observatoire de Paris, 92195 Meudon Principal Cedex, France), AH(LESIA, Observatoire de Paris, 92195 Meudon Principal Cedex, France; Dipartimento di Astronomia di Padova, Vicolo dell'Osservatorio 2, 35122 Padova, Italy)
Journal:		Astronomy and Astrophysics, Volume 436, Issue 3, June IV 2005, pp.1113-1121 (A&A Homepage)
Publication Date:		06/2005
Origin:		EDP
Keywords:		minor planets, asteroids, techniques: spectroscopic, infrared: solar system
DOI:		10.1051/0004-6361:20042506
Bibliographic Code:		2005A&A...436.1113V

Abstract

We obtained high signal to noise spectra of the two targets of the Dawn mission, 4 Vesta and 1 Ceres from observations carried out in remote control between the Observatoire de Paris-Meudon and the NASA Infrared Telescope Facility on Mauna Kea. 4 Vesta was observed in the 0.7-2.5 μm spectral region at three different rotational phases in order to i) determine the mineral composition; ii) understand the spectral variations across the surface. Vesta was also observed in the 2.0-3.8 μm range. The 3 μm absorption feature was not detected, implying the absence of OH and/or H2O-bearing minerals on the asteroid surface at the latitude of our observations. The spectrum of 1 Ceres was obtained in the 2.0-4.1 μm range and the presence of the 3.06 μm absorption feature confirmed. Laboratory measurement of ion-irradiated organics and ices suggest that the 3.06 μm feature can be reproduced with a linear mixture of crystalyne ice and residues of ion-irradiated asphaltite.

Title:		Nutational damping times in solids of revolution
Authors:		Sharma, Ishan; Burns, Joseph A.; Hui, C.-Y.
Affiliation:		AA(Department of Theoretical and Applied Mechanics, Cornell University, Ithaca, NY 14853, USA), AB(Department of Theoretical and Applied Mechanics, Cornell University, Ithaca, NY 14853, USA; Department of Astronomy, Cornell University, Ithaca, NY 14853, USA), AC(Department of Theoretical and Applied Mechanics, Cornell University, Ithaca, NY 14853, USA)
Journal:		Monthly Notices of the Royal Astronomical Society, Volume 359, Issue 1, pp. 79-92. (MNRAS Homepage)
Publication Date:		05/2005
Origin:		MNRAS
Abstract Copyright:		(c) 2005 RAS
DOI:		10.1111/j.1365-2966.2005.08864.x
Bibliographic Code:		2005MNRAS.359...79S

Abstract

We derive the characteristic nutational damping time T_d for a linear, anelastic ellipsoid of revolution. Our calculation is based on the well-known idea that energy loss within an isolated spinning body causes the axis of maximum inertia of the body to align with its angular momentum vector, leading to pure spin. Energy loss occurs within an anelastic material whenever internal stresses are time variable; thus even freely rotating bodies in space, if they are wobbling, lose energy because internal stresses are associated with the accelerations caused by nutation. We find that , where D(h) is a constant of the order of a few times 10² that depends on the shape of the body with h being the (aspect) ratio of the lengths of axes to one another, μ is the elastic modulus, Q is a quality factor that describes the anelasticity of the material, ρ is the density of the body, a is its radius and Ω is an angular velocity. This functional form of the damping time is consistent with previous results but is more soundly based. Coefficients in past expressions vary between various authors, leading to predicted damping times that can differ by factors of the order of 10. To estimate damping times for typical asteroids, we choose values for the various parameters in this expression. We conclude that the extent of energy dissipation was over, rather than underestimated, in previous treatments. None the less, we argue that asteroids will generally be found in pure rotation, unless objects are small, spinning slowly and recently excited.

Title:		Ceres: Evolution and current state
Authors:		McCord, Thomas B.; Sotin, Christophe
Journal:		Journal of Geophysical Research, Volume 110, Issue E5, CiteID E05009 (JGRE Homepage)
Publication Date:		05/2005
Origin:		AGU
AGU Keywords:		Planetary Sciences: Solar System Objects: Asteroids, Planetary Sciences: Solid Surface Planets: Origin and evolution, Planetary Sciences: Solid Surface Planets: Composition (1060, 3672), Planetary Sciences: Solid Surface Planets: Surface materials and properties
Abstract Copyright:		(c) 2005: American Geophysical Union
DOI:		10.1029/2004JE002244
Bibliographic Code:		2005JGRE..11005009M

Abstract

We modeled several thermal evolution scenarios for Ceres to explore the nature of large, wet protoplanets and to predict current-day evidence that might be found by close inspection, such as by the Dawn mission. The density for Ceres is near 2.1, suggesting a water content between 17% and 27% by mass. Short- and long-lived radioactive nuclide heating is considered. Even if only long-lived radionuclide heating is assumed, the water ice in Ceres melts quickly and a water mantle forms, but an approximately 10-km crust does not melt. The circulating warm water would alter the silicates. As heat is lost by conduction through the frozen crust, water begins to freeze out at the base of the crust. Solid-state convection begins and transports more heat as well as perhaps material dissolved or entrained in the water to or near the surface. Ceres' water layer eventually (but perhaps not entirely) freezes, forming a layered density structure with perhaps some liquid water remaining today. Our differentiated models are in agreement with the recently measured difference between the equatorial and polar radii. We find that Ceres' existence and evolution depend critically on it containing water at formation, and this depends strongly on the combination of when it accreted and the amount of ²⁶Al present in the pre-Ceres ~1-km-sized objects; slightly more ²⁶Al or earlier accretion produces a dry Vesta-like object. Melting and freezing plus mineralization would lead to several dimensional changes over time, creating topographic features, zones of weakness, and perhaps disruptions in the crust.

Title:		New V-type asteroids in near-Earth space
Authors:		Marchi, S.; Lazzarin, M.; Paolicchi, P.; Magrin, S.
Affiliation:		AA(Dipartimento di Astronomia, Università di Padova, vicolo dell'Osservatorio 2, I-35122 Padova, Italy), AB(Dipartimento di Astronomia, Università di Padova, vicolo dell'Osservatorio 2, I-35122 Padova, Italy), AC(Dipartimento di Fisica, Università di Pisa, via Buonarroti 2, I-56127 Pisa, Italy), AD(Dipartimento di Astronomia, Università di Padova, vicolo dell'Osservatorio 2, I-35122 Padova, Italy)
Journal:		Icarus, Volume 175, Issue 1, p. 170-174. (Icarus Homepage)
Publication Date:		05/2005
Origin:		ELSEVIER
Abstract Copyright:		(c) 2005 Elsevier Science B.V. All rights reserved.
DOI:		10.1016/j.icarus.2004.11.015
Bibliographic Code:		2005Icar..175..170M

Abstract

We present new visible and near-infrared spectroscopic observations of 4 small, previously unclassified, near-Earth objects (NEOs). They appear to have basaltic surfaces, and hence they can be classified as V-types. Their visible spectra exhibit a closer spectral match with the Main-Belt (MB) Asteroid (4) Vesta than the other, presently known, V-type NEOs and MB asteroids. The near-infrared spectrum of Asteroid 2003 FT3 shows—for the first time among NEOs—a peculiar shape of the 1 μm band, maybe suggesting an overabundance of olivine compared to the other V-types and to (4) Vesta. The presence of V-type objects among NEOs may be a consequence of the delivery processes connecting the inner MB to the near-Earth region. On the basis of the orbital parameters of the NEOs presented here, both the resonances (3:1 and ν₆), usually considered as the most relevant gateways for the production of near-Earth asteroids, should have been active to transfer the bodies from the MB region.

Title:		Dust transport in photoelectron layers and the formation of dust ponds on Eros
Authors:		Colwell, Joshua E.; Gulbis, Amanda A. S.; Horányi, Mihály; Robertson, Scott
Affiliation:		AA(Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80309-0392, USA), AB(Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA), AC(Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80309-0392, USA), AD(Center for Integrated Plasma Studies, University of Colorado, Boulder, CO 80309-0390, USA)
Journal:		Icarus, Volume 175, Issue 1, p. 159-169. (Icarus Homepage)
Publication Date:		05/2005
Origin:		ELSEVIER
Abstract Copyright:		(c) 2005 Elsevier Science B.V. All rights reserved.
DOI:		10.1016/j.icarus.2004.11.001
Bibliographic Code:		2005Icar..175..159C

Abstract

We investigate the electrostatic transport of charged dust in the photoelectron layer over the dayside surface of an asteroid. Micron-sized dust particles may be levitated above the surface in the photoelectron layer. Horizontal transport within the layer can then lead to net deposition of dust into shadowed regions where the electric field due to the photoelectron layer disappears. We apply a 2D numerical model simulating charged dust dynamics in the near-surface daytime plasma environment of Asteroid 433 Eros to the formation of dust deposits in craters. We find that dust tends to collect in craters and regions of shadow. This electrostatic dust transport mechanism may contribute to the formation of smooth dust ponds observed by the NEAR-Shoemaker spacecraft at Eros. The size distribution of transported dust depends on the particle density and work function, and the work function of the surface and solar wind electron temperature and density. With reasonable values for these parameters, μm-sized and smaller particles are levitated at Eros. Micrometeoroid bombardment is not a sufficient source mechanism for electrostatic transport to create the Eros dust ponds. Laboratory measurements of dust in a plasma sheath show that dust launched off the surface by direct electrostatic levitation can provide a sufficient source for transport to produce the observed Eros ponds.

