1,173 results on '"Tosi, F"'
Search Results
152. Activated Factor VII. Antithrombin Complex plasma concentration in subjects with or without angiographically demonstrated coronary artery disease and myocardial infarction: PA1.11–1
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Tosi, F, Martinelli, N, Baroni, M, Girelli, D, Guarini, P, Udali, S, Branchini, A, Woodhams, B, Bernardi, F, and Olivieri, O
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- 2013
153. MAJIS/JUICE optical head: characterization campaign and derived performance test results
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Coyle, Laura E., Matsuura, Shuji, Perrin, Marshall D., Barbis, A., Barilli, M., Bini, A., Dami, M., Fossati, E., Pilato, G., Tommasi, L., Filacchione, G., De Angelis, S., Piccioni, G., Stefani, S., Tosi, F., Dumesnil, C., Haffoud, P., Langevin, Y., Amoroso, M., Mugnuolo, R., and Poulet, F.
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- 2022
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154. Dark material on Vesta from the infall of carbonaceous volatile-rich material
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McCord, T. B., Li, J.-Y., Combe, J.-P., McSween, H. Y., Jaumann, R., Reddy, V., Tosi, F., Williams, D. A., Blewett, D. T., Turrini, D., Palomba, E., Pieters, C. M., De Sanctis, M. C., Ammannito, E., Capria, M. T., Le Corre, L., Longobardo, A., Nathues, A., Mittlefehldt, D. W., Schröder, S. E., Hiesinger, H., Beck, A. W., Capaccioni, F., Carsenty, U., Keller, H. U., Denevi, B. W., Sunshine, J. M., Raymond, C. A., and Russell, C. T.
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- 2012
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155. Numerical stability of Entropic versus positivity-enforcing Lattice Boltzmann schemes
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Tosi, F., Ubertini, S., Succi, S., Chen, H., and Karlin, I.V.
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- 2006
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156. VIRTIS: An Imaging Spectrometer for the ROSETTA Mission
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Coradini, A., primary, Capaccioni, F., additional, Drossart, P., additional, Erard, S., additional, Filacchione, G., additional, Sanctis, M.C. De, additional, Capria, M.T., additional, Crovisier, J., additional, Ammannito, E., additional, Orosei, R., additional, Tosi, F., additional, Arnold, G., additional, Barucci, A., additional, Bellucci, G., additional, Benkhoff, J., additional, Bibring, J.P., additional, Blecka, M., additional, Bockelée-Morvan, D., additional, Carsenty, U., additional, Cerroni, P., additional, Combes, M., additional, Combi, M., additional, Encrenaz, T., additional, Federico, C., additional, Fonti, S., additional, Formisano, V., additional, Jaumann, R., additional, Kuehrt, E., additional, Langevin, Y., additional, Magni, G., additional, McCord, T., additional, Mottola, S., additional, Neukum, G., additional, Piccioni, G., additional, Rauer, H., additional, Schmitt, B., additional, Tozzi, G., additional, and Tiphene, D., additional
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- 2009
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157. Thermal Analysis of Unusual Local-scale Features on the Surface of Vesta
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Tosi, F, Capria, M. T, DeSanctis, M. C, Capaccioni, F, Palomba, E, Zambon, F, Ammannito, E, Blewett, D. T, Combe, J.-Ph, Denevi, B. W, Li, J.-Y, Mittlefehldt, D. W, Palmer, E, Sunshine, J. M, Titus, T. N, Raymond, C. A, and Russell, C. T
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Astrophysics - Abstract
At 525 km in mean diameter, Vesta is the second-most massive object in the main asteroid belt of our Solar System. At all scales, pyroxene absorptions are the most prominent spectral features on Vesta and overall, Vesta mineralogy indicates a complex magmatic evolution that led to a differentiated crust and mantle [1]. The thermal behavior of areas of unusual albedo seen on the surface at the local scale can be related to physical properties that can provide information about the origin of those materials. Dawn's Visible and Infrared Mapping Spectrometer (VIR) [2] hyperspectral images are routinely used, by means of temperature-retrieval algorithms, to compute surface temperatures along with spectral emissivities. Here we present temperature maps of several local-scale features of Vesta that were observed by Dawn under different illumination conditions and different local solar times.
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- 2013
158. Mesosiderites on Vesta: A Hyperspectral VIS-NIR Investigation
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Palomba, E, Longobardo, A, DeSanctis, M. C, Mittlefehldt, D. W, Ammannito, E, Capaccioni, F, Capria, M. T, Frigeri, A, Tosi, F, Zambon, F, Russell, C. T, and Raymond, C. A
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Geophysics - Abstract
The discussion about the mesosiderite origin is an open issue since several years. Mesosiderites are mixtures of silicate mineral fragments or clasts, embedded in a FeNi metal matrix. Silicates are very similar in mineralogy and texture to howardites [1]. This led some scientists to conclude that mesosiderites could come from the same parent parent asteroid of the howardite, eucrite and diogenite (HED) meteorites [2, 3]. Other studies found a number of differences between HEDs and mesosiderite silicates that could be explained only by separate parent asteroids [4]. Recently, high precision oxygen isotope measurements of m esosiderites silicate fraction were found to be isotopically identical to the HEDs, requiring common parent body, i.e. 4 Vesta [5]. Another important element in favor of a common origin was given by the identification of a centimeter-sized mesosiderite clast in a howardite (Dar al Gani 779): a metal-rich inclusion with fragments of olivine, anorthite, and orthopyroxene plus minor amounts of chromite, tridymite, and troilite [6]. The Dawn mission with its instruments, the Infrared Mapping Spectrometer (VIR) [7], the Framing Camera [8] and the Gamma-Ray and Neutron Detector (GRaND) [9] confirmed that Vesta has a composition fully compatible with HED meteorites [10]. We investigate here the possibility to discern mesosiderite rich locations on the surface of Vesta by means of hyperspectral IR images.
