Publications (7)20.55 Total impact

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ABSTRACT: Asteroid modeling efforts in the last decade resulted in a comprehensive dataset of almost 400 convex shape models and their rotation states. This amount already provided a deep insight into physical properties of mainbelt asteroids or large collisional families. We aim to increase the number of asteroid shape models and rotation states. Such results are an important input for various further studies such as analysis of asteroid physical properties in different populations, including smaller collisional families, thermophysical modeling, and scaling shape models by diskresolved images, or stellar occultation data. This provides, in combination with known masses, bulk density estimates, but constrains also theoretical collisional and evolutional models of the Solar System. We use all available diskintegrated optical data (i.e., classical denseintime photometry obtained from public databases and through a large collaboration network as well as sparseintime individual measurements from a few sky surveys) as an input for the convex inversion method, and derive 3D shape models of asteroids, together with their rotation periods and orientations of rotation axes. The key ingredient is the support of more that one hundred observers who submit their optical data to publicly available databases. We present updated shape models for 36 asteroids, for which mass estimates are currently available in the literature or their masses will be most likely determined from their gravitational influence on smaller bodies, which orbital deflection will be observed by the ESA Gaia astrometric mission. This was achieved by using additional optical data from recent apparitions for the shape optimization. Moreover, we also present new shape model determinations for 250 asteroids, including 13 Hungarias and 3 nearEarth asteroids.  [Show abstract] [Hide abstract]
ABSTRACT: In understanding the composition and internal structure of asteroids, their density is perhaps the most diagnostic quantity. We aim here to characterize the surface composition, mutual orbit, size, mass, and density of the small mainbelt binary asteroid (939) Isberga. For that, we conduct a suite of multitechnique observations, including optical lightcurves over many epochs, nearinfrared spectroscopy, and interferometry in the thermal infrared. We develop a simple geometric model of binary systems to analyze the interferometric data in combination with the results of the lightcurve modeling. From spectroscopy, we classify Ibserga as a Sqtype asteroid, consistent with the albedo of 0.14$^{+0.09}_{0.06}$ (all uncertainties are reported as 3$\sigma$ range) we determine (average albedo of Stypes is 0.197 $\pm$ 0.153, Pravec et al., 2012, Icarus 221, 365387). Lightcurve analysis reveals that the mutual orbit has a period of 26.6304 $\pm$ 0.0001 h, is close to circular, and has pole coordinates within 7 deg. of (225, +86) in ECJ2000, implying a low obliquity of 1.5 deg. The combined analysis of lightcurves and interferometric data allows us to determine the dimension of the system and we find volumeequivalent diameters of 12.4$^{+2.5}_{1.2}$ km and 3.6$^{+0.7}_{0.3}$ km for Isberga and its satellite, circling each other on a 33 km wide orbit. Their density is assumed equal and found to be $2.91^{+1.72}_{2.01}$ g.cm$^{3}$, lower than that of the associated ordinary chondrite meteorites, suggesting the presence of some macroporosity, but typical of Stypes of the same size range (Carry, 2012, P\&SS 73, 98118). The present study is the first direct measurement of the size of a small mainbelt binary. Although the interferometric observations of Isberga are at the edge of MIDI capabilities, the method described here is applicable to others suites of instruments (e.g, LBT, ALMA).  [Show abstract] [Hide abstract]
ABSTRACT: The larger number of models of asteroid shapes and their rotational states derived by the lightcurve inversion give us better insight into both the nature of individual objects and the whole asteroid population. With a larger statistical sample we can study the physical properties of asteroid populations, such as mainbelt asteroids or individual asteroid families, in more detail. Shape models can also be used in combination with other types of observational data (IR, adaptive optics images, stellar occultations), e.g., to determine sizes and thermal properties. We use all available photometric data of asteroids to derive their physical models by the lightcurve inversion method and compare the observed pole