Title:		Near-IR spectral evidence for the presence of iron-poor orthopyroxenes on the surfaces of six M-type asteroids
Authors:		Hardersen, Paul S.; Gaffey, Michael J.; Abell, Paul A.
Affiliation:		AA(Department of Space Studies, Room 526, Box 9008, University of North Dakota, Grand Forks, ND 58202, USA), AB(Department of Space Studies, Room 518, Box 9008, University of North Dakota, Grand Forks, ND 58202, USA; Visiting astronomer at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement No. NCC 5-538 with the National Aeronautics and Space Administration, Office of Space Science, Planetary Astronomy Program.), AC(NASA Johnson Space Center, Mail Code SR, Houston, TX 77058, USA; Visiting astronomer at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement No. NCC 5-538 with the National Aeronautics and Space Administration, Office of Space Science, Planetary Astronomy Program.)
Journal:		Icarus, Volume 175, Issue 1, p. 141-158. (Icarus Homepage)
Publication Date:		05/2005
Origin:		ELSEVIER
DOI:		10.1016/j.icarus.2004.10.017
Bibliographic Code:		2005Icar..175..141H

Abstract

The first verifiable near-infrared absorption features in the ∼0.9-μm spectral region are reported for Asteroids 16 Psyche, 69 Hesperia, 110 Lydia, 125 Liberatrix, 201 Penelope, and 216 Kleopatra. These weak features (∼1 3%) are attributed to orthopyroxenes present on the surfaces of these asteroids. 16 Psyche and 125 Liberatrix have full rotational coverage while 69 Hesperia, 110 Lydia, 201 Penelope, and 216 Kleopatra have ∼75% rotational coverage. Qualitative ∼2-μm absorption features are present, but are very weak (<1%). Absorption band positions suggest relatively low abundances of calcium and iron in the pyroxenes. This indicates relatively reducing redox conditions for these asteroids, their parent bodies, and the nebular regions in which they formed. Four potential interpretations for these asteroids include: (1) they are exposed metallic cores or core fragments of differentiated parent bodies with residual orthopyroxene mantle material, (2) they are the result of a smelting-like reaction that converts olivine to pyroxene and metallic iron in the presence of carbon at high temperatures, (3) they are analogs to the primitive metal-rich Bencubbinite meteorites, or (4) they represent metallic surfaces which have accumulated silicate debris from external sources. Of the two original interpretations for the M-asteroids, the enstatite chondrite interpretation (Chapman and Salisbury, 1973, Icarus 19, 507 522; Gaffey and McCord, 1979, Mineralogical and petrological characterizations of asteroids. In: Gehrels T. (Ed.), Asteroids. Univ. of Arizona Press, Tucson, pp. 688 723) can be eliminated for these asteroids because the pyroxene in enstatite chondrites is iron-free and does not exhibit such absorption features. The iron meteorite interpretation remains valid, but with modification. For M-Asteroids 16 Psyche and 216 Kleopatra, these spectral results combined with previous determinations of high radar albedos indicate that these bodies are most probably exposed core fragments of differentiated bodies. M-Asteroids 69 Hesperia, 110 Lydia, 125 Liberatrix, and 201 Penelope exhibit similar spectral features consistent with exposed core fragments, but radar observations would be needed to confirm a high metal abundance. Observations of M-Asteroids 136 Austria and 325 Heidelberga suggest the absence of absorption features in the ∼0.4- to ∼2.5-μm region within the scatter of the data. Verification of the presence or absence of features across the surfaces of these two asteroids requires full rotational coverage. The interpretations for these “featureless” M-asteroids are not well-constrained, but remain consistent with the iron meteorite and enstatite chondrite interpretations.

Title:		The fossilized size distribution of the main asteroid belt
Authors:		Bottke, William F.; Durda, Daniel D.; Nesvorný, David; Jedicke, Robert; Morbidelli, Alessandro; Vokrouhlický, David; Levison, Hal
Affiliation:		AA(Department of Space Studies, Southwest Research Institute, 1050 Walnut St, Suite 400, Boulder, CO 80302, USA), AB(Department of Space Studies, Southwest Research Institute, 1050 Walnut St, Suite 400, Boulder, CO 80302, USA), AC(Department of Space Studies, Southwest Research Institute, 1050 Walnut St, Suite 400, Boulder, CO 80302, USA), AD(Institute for Astronomy, University of Hawaii, Honolulu, HI 96822-1897, USA), AE(Observatoire de la Côte d'Azur, B.P. 4229, 06034 Nice Cedex 4, France), AF(Institute of Astronomy, Charles University, V Holešovičkách 2, 180 00 Prague 8, Czech Republic), AG(Department of Space Studies, Southwest Research Institute, 1050 Walnut St, Suite 400, Boulder, CO 80302, USA)
Journal:		Icarus, Volume 175, Issue 1, p. 111-140. (Icarus Homepage)
Publication Date:		05/2005
Origin:		ELSEVIER
DOI:		10.1016/j.icarus.2004.10.026
Bibliographic Code:		2005Icar..175..111B

Abstract

Planet formation models suggest the primordial main belt experienced a short but intense period of collisional evolution shortly after the formation of planetary embryos. This period is believed to have lasted until Jupiter reached its full size, when dynamical processes (e.g., sweeping resonances, excitation via planetary embryos) ejected most planetesimals from the main belt zone. The few planetesimals left behind continued to undergo comminution at a reduced rate until the present day. We investigated how this scenario affects the main belt size distribution over Solar System history using a collisional evolution model (CoEM) that accounts for these events. CoEM does not explicitly include results from dynamical models, but instead treats the unknown size of the primordial main belt and the nature/timing of its dynamical depletion using innovative but approximate methods. Model constraints were provided by the observed size frequency distribution of the asteroid belt, the observed population of asteroid families, the cratered surface of differentiated Asteroid (4) Vesta, and the relatively constant crater production rate of the Earth and Moon over the last 3 Gyr. Using CoEM, we solved for both the shape of the initial main belt size distribution after accretion and the asteroid disruption scaling law Q_D^∗. In contrast to previous efforts, we find our derived Q_D^∗ function is very similar to results produced by numerical hydrocode simulations of asteroid impacts. Our best fit results suggest the asteroid belt experienced as much comminution over its early history as it has since it reached its low-mass state approximately 3.9 4.5 Ga. These results suggest the main belt's wavy-shaped size-frequency distribution is a “fossil” from this violent early epoch. We find that most diameter D≳120 km asteroids are primordial, with their physical properties likely determined during the accretion epoch. Conversely, most smaller asteroids are byproducts of fragmentation events. The observed changes in the asteroid spin rate and lightcurve distributions near D∼100 120 km are likely to be a byproduct of this difference. Estimates based on our results imply the primordial main belt population (in the form of D<1000 km bodies) was 150 250 times larger than it is today, in agreement with recent dynamical simulations.

Title:		Optical and thermal infrared observations of six near-Earth asteroids in 2002
Authors:		Wolters, Stephen D.; Green, Simon F.; McBride, Neil; Davies, John K.
Affiliation:		AA(Planetary and Space Sciences Research Institute, The Open University, Walton Hall, Milton Keynes, Buckinghamshire, MK7 6AA, UK), AB(Planetary and Space Sciences Research Institute, The Open University, Walton Hall, Milton Keynes, Buckinghamshire, MK7 6AA, UK), AC(Planetary and Space Sciences Research Institute, The Open University, Walton Hall, Milton Keynes, Buckinghamshire, MK7 6AA, UK), AD(Astronomy Technology Centre, Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK)
Journal:		Icarus, Volume 175, Issue 1, p. 92-110. (Icarus Homepage)
Publication Date:		05/2005
Origin:		ELSEVIER
DOI:		10.1016/j.icarus.2004.10.013
Bibliographic Code:		2005Icar..175...92W

Abstract

We present thermal infrared photometry and spectrophotometry of six Near-Earth Asteroids (NEAs) using the 3.8 m United Kingdom Infrared Telescope (UKIRT) together with quasi-simultaneous optical observations of five NEAs taken at the 1.0 m Jacobus Kapteyn Telescope (JKT). For Asteroid (6455) 1992 HE we derive a rotational period P=2.736±0.002 h, and an absolute visual magnitude H=14.32±0.24. For Asteroid 2002 HK₁₂ we derive H=18.22(+0.37,−0.30). The Standard Thermal Model (STM), the Fast Rotating Model (FRM) and the Near-Earth Asteroid Thermal Model (NEATM) have been fitted to the measured fluxes to derive albedos and effective diameters. The derived geometric albedos and effective diameters are (6455) 1992 HE: p_v=0.26±0.08, D_eff=3.55±0.5 km; 1999 HF₁: p_v=0.18±0.07, D_eff=3.73(+1.0,−0.5) km; 2000 ED₁₀₄: p_v=0.18±0.05, D_eff=1.21±0.2 km; 2002 HK₁₂: p_v=0.24(+0.25,−0.11), D_eff=0.62±0.2 km; 2002 NX₁₈: p_v=0.031±0.009, D_eff=2.24±0.3 km; 2002 QE₁₅: p_v=0.15(+0.08,−0.06), D_eff=1.94±0.4 km. The limitations of using the NEATM to observe NEAs at high phase angles are discussed.

