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
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Title: |
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Widespread magma oceans on asteroidal bodies in the early Solar System |
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Authors: |
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Greenwood, Richard C.; Franchi, Ian A.; Jambon, Albert; Buchanan, Paul C. |
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Journal: |
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Nature, Volume 435, Issue 7044, pp. 916-918 (2005). (Nature Homepage) |
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Publication Date: |
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06/2005 |
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Origin: |
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NATURE |
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Abstract Copyright: |
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(c) 2005: Nature |
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DOI: |
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Bibliographic Code: |
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2005Natur.435..916G |
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.
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Title: |
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Yarkovsky origin of the unstable asteroids in the 2/1 mean motion resonance with Jupiter |
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Authors: |
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Brož, M.; Vokrouhlický, D.; Roig, F.; Nesvorný, D.; Bottke, W. F.; Morbidelli, A. |
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Affiliation: |
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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) |
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Journal: |
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Monthly Notices of the Royal Astronomical Society, Volume 359, Issue 4, pp. 1437-1455. (MNRAS Homepage) |
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Publication Date: |
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06/2005 |
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Origin: |
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MNRAS |
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Abstract Copyright: |
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(c) 2005 RAS |
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DOI: |
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Bibliographic Code: |
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2005MNRAS.359.1437B |
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
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Title: |
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Spectral study of the Eunomia asteroid family |
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Authors: |
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Nathues, Andreas; Mottola, Stefano; Kaasalainen, Mikko; Neukum, Gerhard |
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Affiliation: |
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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) |
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Journal: |
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Icarus, Volume 175, Issue 2, p. 452-463. (Icarus Homepage) |
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Publication Date: |
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06/2005 |
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Origin: |
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ELSEVIER |
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Abstract Copyright: |
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(c) 2005 Elsevier Science B.V. All rights reserved. |
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DOI: |
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Bibliographic Code: |
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2005Icar..175..452N |
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.
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Title: |
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The spin state of 433 Eros and its possible implications |
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Authors: |
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Affiliation: |
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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) |
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Journal: |
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Icarus, Volume 175, Issue 2, p. 419-434. (Icarus Homepage) |
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Publication Date: |
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06/2005 |
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Origin: |
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ELSEVIER |
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DOI: |
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Bibliographic Code: |
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2005Icar..175..419V |
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 ≃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 ≃61.4
kyr. Eros' resonant state forces its obliquity to oscillate with a period of
≃53.4 kyr between ≃76° and
≃89.5°. The observed value of ≃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.
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Title: |
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An equal-area map projection for irregular objects |
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Authors: |
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Affiliation: |
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Center for Radiophysics and Space Research, 306 Space
Sciences, |
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Journal: |
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Icarus, Volume 175, Issue 2, p. 382-389. (Icarus Homepage) |
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Publication Date: |
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06/2005 |
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Origin: |
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ELSEVIER |
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Abstract Copyright: |
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(c) 2005 Elsevier Science B.V. All rights reserved. |
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DOI: |
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Bibliographic Code: |
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2005Icar..175..382B |
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.
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Title: |
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The Statistical Asteroid Model. I. The Main-Belt Population for Diameters Greater than 1 Kilometer |
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Authors: |
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Affiliation: |
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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; , ) |
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Journal: |
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The Astronomical Journal, Volume 129, Issue 6, pp. 2869-2886. (AJ Homepage) |
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Publication Date: |
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06/2005 |
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Origin: |
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UCP |
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AJ Keywords: |
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Infrared: Solar System, Minor Planets, Asteroids, Solar System: General |
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Abstract Copyright: |
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(c) 2005: The American Astronomical Society |
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DOI: |
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Bibliographic Code: |
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2005AJ....129.2869T |
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.
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Title: |
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Analysis of near-IR spectra of 1 Ceres and 4 Vesta, targets of the Dawn mission |
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Authors: |
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Vernazza, P.; Mothé-Diniz, T.; Barucci, M. A.; Birlan, M.; Carvano, J. M.; Strazzulla, G.; Fulchignoni, M.; Migliorini, A. |
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Affiliation: |
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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) |
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Journal: |
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Astronomy and Astrophysics, Volume 436, Issue 3, June IV 2005, pp.1113-1121 (A&A Homepage) |
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Publication Date: |
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06/2005 |
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Origin: |
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EDP |
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Keywords: |
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minor planets, asteroids, techniques: spectroscopic, infrared: solar system |
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DOI: |
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Bibliographic Code: |
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2005A&A...436.1113V |
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
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Title: |
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Nutational damping times in solids of revolution |
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Authors: |
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Affiliation: |
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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) |
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Journal: |
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Monthly Notices of the Royal Astronomical Society, Volume 359, Issue 1, pp. 79-92. (MNRAS Homepage) |
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Publication Date: |
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05/2005 |
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Origin: |
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MNRAS |
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Abstract Copyright: |
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(c) 2005 RAS |
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DOI: |
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Bibliographic Code: |
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2005MNRAS.359...79S |
We derive the characteristic
nutational damping time Td 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.
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Title: |
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Ceres: Evolution and current state |
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Authors: |
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Journal: |
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Journal of Geophysical Research, Volume 110, Issue E5, CiteID E05009 (JGRE Homepage) |
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Publication Date: |
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05/2005 |
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Origin: |
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AGU |
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AGU Keywords: |
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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 |
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Abstract Copyright: |
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(c) 2005: American Geophysical |
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DOI: |
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Bibliographic Code: |
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2005JGRE..11005009M |
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.
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Title: |
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New V-type asteroids in near-Earth space |
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Authors: |
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Affiliation: |
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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) |
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Journal: |
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Icarus, Volume 175, Issue 1, p. 170-174. (Icarus Homepage) |
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Publication Date: |
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05/2005 |
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Origin: |
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ELSEVIER |
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Abstract Copyright: |
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(c) 2005 Elsevier Science B.V. All rights reserved. |
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DOI: |
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Bibliographic Code: |
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2005Icar..175..170M |
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.
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Title: |
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Dust transport in photoelectron layers and the formation of dust ponds on Eros |
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Authors: |
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Colwell, Joshua E.; Gulbis, Amanda A. S.; Horányi, Mihály; Robertson, Scott |
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Affiliation: |
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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) |
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Journal: |
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Icarus, Volume 175, Issue 1, p. 159-169. (Icarus Homepage) |
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Publication Date: |
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05/2005 |
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Origin: |
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ELSEVIER |
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Abstract Copyright: |
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(c) 2005 Elsevier Science B.V. All rights reserved. |
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DOI: |