latitude distributions of all asteroids with known convex shape models with the simulated pole latitude distributions. We used classical dense photometric lightcurves from several sources and sparseintime photometry from the U.S. Naval Observatory in Flagstaff, Catalina Sky Survey, and La Palma surveys (IAU codes 689, 703, 950) in the lightcurve inversion method to determine asteroid convex models and their rotational states. We also extended a simple dynamical model for the spin evolution of asteroids used in our previous paper. We present 119 new asteroid models derived from combined dense and sparseintime photometry. We discuss the reliability of asteroid shape models derived only from Catalina Sky Survey data (IAU code 703) and present 20 such models. By using different values for a scaling parameter cYORP (corresponds to the magnitude of the YORP momentum) in the dynamical model for the spin evolution and by comparing synthetics and observed polelatitude distributions, we were able to constrain the typical values of the cYORP parameter as between 0.05 and 0.6.  [Show abstract] [Hide abstract]
ABSTRACT: Context. Aims.We present evidence that four minor planets of the main belt are binary systems. Methods.These discoveries are based on CCD photometric measurements made by many observers coordinated in a network of observatories. Results.Orbital and physical properties are derived from a total of 134 partial light curves involving 26 stations. (854) Frostia, (1089) Tama, (1313) Berna, and (4492) Debussy show mutual eclipses features on their light curves. In all cases, rotation and revolution are synchronous. Synodic periods are 37.728, 16.444, 25.464 and 26.606 h respectively. From a simple model, we have derived their bulk densities as follows: 0.89 $\pm$ 0.14, 2.52 $\pm$ 0.30, 1.22 $\pm$ 0.15 and 0.91 $\pm$ 0.10 g cm$^{3}$ respectively. Uncertainties in the bulk densities, arising from scattering and shadow effects are not taken into account. These could increase the density estimates by a factor up to 1.6. Our method of determining bulk density is completely independent of their mass and their diameter estimates. The low rotational periods and the low bulk densities clearly imply a collisional process to explain this kind of binary asteroid. Based on our database of a few thousand light curves of minor planets, the population of similarsized objects in the main belt is estimated to $6\pm 3$ percent in the 10–50 km diameter class. Conclusions.  [Show abstract] [Hide abstract]
ABSTRACT: The minor planet (1139) Atami showed mutual eclipses features on its light curves during its 2005 opposition. Photometric and radar analysis reveal the binarity of this system composed by two bodies of the same size (7.4x4.4x4.4 km 15%) separated by about 17.7 1.1 km. Rotations and revolutions are synchronous and the period is T =1.145 0.002 days. From a model, we derived bulk density =2.2 0.5 g/cm3. Spectrometry was performed during an eclipse. It reveals that the two bodies have the same reectance 
Article: Four new binary minor planets
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ABSTRACT: ABSTRACT Aims. We present evidence that four minor planets of the main belt are binary systems. Methods. These discoveries are based on CCD photometric measurements,made,by many,observers coordinated in a network of observatories. Results. Orbital and physical properties are derived from a total of 134 partial light curves involving 26 stations. (854) Frostia, (1089) Tama, (1313) Berna, and (4492) Debussy show mutual eclipses features on their light curves. In all cases, rotation and revolution are synchronous. Synodic periods are 37.728, 16.444, 25.464 and 26.606 h respectively. From a simple model, we have derived their bulk densities as follows: 0.89 ± 0.14, 2.52 ± 0.30, 1.22 ± 0.15 and 0.91 ± 0.10 g cm,3 respectively. Uncertainties in the bulk densities, arising from scattering and shadow effects are not taken into account. These could increase the density estimates by a factor up to 1.6. Our method,of determining bulk density is completely independent,of their mass and their diameter estimates. The low rotational periods and the low bulk densities clearly imply a collisional process to explain this kind of binary asteroid. Based on our database of a few thousand light curves of minor planets, the population of similarsized objects in the main belt is estimated to 6 ± 3 percent in the 10–50 km diameter class. Key words. planets and satellites: formation – minor planets, asteroids – techniques: photometric
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