Title:		The High-Albedo Kuiper Belt Object (55565) 2002 AW₁₉₇
Authors:		Cruikshank, Dale P.; Stansberry, John A.; Emery, Joshua P.; Fernández, Yanga R.; Werner, Michael W.; Trilling, David E.; Rieke, George H.
Affiliation:		AA(NASA Ames Research Center, MS 245-6, Moffett Field, CA 94035-1000 .), AB(Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065.), AC(Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065.; SETI Institute, 2035 Landings Drive, Mountain View, CA 94043.), AD(Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822.), AE(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109.), AF(Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065.), AG(Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065.)
Journal:		The Astrophysical Journal, Volume 624, Issue 1, pp. L53-L56. (ApJ Homepage)
Publication Date:		05/2005
Origin:		UCP
ApJ Keywords:		Infrared: Solar System, Kuiper Belt, Minor Planets, Asteroids
DOI:		10.1086/430420
Bibliographic Code:		2005ApJ...624L..53C

Abstract

We detected thermal emission from the Kuiper Belt object 2002 AW₁₉₇ in 2003 December and again in 2004 April using the Multiband Imaging Photometer on the Spitzer Space Telescope. In combination with the absolute visual magnitude, the thermal measurements indicate a geometric albedo of 0.17+/-0.03 and a diameter of 700+/-50 km. The albedo of 2002 AW₁₉₇ is significantly higher than the 0.04 value typically assumed for trans-Neptunian objects, and consequently the object is smaller than previously thought based on that assumption. Our thermal measurements at two wavelengths (24 and 70 μm) allow us to constrain the surface temperature and thereby place constraints on the thermal inertia. We find that the standard thermal model (STM) is inconsistent with the 24/70 μm color unless we set the beaming parameter η>0.95, indicating that the object has a significant thermal inertia and, therefore, that the STM is inappropriate. The other end-member thermal inertia model is the fast-rotator, or isothermal-latitude, model (ILM).Â The data are well represented by an ILM with the pole of rotation inclined to the Sun by 45^deg+/-10^deg.Â The high albedo is consistent with a surface containing significant amounts of weakly absorbing materials, with ices and/or fine-grained silicates as likely candidates.

Title:		Search for Activity in 3200 Phaethon
Authors:		Hsieh, Henry H.; Jewitt, David
Affiliation:		AA(Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822; , ), AB(Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822; , )
Journal:		The Astrophysical Journal, Volume 624, Issue 2, pp. 1093-1096. (ApJ Homepage)
Publication Date:		05/2005
Origin:		UCP
ApJ Keywords:		Comets: General, Meteors, Meteoroids, Minor Planets, Asteroids
Abstract Copyright:		(c) 2005: The American Astronomical Society
DOI:		10.1086/429250
Bibliographic Code:		2005ApJ...624.1093H

Abstract

We present deep optical imaging of Geminid meteor stream parent 3200 Phaethon taken in search of low-level cometary activity (i.e., coma or dust trail). Although no unambiguous cometary behavior was observed, we find an upper limit on the object's cometary mass-loss rate of Ṁ_lim~0.01 kg s^-1. The corresponding active fraction (the fraction of the surface area that could consist of freely sublimating water ice) is f<=7×10^-6, at least 2 orders of magnitude smaller than other known comets.

Title:		The high frequency variations in the rotation of Eros
Authors:		Souchay, J.; Bouquillon, S.
Affiliation:		AA(Observatoire de Paris, SYRTE, UMR 8630 du CNRS, 61 avenue de l'Observatoire, 75014 Paris, France ), AB(Tokyo National Astronomical Observatory, Oosawa 2-21-2 Mitaka Shi, Tokyo 181-0005, Japan )
Journal:		Astronomy and Astrophysics, Volume 433, Issue 1, April I 2005, pp.375-383 (A&A Homepage)
Publication Date:		04/2005
Origin:		EDP
Keywords:		minor planets, asteroids, celestial mechanics, astrometry
DOI:		10.1051/0004-6361:20035780
Bibliographic Code:		2005A&A...433..375S

Abstract

We use very precise information concerning the physical properties of the asteroid Eros 433, obtained by the NEAR probe mission, to analytically compute the modifications of its rotation on a short time scale, with a precision never reached before for an asteroid. Two kinds of components are investigated here: the free rotation and the forced one, due to the gravitational torque exerted by the Sun. Coefficients of the short periodic part of Eros' forced nutation are rather large, due to the fact that the asteroid has a significant triaxial shape. They are calculated with the same relative accuracy as the moments of inertia of the asteroid. Our results are compared with those obtained through numerical integration (Miller et al. [CITE], Icarus, 155, 3), which show high frequency oscillations of the position of Eros' axis of figure in space. Some important differences are discussed.

Title:		On the composition of ices incorporated in Ceres
Authors:		Mousis, Olivier; Alibert, Yann
Affiliation:		AA(Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland; ), AB(Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland; )
Journal:		Monthly Notices of the Royal Astronomical Society, Volume 358, Issue 1, pp. 188-192. (MNRAS Homepage)
Publication Date:		03/2005
Origin:		MNRAS
Abstract Copyright:		(c) 2005 RAS
DOI:		10.1111/j.1365-2966.2005.08777.x
Bibliographic Code:		2005MNRAS.358..188M

Abstract

We use the clathrate hydrate trapping theory and gas drag formalism to calculate the composition of ices incorporated in the interior of Ceres. Utilizing a time-dependent solar nebula model, we show that icy solids can drift from beyond 5 au to the present location of the asteroid and be preserved from vaporization. We argue that volatiles were trapped in the outer solar nebula in the form of clathrate hydrates, hydrates and pure condensates prior to having been incorporated in icy solids and subsequently in Ceres. Under the assumption that most of volatiles were not vaporized during the accretion phase and the thermal evolution of Ceres, we determine the per mass abundances with respect to H₂O of CO₂, CO, CH₄, N₂, NH₃, Ar, Xe and Kr in the interior of the asteroid. The Dawn space mission, scheduled to explore Ceres in August 2014, may have the capacity to test some predictions. We also show that an in situ measurement of the D/H ratio in H₂O in Ceres could constrain the distance range in the solar nebula where its icy planetesimals were produced.

Title:		Reanalysis of asteroid families structure through visible spectroscopy
Authors:		Mothé-Diniz, T.; Roig, F.; Carvano, J. M.
Affiliation:		AA(Observatório Nacional, CAA, Rio de Janeiro, Brazil; Observatoire de Paris/Meudon, LESIA, 5 Place Jules Janssen, Bâtiment 10, 92150 Meudon Cedex, France; ), AB(Observatório Nacional, CAA, Rio de Janeiro, Brazil), AC(Observatório Nacional, CAA, Rio de Janeiro, Brazil; Observatoire de Paris/Meudon, LESIA, 5 Place Jules Janssen, Bâtiment 10, 92150 Meudon Cedex, France)
Journal:		Icarus, Volume 174, Issue 1, p. 54-80. (Icarus Homepage)
Publication Date:		03/2005
Origin:		ELSEVIER
Keywords:		Asteroids, Spectroscopy
Abstract Copyright:		Elsevier Inc.
DOI:		10.1016/j.icarus.2004.10.002
Bibliographic Code:		2005Icar..174...54M

Abstract

The taxonomic properties of the main asteroid families are analyzed and discussed in the light of an updated definition of the families using a large proper elements database and the asteroids taxonomy derived from reflectance spectra recently obtained by two large visible spectroscopic surveys: the SMASS II and the S3OS2. Our analysis indicates that most families are quite homogeneous taxonomically and mineralogically—whenever there exists a mineralogical constraint—, being probably originated from homogeneous parent bodies. The exceptions are the Nysa family, that should likely be considered a clan, and the Eos family that encompasses a broad range of taxonomies, whose mineralogical relations cannot be completely ruled out. Only in a few cases the families may be taxonomically distinguished from the background population. That is the case of the Minerva/Gefion, Adeona, Dora, Merxia, Hoffmeister, Koronis, Eos, and Veritas families. Some of the families presented in this work show a larger spectral diversity than previously reported, as it is the case for the Maria and Koronis families. On the other hand, the Veritas family is found to be homogeneous, in sharp contrast with previous works. Mineralogical relations are reported whenever they could be found in the literature and we examine the possible constraints posed by the presence of different taxonomies in certain families.

Title:		Meteoritic and other constraints on the internal structure and impact history of small asteroids
Authors:		Scott, Edward R. D.; Wilson, Lionel
Affiliation:		Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Manoa, Honolulu, HI 96822, USA. Corresponding author. Fax: +1-808-956-6322.;
Journal:		Icarus, Volume 174, Issue 1, p. 46-53. (Icarus Homepage)
Publication Date:		03/2005
Origin:		ELSEVIER
Keywords:		Asteroids, Meteorites, Impact processes, asteroids, Ceres, Eros, Gaspra, Ida, Mathilde, Vesta
Abstract Copyright:		Elsevier Inc.
DOI:		10.1016/j.icarus.2004.10.014
Bibliographic Code:		2005Icar..174...46S

Abstract

Studies of the internal structure of asteroids, which are crucial for understanding their impact history and for hazard mitigation, appear to be in conflict for the S-type asteroids, Eros, Gaspra, and Ida. Spacecraft images and geophysical data show that they are fractured, coherent bodies, whereas models of catastrophic asteroidal impacts, family and satellite formation, and studies of asteroid spin rates, and other diverse properties of asteroids and planetary craters suggest that such asteroids are gravitationally bound aggregates of rubble. These conflicting views may be reconciled if 10-50 km S-type asteroids formed as rubble piles, but were later consolidated into coherent bodies. Many meteorites are breccias that testify to a long history of impact fragmentation and consolidation by alteration, metamorphism, igneous and impact processes. Ordinary chondrites, which are the best analogs for S asteroids, are commonly breccias. Some may have formed in cratering events, but many appear to have formed during disruption and reaccretion of their parent asteroids. Some breccias were lithified during metamorphism, and a few were lithified by injected impact melt, but most are regolith and fragmental breccias that were lithified by mild or moderate shock, like their lunar analogs. Shock experiments show that porous chondritic powders can be consolidated during mild shock by small amounts of silicate melt that glues grains together, and by friction and pressure welding of silicate and metallic Fe,Ni grains. We suggest that the same processes that converted impact debris into meteorite breccias also consolidated asteroidal rubble. Internal voids would be partly filled with regolith by impact-induced seismic shaking. Consolidation of this material beneath large craters would lithify asteroidal rubble to form a more coherent body. Fractures on Ida that were created by antipodal impacts and are concentrated in and near large craters, and small positive gravity anomalies associated with the Psyche and Himeros craters on Eros, are consistent with this concept. Spin data suggest that smaller asteroids 0.6-6 km in size are unconsolidated rubble piles. C-type asteroids, which are more porous than S-types, and their analogs, the volatile-rich carbonaceous chondrites, were probably not lithified by shock.