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- 2013
159. Mineralogical Composition of the Different Types of Bright Deposits on Vesta
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Zambon, F, Capaccioni, F, DeSanctis, M. C, Ammannito, E, Li, J.-Y, Longobardo, A, Mittlefehldt, D. W, Palomba, E, Pieters, C. M, Schroeder, S. E, Tosi, F, Hiesinger, H, Blewett, D. T, Russell, C. T, Raymond, C. A, Capria, M. T, Carraro, F, Fonte, S, Frigeri, A, and Magni, G
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Geophysics - Abstract
VIR-MS, Dawn's Visible and Infrared Mapping Spectrometer, obtained hyperspectral images of a wide part of Vesta's surface at a variety of spatial resolutions [1]. Vesta spectra are similar to those of the howardite-eucrite-diogenite (HED) meteorites. Moreover, they are characterized by the two iron-bearing pyroxene bands at 0.9 (band I) and 1.9 microns (band II). Vesta surface's is dominated by eucrite/howardite with some diogenitic regions situated in the southern hemisphere near the Rheasilvia basin [2]. The surface is heavily craterized and impacts can expose fresh material, thus generating the Bright Material Deposits (BMD) observed within and surrounding certain craters. BMD can be classified into six different types based on their morphological characteristics: Crater Wall/Scarp Material (CWM), Radial Material (RM), Slope Material (SM), Patchy Material (PM), Spot Material (SpM) and Diffuse Plains Material (DPM) [3]. The most widespread BMD are CWM, SM and RM. CWM, SM, RM originate from impacts. CWM is situated on the edge of the craters. Mass wasting from the crater walls and generates the SM, while RM is associated with the ejecta of the craters [4]. BMD are characterized by albedo greater than that of the vestan average, 0.38 [5]. Therefore the different types of deposits present distinct levels of reflectance respect to the Surrounding Regions (SR), in particular: the CWM and SM is approx.40% brighter, the RM is approx.30- 40% brighter; the SpM is about 20-25% brighter and the PM is about 20% brighter. Near the edge of the Rheasilvia basin it is possible to find some extremely bright areas ~80% brighter than the vestan average [6].
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- 2013
160. Pitted Terrain on Vesta and Implications for the Presence of Volatiles
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Denevi, B. W., Blewett, D. T., Buczkowski, D. L., Capaccioni, F., Capria, M. T., De Sanctis, M. C., Garry, W. B., Gaskell, R. W., Corre, L. Le, Li, J.-Y., Marchi, S., McCoy, T. J., Nathues, A., OʼBrien, D. P., Petro, N. E., Pieters, C. M., Preusker, F., Raymond, C. A., Reddy, V., Russell, C. T., Schenk, P., Scully, J. E. C., Sunshine, J. M., Tosi, F., Williams, D. A., and Wyrick, D.
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- 2012
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161. Spectroscopic Characterization of Mineralogy and Its Diversity Across Vesta
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De Sanctis, M. C., Ammannito, E., Capria, M. T., Tosi, F., Capaccioni, F., Zambon, F., Carraro, F., Fonte, S., Frigeri, A., Jaumann, R., Magni, G., Marchi, S., McCord, T. B., McFadden, L. A., McSween, H. Y., Mittlefehldt, D. W., Nathues, A., Palomba, E., Pieters, C. M., Raymond, C. A., Russell, C. T., Toplis, M. J., and Turrini, D.
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- 2012
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162. The Surface Composition and Temperature of Asteroid 21 Lutetia As Observed by Rosetta/VIRTIS
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Coradini, A., Capaccioni, F., Erard, S., Arnold, G., De Sanctis, M. C., Filacchione, G., Tosi, F., Barucci, M. A., Capria, M. T., Ammannito, E., Grassi, D., Piccioni, G., Giuppi, S., Bellucci, G., Benkhoff, J., Bibring, J. P., Blanco, A., Blecka, M., Bockelee-Morvan, D., Carraro, F., Carlson, R., Carsenty, U., Cerroni, P., Colangeli, L., Combes, M., Combi, M., Crovisier, J., Drossart, P., Encrenaz, E. T., Federico, C., Fink, U., Fonti, S., Giacomini, L., Ip, W. H., Jaumann, R., Kuehrt, E., Langevin, Y., Magni, G., McCord, T., Mennella, V., Mottola, S., Neukum, G., Orofino, V., Palumbo, P., Schade, U., Schmitt, B., Taylor, F., Tiphene, D., and Tozzi, G.