Title:		Space weathering and the low sulfur abundance of Eros
Authors:		Kracher, Alfred; Sears, Derek W. G.
Affiliation:		Center for Space and Planetary Sciences and Department of Chemistry and Biochemistry, 101 Chemistry Building, University of Arkansas, Fayetteville, AR 72701, USA. Corresponding author. Current address: Ames Laboratory (USDOE), 227 Wilhelm Hall, Iowa State University, Ames, IA 50011-3020, USA.;
Journal:		Icarus, Volume 174, Issue 1, p. 36-45. (Icarus Homepage)
Publication Date:		03/2005
Origin:		ELSEVIER
Abstract Copyright:		Elsevier Inc.
DOI:		10.1016/j.icarus.2004.10.010
Bibliographic Code:		2005Icar..174...36K

Abstract

The surprisingly low S/Si ratio of Asteroid 433 Eros measured by the NEAR Shoemaker spacecraft probably reflects a surface depletion rather than a bulk property of the asteroid. The sulfur X-ray signal originates at a depth <10 μm in the regolith. The most efficient process for vaporizing minerals at the heliocentric distance of Eros are sputtering by solar wind ions and hypervelocity impacts. These are the same processes that account for the changes in optical properties of asteroids attributed to "space weathering" of lunar surface materials, although the relative importance of sputtering and impacts need not be the same for the Moon and asteroids. Troilite, FeS, which is the most important sulfide mineral in meteorites, and presumably on S-type asteroids like Eros, can be vaporized by much less energy than other major minerals, and will therefore be preferentially lost. Within 10⁶ years either process can remove sulfide from the top 10-100 μm of regolith. Sulfur will be lost into space and some sulfur will migrate to deeper regolith layers. We also consider other possible mechanisms of surficial sulfur depletion, such as mineral segregation in the regolith and perhaps even incipient melting. Although we consider solar wind sputtering the most likely cause of the sulfur depletion on Eros, we cannot entirely rule out other processes as causes of the sulfur deficiency. Laboratory simulations of the relevant processes can address some of the open questions. Simulations will have to be carried out in such a way that potential sulfur loss processes as well as resurfacing can be studied simultaneously, requiring a large and complex environmental chamber.

Title:		Spectral alteration of the Meteorite Epinal (H5) induced by heavy ion irradiation: a simulation of space weathering effects on near-Earth asteroids
Authors:		Strazzulla, G.; Dotto, E.; Binzel, R.; Brunetto, R.; Barucci, M. A.; Blanco, A.; Orofino, V.
Affiliation:		AA(INAF—Osservatorio Astrofisico di Catania, Via S. Sofia 78, I-95123 Catania, Italy; ), AB(INAF—Osservatorio Astronomico di Roma, Italy), AC(Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA), AD(INAF—Osservatorio Astrofisico di Catania, Via S. Sofia 78, I-95123 Catania, Italy), AE(LESIA, Observatoire de Paris, 92195 Meudon Principal Cedex, France), AF(Dipartimento di Fisica, Università di Lecce, Italy), AG(Dipartimento di Fisica, Università di Lecce, Italy)
Journal:		Icarus, Volume 174, Issue 1, p. 31-35. (Icarus Homepage)
Publication Date:		03/2005
Origin:		ELSEVIER
Keywords:		Meteorites, Spectroscopy, Experimental techniques, Radiation chemistry, Asteroid surfaces
Abstract Copyright:		Elsevier Inc.
DOI:		10.1016/j.icarus.2004.09.013
Bibliographic Code:		2005Icar..174...31S

Abstract

We present results obtained for Epinal (H5), an ordinary chondrite meteorite, irradiated with 60 keV Ar⁺⁺ ions, simulating solar wind heavy particle irradiation. Bidirectional reflectance spectra (0.3-2.67 μm) measured after irradiating Epinal samples with different ion fluences exhibit a progressive reddening that is similar to the spread of spectra observed for S-type near-Earth asteroids. The timescales for inducing the same effects in space as those obtained in laboratory are estimated to be 10⁴-10⁶ yr. These results suggest irradiation by heavy ions may be a very efficient weathering process in near-Earth space.

Title:		Statistical analysis of asteroidal and cometary polarization phase curves
Authors:		Penttilä, A.; Lumme, K.; Hadamcik, E.; Levasseur-Regourd, A.-C.
Affiliation:		AA(Observatory, University of Helsinki, PO Box 14, 00014 University of Helsinki, Finland ), AB(Observatory, University of Helsinki, PO Box 14, 00014 University of Helsinki, Finland), AC(Université Paris VI/Aéronomie CNRS-IPSL, BP 3, 92371 Verrières, France), AD(Université Paris VI/Aéronomie CNRS-IPSL, BP 3, 92371 Verrières, France)
Journal:		Astronomy and Astrophysics, Volume 432, Issue 3, March IV 2005, pp.1081-1090 (A&A Homepage)
Publication Date:		03/2005
Origin:		EDP
Keywords:		polarization, methods: statistical, techniques: polarimetric, astronomical data bases: miscellaneous, comets: general, minor planets, asteroids
DOI:		10.1051/0004-6361:20042133
Bibliographic Code:		2005A&A...432.1081P

Abstract

We use an empirical polarization phase curve model at various wavelengths to predict some statistical properties of comets and asteroids. First, we show how our model with Bayesian MCMC numerical methods predicts polarization behaviour at larger phase angles when only the smaller angle data are used. Our empirical model incorporates both the phase and colour dependency on the same footing. Second, a comparison between the existing taxonomy of asteroids and the clustering of asteroid classes based on polarization suggests a new method for the classification. We also heavily concentrate on the derivations of quantitative errors in our analysis.

Title:		A study of Cybele asteroids
Authors:		Lagerkvist, C.-I.; Moroz, L.; Nathues, A.; Erikson, A.; Lahulla, F.; Karlsson, O.; Dahlgren, M.
Affiliation:		AA(Astronomical Observatory, Box 515, 751 20 Uppsala, Sweden ), AB(DLR, Optical Information Systems, Rutherfordstrasse 2, 12489 Berlin, Germany), AC(Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Strasse 2, 37191 Katlenburg-Lindau, Germany), AD(DLR, Institute of Planetary Research, Rutherfordstrasse 2, 12489 Berlin, Germany), AE(Observatorio Astronomico, Alfonso XII 3, 28014 Madrid, Spain), AF(Astronomical Observatory, Box 515, 751 20 Uppsala, Sweden), AG(Astronomical Observatory, Box 515, 751 20 Uppsala, Sweden)
Journal:		Astronomy and Astrophysics, Volume 432, Issue 1, March II 2005, pp.349-354 (A&A Homepage)
Publication Date:		03/2005
Origin:		A&A
Keywords:		minor planets, asteroids
DOI:		10.1051/0004-6361:20041152
Bibliographic Code:		2005A&A...432..349L

Abstract

We have used the 3.5 m New Technology Telescope at ESO, La Silla, to obtain spectra of 18 asteroids belonging to the Cybele group. One additional Cybele asteroid was observed with the ESO 3.6 m telescope. From the spectra we have derived spectral slopes and taxonomy classifications. Our observations show that spectrally red D-type Cybeles tend to be smaller than more spectrally neutral P- and C-type objects from this group. Similar colour-diameter trends have previously been reported for other outer belt low albedo asteroids (Hildas and Trojans). We discuss possible reasons for this trend. In particular, the observed dominance of red objects for small diameters is consistent with a space weathering scenario, where irradiation of asteroid regoliths with solar wind plasma neutralizes their surface colours due to carbonization of originally reddish organic components. Collisional disruption of such large greyish "aged" P-type objects would produce a number of redder D-type fragments lacking mature regoliths. In addition, the observed colour-diameter trend may be due to compositional differences between D-, P- and C-type asteroids. P- and C-types may be lacking at small diameters, since their materials are less susceptible to collisional break-up than spectrally red D-type material. A simultaneous contribution of both factors (compositional differences and space weathering) to the observed trend is possible as well.

Observations were made at the European Southern Observatory (ESO) with the NTT telescope under program 56.F-0355 and the 3.6 m telescope under program 62.S-0133.

Title:		Negative report of occultation by the D-type asteroid (773) Irmintraud
Authors:		Christou, A.; Bailey, M.
Journal:		The Observatory, Vol. 125, p. 23-24
Publication Date:		02/2005
Origin:		OBS
Bibliographic Code:		2005Obs...125...23C

Abstract

Not Available

Title:		A closer look at main belt asteroids 1: WF/PC images
Authors:		Storrs, A. D.; Dunne, C.; Conan, J.-M.; Mugnier, L.; Weiss, B. P.; Zellner, B.
Affiliation:		AA(Department of Physics, Astronomy, and Geosciences, Towson University, 8000 York Road, Towson, MD 21252, USA; ), AB(Towson H.S., Cedar Ave., Towson, MD 410-887-3608, USA), AC(ONERA, Département d'Optique Theorique et Appliquee, BP 72, F-92322 Chatillon cedex, France), AD(ONERA, Département d'Optique Theorique et Appliquee, BP 72, F-92322 Chatillon cedex, France), AE(Department of Earth, Atmospheric, and Planetary Sciences, 54-724 Massachusetts Institute of Technology, Cambridge, MA 02139, USA), AF(Department of Physics, GA Southern University, Landrum Box 8031, Statesboro, GA 30460, USA)
Journal:		Icarus, Volume 173, Issue 2, p. 409-416. (Icarus Homepage)
Publication Date:		02/2005
Origin:		ELSEVIER
Keywords:		Main-belt asteroids, Image processing
Abstract Copyright:		Elsevier Inc.
DOI:		10.1016/j.icarus.2004.08.007
Bibliographic Code:		2005Icar..173..409S

Abstract

We present new reconstructions of images of main belt Asteroids 9 Metis, 18 Melpomene, 19 Fortuna, 216 Kleopatra, and 624 Hektor, made with the uncorrected Wide-Field/Planetary Camera (WF/PC) on the Hubble Space Telescope (HST). Deconvolution with the MISTRAL algorithm demonstrates that these asteroids are clearly resolved. We determine diameters, albedos, and lower limits to axial ratios for these bodies. We also review the process used to restore the aberrated images. No surface features or companions are found, but the rotation of 216 Kleopatra is clearly seen. The asteroidal albedos are similar to those determined by other procedures.

Title:		Thermal infrared (8-13 μm) spectra of 29 asteroids: the Cornell Mid-Infrared Asteroid Spectroscopy (MIDAS) Survey
Authors:		Lim, Lucy F.; McConnochie, Timothy H.; Bell, James F.; Hayward, Thomas L.
Affiliation:		AA(Department of Astronomy, Cornell University, Ithaca, NY 14853, USA; NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA; ), AB(Department of Astronomy, Cornell University, Ithaca, NY 14853, USA), AC(Department of Astronomy, Cornell University, Ithaca, NY 14853, USA), AD(Gemini South Observatory, AURA/Casilla 603, La Serena, Chile)
Journal:		Icarus, Volume 173, Issue 2, p. 385-408. (Icarus Homepage)
Publication Date:		02/2005
Origin:		ELSEVIER
Keywords:		surfaces, Spectroscopy, Infrared observations, Ceres, Vesta
Abstract Copyright:		Elsevier Inc.
DOI:		10.1016/j.icarus.2004.08.005
Bibliographic Code:		2005Icar..173..385L

Abstract

We report the results of the Cornell Mid-IR Asteroid Spectroscopy (MIDAS) survey, a program of ground-based observations designed to characterize the 8-13 μm spectral properties of a statistically significant sample of asteroids from a wide variety of visible to near-IR spectral classes. MIDAS is conducted at Palomar Observatory using the Spectrocam-10 (SC-10) spectrograph on the 200-in Hale telescope. We have measured the mid-infrared spectra of twenty-nine asteroids and have derived temperature estimates from our data that are largely consistent with the predictions of the standard thermal model. We have also generated relative emissivity spectra for the target asteroids. On only one asteroid, 1 Ceres, have we found emissivity features with spectral contrast greater than 5%. Our spectrum of 4 Vesta suggests emissivity variation at the 2-3% level. Published spectra of several of the small number of asteroids observed with ISO (six of which are also included in our survey), which appeared to exhibit much stronger emissivity features, are difficult to reconcile with our measurements. Laboratory work on mineral and meteorite samples has shown that the contrast of mid-IR spectral features is greatly reduced at fine grain sizes. Moreover, the NEAR mission found that 433 Eros is covered by a relatively thick fine-grained regolith. If small bodies in general possess such regoliths, their mid-IR spectral features may be quite subtle. This may explain the evident absence of strong emissivity variation in the majority of the MIDAS spectra.

Title:		Numerical experiments with rubble piles: equilibrium shapes and spins
Authors:		Richardson, Derek C.; Elankumaran, Pradeep; Sanderson, Robyn E.
Affiliation:		Department of Astronomy, Computer and Space Sciences Building, Stadium Drive, University of Maryland, College Park, MD 20740-2421, USA. Corresponding author. Fax: +1-301-314-9067.;
Journal:		Icarus, Volume 173, Issue 2, p. 349-361. (Icarus Homepage)
Publication Date:		02/2005
Origin:		ELSEVIER
Keywords:		Asteroids, Planetesimals, Rotational dynamics, Solid body tides, Satellites of Jupiter
Abstract Copyright:		Elsevier Inc.
DOI:		10.1016/j.icarus.2004.09.007
Bibliographic Code:		2005Icar..173..349R

Abstract

We present numerical experiments investigating the shape and spin limits of self-gravitating "perfect" rubble piles that consist of identical, smooth, rigid, spherical particles with configurable normal coefficient of restitution and no sliding friction. Such constructs are currently employed in a variety of investigations, ranging from the formation of asteroid satellites to the dynamical properties of Saturn's densest rings. We find that, owing to cannonball stacking behavior, rubble piles can maintain non-spherical shapes without bulk spin, unlike a fluid, and can spin faster than a perfect fluid before shedding mass, consistent with the theory for the more general continuum rubble pile model (Holsapple, 2004, Icarus 172, 272-303). Rubble piles that reassemble following a catastrophic disruption reconfigure themselves to lie within stability limits predicted by the continuum theory. We also find that coarse configurations consisting of a small number of particles are more resistant to tidal disruption than fine configurations with many particles. Overall this study shows that idealized rubble piles behave qualitatively in a manner similar to certain granular materials, at least in the limit where global shape readjustments and/or mass shedding begins. The limits obtained here may provide constraints on the possible internal structure of some small Solar System bodies that have extreme shapes or are under high stress. Amalthea is presented as a case study.

Title:		The W isotope composition of eucrite metals: constraints on the timing and cause of the thermal metamorphism of basaltic eucrites
Authors:		Kleine, T.; Mezger, K.; Palme, H.; Scherer, E.; Münker, C.
Affiliation:		AA(Zentrallabor für Geochronologie, Institut für Mineralogie, Universität Münster, Corrensstr. 24, D-48149 Münster, Germany), AB(Zentrallabor für Geochronologie, Institut für Mineralogie, Universität Münster, Corrensstr. 24, D-48149 Münster, Germany), AC(Institut für Mineralogie und Geochemie, Universität zu Köln, Zülpicherstr. 49b, D-50476 Köln, Germany), AD(Zentrallabor für Geochronologie, Institut für Mineralogie, Universität Münster, Corrensstr. 24, D-48149 Münster, Germany), AE(Zentrallabor für Geochronologie, Institut für Mineralogie, Universität Münster, Corrensstr. 24, D-48149 Münster, Germany)
Journal:		Earth and Planetary Science Letters, Volume 231, Issue 1-2, p. 41-52. (E&PSL Homepage)
Publication Date:		02/2005
Origin:		ELSEVIER
DOI:		10.1016/j.epsl.2004.12.016
Bibliographic Code:		2005E&PSL.231...41K

Title:		433 Eros - comparison of lightcurve extrema from 1901-1931 with the present rotation state
Authors:		Ďurech, J.
Affiliation:		Astronomical Institute, Charles University in Prague, V Holešovičkách 2, 18000 Prague, Czech Republic
Journal:		Astronomy and Astrophysics, v.431, p.381-383 (2005) (A&A Homepage)
Publication Date:		02/2005
Origin:		A&A
A&A Keywords:		minor planets, asteroids, methods: data analysis
DOI:		10.1051/0004-6361:20042095
Bibliographic Code:		2005A&A...431..381D

Title:		Spacecraft exploration of asteroids
Authors:		Shevchenko, V. G.; Mohamed, R. A.
Affiliation:		AA(Institute of Astronomy of Kharkiv National University), AB(Department of Physics, Faculty of Science, University of Garyounis)
Journal:		Solar System Research, Volume 39, Issue 1, pp.73-81
Publication Date:		01/2005
Origin:		SPRINGER
Abstract Copyright:		(c) 2005: MAIK “Nauka/Interperiodica”
DOI:		10.1007/s11208-005-0020-7
Bibliographic Code:		2005SoSyR..39...73S

Title:		Yarkovsky detection opportunities. I. Solitary asteroids
Authors:		Vokrouhlický, D.; Čapek, D.; Chesley, S. R.; Ostro, S. J.
Affiliation:		AA(Institute of Astronomy, Charles University, V Holešovičkách 2, CZ-18000 Prague 8, Czech Republic; ), AB(Institute of Astronomy, Charles University, V Holešovičkách 2, CZ-18000 Prague 8, Czech Republic), AC(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA), AD(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA)
Journal:		Icarus, Volume 173, Issue 1, p. 166-184. (Icarus Homepage)
Publication Date:		01/2005
Origin:		ELSEVIER
Keywords:		Asteroids, Yarkovsky effect, Orbit determination
Abstract Copyright:		Elsevier Inc.
DOI:		10.1016/j.icarus.2004.08.002
Bibliographic Code:		2005Icar..173..166V

Title:		Physical characteristics of Hayabusa target Asteroid 25143 Itokawa
Authors:		Lederer, S. M.; Domingue, D. L.; Vilas, F.; Abe, M.; Farnham, T. L.; Jarvis, K. S.; Lowry, S. C.; Ohba, Y.; Weissman, P. R.; French, L. M.; Fukai, H.; Hasegawa, S.; Ishiguro, M.; Larson, S. M.; Takagi, Y.
Affiliation:		AA(Planetary Astronomy Group, 2101 NASA Road 1, MC SR, NASA Johnson Space Center, Houston, TX 77058, USA; ), AB(Johns Hopkins University/Applied Physics Laboratory, 11100 Johns Hopkins Rd., Laurel, MD 20723, USA), AC(Planetary Astronomy Group, 2101 NASA Road 1, MC SR, NASA Johnson Space Center, Houston, TX 77058, USA), AD(Japanese Aerospace Exploration Agency/Institute of Space and Astronautical Science, 3-1-1, Yoshinodai, Sagamihara, Kanagawa, 229-8510, Japan), AE(Department of Astronomy, University of Maryland, College Park, MD 20742, USA), AF(Lockheed-Martin Space Operations, 2400 NASA Rd. 1, C-23, Houston, TX 77058, USA), AG(Earth and Space Sciences Division, Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA; Current address: Department of Physics, Queens University, Belfast, BT7 1NN, UK.), AH(Japanese Aerospace Exploration Agency/Institute of Space and Astronautical Science, 3-1-1, Yoshinodai, Sagamihara, Kanagawa, 229-8510, Japan), AI(Earth and Space Sciences Division, Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA), AJ(Department of Physics, Illinois Wesleyan University, PO Box 2900, Bloomington, IL 61701, USA), AK(Japanese Aerospace Exploration Agency/Institute of Space and Astronautical Science, 3-1-1, Yoshinodai, Sagamihara, Kanagawa, 229-8510, Japan), AL(Japanese Aerospace Exploration Agency/Institute of Space and Astronautical Science, 3-1-1, Yoshinodai, Sagamihara, Kanagawa, 229-8510, Japan), AM(Japanese Aerospace Exploration Agency/Institute of Space and Astronautical Science, 3-1-1, Yoshinodai, Sagamihara, Kanagawa, 229-8510, Japan), AN(Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA), AO(Toho Gakuen University, 3-11 Heiwagaoka, Meito-ku, Nagoya, 465-8515, Japan)
Journal:		Icarus, Volume 173, Issue 1, p. 153-165. (Icarus Homepage)
Publication Date:		01/2005
Origin:		ELSEVIER
Keywords:		asteroids, Asteroids, Photometry, Regoliths, composition
Abstract Copyright:		Elsevier Inc.
DOI:		10.1016/j.icarus.2004.07.022
Bibliographic Code:		2005Icar..173..153L

Title:		Evidence for asteroid space weathering from the Sloan Digital Sky Survey
Authors:		Nesvorný, David; Jedicke, Robert; Whiteley, Robert J.; Ivezić, Željko
Affiliation:		AA(Southwest Research Institute, 1050 Walnut St, Suite 400, Boulder, CO 80302, USA; ), AB(Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA), AC(Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA), AD(Princeton University Observatory, Princeton, NJ 08544, USA)
Journal:		Icarus, Volume 173, Issue 1, p. 132-152. (Icarus Homepage)
Publication Date:		01/2005
Origin:		ELSEVIER
Keywords:		Asteroids, Composition, Surfaces, Asteroids, Regoliths
Abstract Copyright:		Elsevier Inc.
DOI:		10.1016/j.icarus.2004.07.026
Bibliographic Code:		2005Icar..173..132N

Title:		Tumbling asteroids
Authors:		Pravec, P.; Harris, A. W.; Scheirich, P.; Kušnirák, P.; Šarounová, L.; Hergenrother, C. W.; Mottola, S.; Hicks, M. D.; Masi, G.; Krugly, Yu. N.; Shevchenko, V. G.; Nolan, M. C.; Howell, E. S.; Kaasalainen, M.; Galád, A.; Brown, P.; Degraff, D. R.; Lambert, J. V.; Cooney, W. R.; Foglia, S.
Affiliation:		AA(Astronomical Institute, Academy of Sciences of the Czech Republic, Fričova 1, CZ-25165 Ondřejov, Czech Republic; ), AB(Space Science Institute, Boulder, CO 80301, USA), AC(Astronomical Institute, Academy of Sciences of the Czech Republic, Fričova 1, CZ-25165 Ondřejov, Czech Republic), AD(Astronomical Institute, Academy of Sciences of the Czech Republic, Fričova 1, CZ-25165 Ondřejov, Czech Republic), AE(Astronomical Institute, Academy of Sciences of the Czech Republic, Fričova 1, CZ-25165 Ondřejov, Czech Republic), AF(Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA), AG(DLR Institute of Space Sensor Technology and Planetary Exploration, Rutherfordstr. 2, D-12489 Berlin, Germany), AH(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA), AI(Physics Department, University of Rome "Tor Vergata", Via della Ricerca Scientifica 1, 00133 Rome, Italy; Campo Catino Observatory, Guarcino, I-03016, Italy), AJ(Institute of Astronomy of Kharkiv National University, Sumska Str. 35, Kharkiv 61022, Ukraine), AK(Institute of Astronomy of Kharkiv National University, Sumska Str. 35, Kharkiv 61022, Ukraine), AL(Arecibo Observatory, National Astronomy and Ionosphere Center, PR 00612, USA), AM(Arecibo Observatory, National Astronomy and Ionosphere Center, PR 00612, USA), AN(Department of Mathematics/Rolf Nevanlinna Institute, University of Helsinki, PO Box 4, FIN-00014, Finland), AO(Modra Observatory, Astronomical Institute, FMFI Comenius University, Bratislava, Slovak Republic; Astronomical Institute, Academy of Sciences of the Czech Republic, Fričova 1, CZ-25165 Ondřejov, Czech Republic), AP(Department of Physics and Astronomy, University of Western Ontario, London, ON N6A 3K7, Canada), AQ(Alfred University, 1 Saxon Drive, Alfred, NY 14802, USA), AR(Air Force Maui Optical and Supercomputing Facility, Kihei, HI 96753, USA), AS(Blackberry Observatory, 1927 Fairview Dr., Port Allen, LA 70767, USA), AT(Serafino Zani Observatory, Lumezzane, I-25065, Italy)
Journal:		Icarus, Volume 173, Issue 1, p. 108-131. (Icarus Homepage)
Publication Date:		01/2005
Origin:		ELSEVIER
Keywords:		Asteroids, Excited rotation, Photometry
Abstract Copyright:		Elsevier Inc.
DOI:		10.1016/j.icarus.2004.07.021
Bibliographic Code:		2005Icar..173..108P

Title:		Quantification of porosity and surface roughness in laboratory measurements of the bidirectional reflectance of asteroid surface analogues
Authors:		Sakai, T.; Nakamura, A. M.
Affiliation:		AA(Graduate School of Science and Technology, Kobe University, 1-1 Rokkodai, Nada, Kobe, Japan)
Journal:		Earth, Planets and Space, Volume 57, p. 71-76. (EP&S Homepage)
Publication Date:		01/2005
Origin:		TERRAPUB
Abstract Copyright:		(c) 2005 The Society of Geomagnetism and Earth, Planetary and Space Sciences (SGEPSS); The Seismological Society of Japan; The Volcanological Society of Japan; The Geodetic Society of Japan; The Japanese Society for Planetary Sciences
Bibliographic Code:		2005EP&S...57...71S

Title:		A First Look at the Damocloids
Authors:		Jewitt, David
Affiliation:		AA(Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822; )
Journal:		The Astronomical Journal, Volume 129, Issue 1, pp. 530-538. (AJ Homepage)
Publication Date:		01/2005
Origin:		UCP
AJ Keywords:		Comets: General, Kuiper Belt, Minor Planets, Asteroids
Abstract Copyright:		(c) 2005: The American Astronomical Society
DOI:		10.1086/426328
Bibliographic Code:		2005AJ....129..530J

Title:		Determination of the mass of (4) Vesta based on new close approaches
Authors:		Kovačević, A.
Affiliation:		Department of Astronomy, Faculty of Mathematics, University of Belgrade, Studentski trg 16, 11000 Belgrade, Serbia and Montenegro
Journal:		Astronomy and Astrophysics, v.430, p.319-325 (2005) (A&A Homepage)
Publication Date:		01/2005
Origin:		A&A
A&A Keywords:		celestial mechanics, astrometry
DOI:		10.1051/0004-6361:20035872
Bibliographic Code:		2005A&A...430..319K

Title:		Asteroid target selection for the new Rosetta mission baseline. 21 Lutetia and 2867 Steins
Authors:		Barucci, M. A.; Fulchignoni, M.; Fornasier, S.; Dotto, E.; Vernazza, P.; Birlan, M.; Binzel, R. P.; Carvano, J.; Merlin, F.; Barbieri, C.; Belskaya, I.
Affiliation:		AA(LESIA, Observatoire de Paris, 92195 Meudon Principal Cedex, France ), AB(LESIA, Observatoire de Paris, 92195 Meudon Principal Cedex, France ), AC(Astronomy Department, Padova University, Vicolo dell'Osservatorio 2, 35122 Padova, Italy), AD(INAF - Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monte Porzio Catone, Roma, Italy), AE(LESIA, Observatoire de Paris, 92195 Meudon Principal Cedex, France), AF(IMCCE, Observatoire de Paris, 75014 Paris, France), AG(Dep. of Earth, Atmosph. and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA), AH(LESIA, Observatoire de Paris, 92195 Meudon Principal Cedex, France), AI(LESIA, Observatoire de Paris, 92195 Meudon Principal Cedex, France), AJ(Astronomy Department, Padova University, Vicolo dell'Osservatorio 2, 35122 Padova, Italy), AK(Astronomical Observatory of Kharkiv National University, Ukrania)
Journal:		Astronomy and Astrophysics, v.430, p.313-317 (2005) (A&A Homepage)
Publication Date:		01/2005
Origin:		A&A
A&A Keywords:		minor planets, asteroids, techniques: spectroscopic
DOI:		10.1051/0004-6361:20041505
Bibliographic Code:		2005A&A...430..313B

Title:		Photometric Observations of a Very Young Family-Member Asteroid (832) Karin
Authors:		Yoshida, Fumi; Dermawan, Budi; Ito, Takashi; Sawabe, Yu; Haji, Masashige; Saito, Ryoko; Hirai, Masanori; Nakamura, Tsuko; Sato, Yusuke; Yanagisawa, Toshifumi; Malhotra, Renu
Affiliation:		AA(National Astronomical Observatory, Osawa, Mitaka, Tokyo 181-8588) AB(School of Science, The University of Tokyo, Hongo, Bunkyo-ku, Tokyo 113-0033; Department of Astronomy, Bandung Institute of Technology, Bandung 40132, Indonesia) AC(Lunar and Planetary Laboratory, The University of Arizona, Tucson, AZ 85721-0092, USA) AD(Department of Earth Sciences and Astronomy, Fukuoka University of Education, 1-1 Akama-bunkyo-machi, Munakata, Fukuoka 811-4192) AE(Department of Earth Sciences and Astronomy, Fukuoka University of Education, 1-1 Akama-bunkyo-machi, Munakata, Fukuoka 811-4192) AF(Department of Earth Sciences and Astronomy, Fukuoka University of Education, 1-1 Akama-bunkyo-machi, Munakata, Fukuoka 811-4192) AG(Department of Earth Sciences and Astronomy, Fukuoka University of Education, 1-1 Akama-bunkyo-machi, Munakata, Fukuoka 811-4192) AH(National Astronomical Observatory, Osawa, Mitaka, Tokyo 181-8588) AI(Department of Earth Science and Astronomy, Graduate School of Arts and Sciences, The University of Tokyo, Komaba, Meguro-ku, Tokyo 153-8902) AJ(Department of Earth Science and Astronomy, Graduate School of Arts and Sciences, The University of Tokyo, Komaba, Meguro-ku, Tokyo 153-8902; Japan Aerospace Exploration Agency, Institute of Space Technology and Aeronautics, 7-44-1 Jindaiji-higashi-machi, Chofu, Tokyo 182-8522) AK(Lunar and Planetary Laboratory, The University of Arizona, Tucson, AZ 85721-0092, USA)
Journal:		Publications of the Astronomical Society of Japan, Vol.56, No.6, pp. 1105-1113 (PASJ Homepage)
Publication Date:		12/2004
Origin:		PASJ
Keywords:		minor planets, asteroids: individual (Karin), minor planets, asteroids: photometry
Abstract Copyright:		(c) 2004: Astronomical Society of Japan
Bibliographic Code:		2004PASJ...56.1105Y

Title:		A Shape-and-Density Model of the Putative Binary EKBO 2001 QG298
Authors:		Takahashi, Shigeru; Ip, Wing-Huen
Affiliation:		AA(Institute of Space Science, National Central University, 300 Jungda Road, Chung-Li, Tao-Yuan, 32054, Taiwan; ; ) AB(Institute of Space Science, National Central University, 300 Jungda Road, Chung-Li, Tao-Yuan, 32054, Taiwan; )
Journal:		Publications of the Astronomical Society of Japan, Vol.56, No.6, pp. 1099-1103 (PASJ Homepage)
Publication Date:		12/2004
Origin:		PASJ
Keywords:		Kuiper Belt, minor planets, asteroids, planets and satellites: individual (Janus)
Abstract Copyright:		(c) 2004: Astronomical Society of Japan
Bibliographic Code:		2004PASJ...56.1099T

Title:		The YORP effect with finite thermal conductivity
Authors:		Čapek, D.; Vokrouhlický, D.
Affiliation:		Institute of Astronomy, Charles University, Prague, V Holešovičkách 2, CZ-18000 Prague 8, Czech Republic. Corresponding author. Fax: +420-2-2191-2567.
Journal:		Icarus, Volume 172, Issue 2, p. 526-536. (Icarus Homepage)
Publication Date:		12/2004
Origin:		ELSEVIER
Keywords:		rotation, Meteoroids, YORP effect
Abstract Copyright:		Elsevier Inc.
DOI:		10.1016/j.icarus.2004.07.003
Bibliographic Code:		2004Icar..172..526C

Title:		Photometric analysis of Eros from NEAR data
Authors:		Li, Jianyang; A'Hearn, Michael F.; McFadden, Lucy A.
Affiliation:		Department of Astronomy, University of Maryland, College Park, MD 20742, USA. Corresponding author.;
Journal:		Icarus, Volume 172, Issue 2, p. 415-431. (Icarus Homepage)
Publication Date:		12/2004
Origin:		ELSEVIER
Keywords:		433 Eros, Photometry, NEAR
Abstract Copyright:		Elsevier Inc.
DOI:		10.1016/j.icarus.2004.07.024
Bibliographic Code:		2004Icar..172..415L

Title:		Infrared spectroscopic observations of 69230 Hermes (1937 UB): possible unweathered endmember among ordinary chondrite analogs
Authors:		Rivkin, A. S.; Binzel, R. P.; Sunshine, J.; Bus, S. J.; Burbine, T. H.; Saxena, A.
Affiliation:		AA(Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, 54-418, 77 Massachusetts Avenue, Cambridge, MA 02139, USA; ), AB(Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, 54-418, 77 Massachusetts Avenue, Cambridge, MA 02139, USA), AC(Science Applications International Corporation, 5180 Parkstone Dr. Chantilly, VA 20151, USA), AD(Institute for Astronomy, 640 North A'ohoku Place, Hilo, HI 96720, USA), AE(Laboratory for Extraterrestrial Physics, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA), AF(Needham High School, 609 Webster Street, Needham, MA 02494, USA)
Journal:		Icarus, Volume 172, Issue 2, p. 408-414. (Icarus Homepage)
Publication Date:		12/2004
Origin:		ELSEVIER
Keywords:		Asteroids, Asteroids near-Earth, Asteroids composition, Meteorites
Abstract Copyright:		Elsevier Inc.
DOI:		10.1016/j.icarus.2004.07.006
Bibliographic Code:		2004Icar..172..408R

Title:		Rotational lightcurves of asteroids belonging to families
Authors:		Alvarez-Candal, Alvaro; Duffard, René; Angeli, Cláudia A.; Lazzaro, Daniela; Fernández, Silvia
Affiliation:		AA(Observatório Nacional, MCT. Rua Gal. José Cristino 77, 20921-400, Rio de Janeiro, RJ, Brazil; ), AB(Observatório Nacional, MCT. Rua Gal. José Cristino 77, 20921-400, Rio de Janeiro, RJ, Brazil), AC(Observatório Nacional, MCT. Rua Gal. José Cristino 77, 20921-400, Rio de Janeiro, RJ, Brazil), AD(Observatório Nacional, MCT. Rua Gal. José Cristino 77, 20921-400, Rio de Janeiro, RJ, Brazil), AE(Observatorio Astronómico, Universidad Nacional de Córdoba, Laprida 854, 5000, Córdoba, Argentina)
Journal:		Icarus, Volume 172, Issue 2, p. 388-401. (Icarus Homepage)
Publication Date:		12/2004
Origin:		ELSEVIER
Keywords:		Asteroids, rotation, Photometry
Abstract Copyright:		Elsevier Inc.
DOI:		10.1016/j.icarus.2004.06.008
Bibliographic Code:		2004Icar..172..388A

Title:		Spectroscopy of X-Type Asteroids
Authors:		Clark, B. E.; Bus, S. J.; Rivkin, A. S.; Shepard, M. K.; Shah, S.
Affiliation:		AA(Department of Physics, Ithaca College, Ithaca, NY 14850-7288 ), AB(Institute for Astronomy, University of Hawaii, 640 North A`ohoku Place, Hilo, HI 96720-2700), AC(Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology,77 Massachusetts Avenue, Cambridge, MA 02139-4307), AD(Department of Geography and Geosciences, Bloomsburg University, 400 East 2nd Street,Bloomsburg, PA 17815-1301), AE(Ithaca College, Ithaca, NY 14850-7231)
Journal:		The Astronomical Journal, Volume 128, Issue 6, pp. 3070-3081. (AJ Homepage)
Publication Date:		12/2004
Origin:		UCP
AJ Keywords:		Minor Planets, Asteroids, Techniques: Spectroscopic
Abstract Copyright:		(c) 2004: The American Astronomical Society
DOI:		10.1086/424856
Bibliographic Code:		2004AJ....128.3070C

Title:		308 Polyxo: ISO-SWS spectrum up to 26 micron
Authors:		Dotto, E.; Barucci, M. A.; Brucato, J. R.; Müller, T. G.; Carvano, J.
Affiliation:		AA(INAF - Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio Catone (Roma), Italy ), AB(LESIA - Observatoire de Paris, 5 place J. Janssen, 92195 Meudon Cedex, France), AC(INAF - Osservatorio Astronomico di Capodimonte, via Moiariello 16, 80131 Napoli, Italy), AD(Max-Planck-Institut fuer extraterrestrische Physik, Giessenbachstrasse, 85748 Garching, Germany), AE(LESIA - Observatoire de Paris, 5 place J. Janssen, 92195 Meudon Cedex, France; Observatório Nacional/MCT, Coordenação de Astronomia e Astrofísica - CAA, 20921-400 Rio de Janeiro, Brazil)
Journal:		Astronomy and Astrophysics, v.427, p.1081-1084 (2004) (A&A Homepage)
Publication Date:		12/2004
Origin:		A&A
A&A Keywords:		minor planets, asteroids, radiation mechanisms: thermal, infrared: solar system, meteors, meteorites
DOI:		10.1051/0004-6361:20041638
Bibliographic Code:		2004A&A...427.1081D

Title:		Impact-Induced Seismic Activity on Asteroid 433 Eros: A Surface Modification Process
Authors:		Richardson, James E.; Melosh, H. Jay; Greenberg, Richard
Journal:		Science, Volume 306, Issue 5701, pp. 1526-1529 (2004).
Publication Date:		11/2004
Category:		PLANET SCI
Origin:		SCIENCE
DOI:		10.1126/science.1104731
Bibliographic Code:		2004Sci...306.1526R

Title:		Equilibrium figures of spinning bodies with self-gravity
Authors:		Holsapple, Keith A.
Affiliation:		Department of Aeronautics and Astronautics, University of Washington 352400, Seattle, WA 98195, USA. Fax: 206-543-0217.;
Journal:		Icarus, Volume 172, Issue 1, p. 272-303. (Icarus Homepage)
Publication Date:		11/2004
Origin:		ELSEVIER
Keywords:		Asteroids, rotation, Comets, Equilibrium shapes, Equilibrium figures, Stability
Abstract Copyright:		Elsevier Inc.
DOI:		10.1016/j.icarus.2004.05.023
Bibliographic Code:		2004Icar..172..272H

Title:		Visible spectroscopic and photometric survey of L5 Trojans: investigation of dynamical families
Authors:		Fornasier, S.; Dotto, E.; Marzari, F.; Barucci, M. A.; Boehnhardt, H.; Hainaut, O.; de Bergh, C.
Affiliation:		AA(Dipartimento di Astronomia, Università di Padova, Vicolo dell'Osservatorio, 2, 35122 Padova, Italy; ), AB(INAF—Osservatorio Astronomico di Roma, Italy), AC(Dipartimento di Fisica, Università di Padova, Italy), AD(LESIA—Observatoire de Paris, France), AE(Max-Planck-Institute for Astronomy, Germany), AF(European Southern Observatory, Chile), AG(LESIA—Observatoire de Paris, France)
Journal:		Icarus, Volume 172, Issue 1, p. 221-232. (Icarus Homepage)
Publication Date:		11/2004
Origin:		ELSEVIER
Keywords:		Asteroids, Photometry, Spectroscopy, Jupiter Trojans, Families
Abstract Copyright:		Elsevier Inc.
DOI:		10.1016/j.icarus.2004.06.015
Bibliographic Code:		2004Icar..172..221F

Title:		S³OS²: the visible spectroscopic survey of 820 asteroids
Authors:		Lazzaro, D.; Angeli, C. A.; Carvano, J. M.; Mothé-Diniz, T.; Duffard, R.; Florczak, M.
Affiliation:		AA(Observatório Nacional, R. Gal. José Cristino 77, 20921-400 Rio de Janeiro, Brazil; ), AB(Observatório Nacional, R. Gal. José Cristino 77, 20921-400 Rio de Janeiro, Brazil), AC(Observatório Nacional, R. Gal. José Cristino 77, 20921-400 Rio de Janeiro, Brazil), AD(Observatório Nacional, R. Gal. José Cristino 77, 20921-400 Rio de Janeiro, Brazil), AE(Observatório Nacional, R. Gal. José Cristino 77, 20921-400 Rio de Janeiro, Brazil), AF(CEFET, Departamento Física, Av. Sete de Setembro 3165, 8230-091 Curitiba, Brazil)
Journal:		Icarus, Volume 172, Issue 1, p. 179-220. (Icarus Homepage)
Publication Date:		11/2004
Origin:		ELSEVIER
Keywords:		Asteroids, composition, Spectroscopy, asteroids
Abstract Copyright:		Elsevier Inc.
DOI:		10.1016/j.icarus.2004.06.006
Bibliographic Code:		2004Icar..172..179L

Title:		Radar detection of near-Earth Asteroids 1915 Quetzalcoatl, 3199 Nefertiti, 3757 (1982 XB), and 4034 (1986 PA)
Authors:		Shepard, Michael K.; Benner, Lance A. M.; Ostro, Steven J.; Campbell, Donald B.; Shapiro, Irwin I.; Chandler, John F.
Affiliation:		AA(Department of Geography and Geosciences, Bloomsburg University, Bloomsburg, PA 17815, USA; ), AB(Jet Propulsion Laboratory, Pasadena, CA 91109, USA), AC(Jet Propulsion Laboratory, Pasadena, CA 91109, USA), AD(National Astronomy and Ionosphere Center, Cornell University, Ithaca, NY 14853, USA), AE(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA), AF(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA)
Journal:		Icarus, Volume 172, Issue 1, p. 170-178. (Icarus Homepage)
Publication Date:		11/2004
Origin:		ELSEVIER
Keywords:		Asteroids, Radar
Abstract Copyright:		Elsevier Inc.
DOI:		10.1016/j.icarus.2004.06.003
Bibliographic Code:		2004Icar..172..170S

Title:		Mature and Fresh Surfaces on the Newborn Asteroid Karin
Authors:		Sasaki, Takanori; Sasaki, Sho; Watanabe, Jun-ichi; Sekiguchi, Tomohiko; Yoshida, Fumi; Kawakita, Hideyo; Fuse, Tetsuharu; Takato, Naruhisa; Dermawan, Budi; Ito, Takashi
Affiliation:		AA(Department of Earth and Planetary Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan; .), AB(Department of Earth and Planetary Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan; .; National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan.), AC(National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan.), AD(National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan.), AE(National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan.), AF(Gunma Astronomical Observatory, 6860-86 Nakayama, Takayama, Gunma 377-0702, Japan.), AG(Subaru Telescope, National Astronomical Observatory of Japan, 650 North A'ohoku Place, Hilo, HI 96720.), AH(Subaru Telescope, National Astronomical Observatory of Japan, 650 North A'ohoku Place, Hilo, HI 96720.), AI(School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan.; Department of Astronomy, Bandung Institute of Technology, Bandung 40132, Indonesia.), AJ(National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan.; Lunar and Planetary Laboratory, University of Arizona, 1629 East University Boulevard, Tucson, AZ 85721.)
Journal:		The Astrophysical Journal, Volume 615, Issue 2, pp. L161-L164. (ApJ Homepage)
Publication Date:		11/2004
Origin:		UCP
ApJ Keywords:		Minor Planets, Asteroids, Solar System: General
Abstract Copyright:		(c) 2004: The American Astronomical Society
DOI:		10.1086/426431
Bibliographic Code:		2004ApJ...615L.161S

Title:		The Orbit and Albedo of Trans-Neptunian Binary (58534) 1997 CQ₂₉
Authors:		Noll, Keith S.; Stephens, Denise C.; Grundy, Will M.; Osip, David J.; Griffin, Ian
Affiliation:		AA(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218; , ), AB(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218; , ), AC(Lowell Observatory, 1400 West Mars Hill Road, Flagstaff, AZ 86001-4470 ), AD(Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101; ), AE(Greater Manchester Museum of Science and Industry, Liverpool Road,Manchester M3 4FP, UK; )
Journal:		The Astronomical Journal, Volume 128, Issue 5, pp. 2547-2552. (AJ Homepage)
Publication Date:		11/2004
Origin:		UCP
AJ Keywords:		Kuiper Belt, Minor Planets, Asteroids
Abstract Copyright:		(c) 2004: The American Astronomical Society
DOI:		10.1086/424535
Bibliographic Code:		2004AJ....128.2547N

Title:		Searching for the short timescale variations in the lightcurve of minor planet 1689 Floris-Jan in 1999 and 2002
Authors:		Toth, I.
Affiliation:		Konkoly Observatory, Budapest 1525 PO Box 67, Hungary
Journal:		Astronomy and Astrophysics, v.427, p.363-369 (2004) (A&A Homepage)
Publication Date:		11/2004
Origin:		A&A
A&A Keywords:		minor planets, asteroids, techniques: photometric
DOI:		10.1051/0004-6361:20034112
Bibliographic Code:		2004A&A...427..363T

Title:		Meteoritical evidence and constraints on asteroid impacts and disruption
Authors:		Guy, Consolmagno, S. J.; Britt, Daniel T.
Affiliation:		AA(Specola Vaticana, V-00120, Vatican City State), AB(Department of Physics, University of Central Florida, P.O. Box 162385, Orlando, FL 32816-2385, USA)
Journal:		Planetary and Space Science, Volume 52, Issue 12, p. 1119-1128. (P&SS Homepage)
Publication Date:		10/2004
Origin:		ELSEVIER
DOI:		10.1016/j.pss.2004.07.009
Bibliographic Code:		2004P&SS...52.1119G

Title:		Catastrophic disruption of asteroids and family formation: a review of numerical simulations including both fragmentation and gravitational reaccumulations
Authors:		Michel, Patrick; Benz, Willy; Richardson, Derek C.
Affiliation:		AA(Observatoire de la Côte d'Azur, B.P. 4229, 06304 Nice cedex 4, France), AB(Physikalisches Institut, Univ. Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland), AC(Department of Astronomy, University of Maryland, College Park, MD 20742-2421, USA)
Journal:		Planetary and Space Science, Volume 52, Issue 12, p. 1109-1117. (P&SS Homepage)
Publication Date:		10/2004
Origin:		ELSEVIER
DOI:		10.1016/j.pss.2004.07.008
Bibliographic Code:		2004P&SS...52.1109M

Title:		3782 Celle: Discovery of a binary system within the Vesta family of asteroids
Authors:		Ryan, W. H.; Ryan, E. V.; Martinez, C. T.
Affiliation:		AA(MRO/R&ED, New Mexico Institute of Mining and Technology, 801 Leroy Place, Socorro, NM 87801, USA), AB(MRO/R&ED, New Mexico Institute of Mining and Technology, 801 Leroy Place, Socorro, NM 87801, USA), AC(University of New Mexico, Department of Physics and Astronomy, Albuquerque, NM 87131, USA)
Journal:		Planetary and Space Science, Volume 52, Issue 12, p. 1093-1101. (P&SS Homepage)
Publication Date:		10/2004
Origin:		ELSEVIER
DOI:		10.1016/j.pss.2004.07.006
Bibliographic Code:		2004P&SS...52.1093R

Title:		Yarkovsky depletion and asteroid collisional evolution
Authors:		Penco, U.; dell'Oro, A.; Paolicchi, P.; Campo Bagatin, A.; La Spina, A.; Cellino, A.
Affiliation:		AA(Dipartimento di Fisica, Università di Pisa, Largo Pontecorvo 1, 56127 Pisa, Italy), AB(INAF, Osservatorio di Torino, Pino Torinese, TO, Italy), AC(Dipartimento di Fisica, Università di Pisa, Largo Pontecorvo 1, 56127 Pisa, Italy), AD(Departamento de Fisica, Universidad de Alicante, C.tra San Vicente, San Vicente del Raspeig, Alicante, Spain), AE(Dipartimento di Matematica, Università di Pisa, via Buonarroti 2, Pisa, Italy), AF(INAF, Osservatorio di Torino, Pino Torinese, TO, Italy)
Journal:		Planetary and Space Science, Volume 52, Issue 12, p. 1087-1091. (P&SS Homepage)
Publication Date:		10/2004
Origin:		ELSEVIER
DOI:		10.1016/j.pss.2004.07.005
Bibliographic Code:		2004P&SS...52.1087P