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- 2011
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163. The surface of (1) Ceres in visible light as seen by Dawn/VIR
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Rousseau, B., primary, De Sanctis, M. C., additional, Raponi, A., additional, Ciarniello, M., additional, Ammannito, E., additional, Frigeri, A., additional, Ferrari, M., additional, De Angelis, S., additional, Carrozzo, F. C., additional, Tosi, F., additional, Schröder, S. E., additional, Raymond, C. A., additional, and Russell, C. T., additional
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- 2020
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164. Multidimensional evaluation of telepresence robot: results from a field trial
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Fiorini, L., primary, Mancioppi, G., additional, Becchimanzi, C., additional, Sorrentino, A., additional, Pistolesi, M., additional, Tosi, F., additional, and Cavallo, F., additional
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- 2020
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165. Insulin resistance and PCOS: chicken or egg?
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Moghetti, P., primary and Tosi, F., additional
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- 2020
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166. Turbulence Power Spectra in Regions Surrounding Jupiter's South Polar Cyclones From Juno/JIRAM
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Moriconi, M. L., primary, Migliorini, A., additional, Altieri, F., additional, Adriani, A., additional, Mura, A., additional, Orton, G., additional, Lunine, J. I., additional, Grassi, D., additional, Atreya, S. K., additional, Ingersoll, A. P., additional, Dinelli, B. M., additional, Bolton, S. J., additional, Levin, S., additional, Tosi, F., additional, Noschese, R., additional, Plainaki, C., additional, Cicchetti, A., additional, Sindoni, G., additional, and Olivieri, A., additional
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- 2020
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167. Two‐Year Observations of the Jupiter Polar Regions by JIRAM on Board Juno
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Adriani, A., primary, Bracco, A., additional, Grassi, D., additional, Moriconi, M. L., additional, Mura, A., additional, Orton, G., additional, Altieri, F., additional, Ingersoll, A., additional, Atreya, S. K., additional, Lunine, J. I., additional, Migliorini, A., additional, Noschese, R., additional, Cicchetti, A., additional, Sordini, R., additional, Tosi, F., additional, Sindoni, G., additional, Plainaki, C., additional, Dinelli, B. M., additional, Turrini, D., additional, Filacchione, G., additional, Piccioni, G., additional, and Bolton, S. J., additional
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- 2020
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168. On the Spatial Distribution of Minor Species in Jupiter's Troposphere as Inferred From Juno JIRAM Data
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Grassi, D., primary, Adriani, A., additional, Mura, A., additional, Atreya, S. K., additional, Fletcher, L. N., additional, Lunine, J. I., additional, Orton, G. S., additional, Bolton, S., additional, Plainaki, C., additional, Sindoni, G., additional, Altieri, F., additional, Cicchetti, A., additional, Dinelli, B. M., additional, Filacchione, G., additional, Migliorini, A., additional, Moriconi, M. L., additional, Noschese, R., additional, Olivieri, A., additional, Piccioni, G., additional, Sordini, R., additional, Stefani, S., additional, Tosi, F., additional, and Turrini, D., additional
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- 2020
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169. High Thermal Inertia Zones on Ceres From Dawn Data
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Rognini, E., primary, Capria, M. T., additional, Tosi, F., additional, De Sanctis, M. C., additional, Ciarniello, M., additional, Longobardo, A., additional, Carrozzo, F. G., additional, Raponi, A., additional, Frigeri, A., additional, Palomba, E., additional, Fonte, S., additional, Giardino, M., additional, Ammannito, E., additional, Raymond, C. A., additional, and Russell, C. T., additional
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- 2020
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170. Ceres observed at low phase angles by VIR-Dawn
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Ciarniello, M., primary, De Sanctis, M. C., additional, Raponi, A., additional, Rousseau, B., additional, Longobardo, A., additional, Li, J.-Y., additional, Schröder, S. E., additional, Tosi, F., additional, Zambon, F., additional, Ammannito, E., additional, Carrozzo, F. G., additional, Frigeri, A., additional, Rognini, E., additional, Raymond, C. A., additional, and Russell, C. T., additional
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- 2020
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171. Infrared detection of aliphatic organics on a cometary nucleus
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Raponi, A., primary, Ciarniello, M., additional, Capaccioni, F., additional, Mennella, V., additional, Filacchione, G., additional, Vinogradoff, V., additional, Poch, O., additional, Beck, P., additional, Quirico, E., additional, De Sanctis, M. C., additional, Moroz, L. V., additional, Kappel, D., additional, Erard, S., additional, Bockelée-Morvan, D., additional, Longobardo, A., additional, Tosi, F., additional, Palomba, E., additional, Combe, J.-P., additional, Rousseau, B., additional, Arnold, G., additional, Carlson, R. W., additional, Pommerol, A., additional, Pilorget, C., additional, Fornasier, S., additional, Bellucci, G., additional, Barucci, A., additional, Mancarella, F., additional, Formisano, M., additional, Rinaldi, G., additional, Istiqomah, I., additional, and Leyrat, C., additional
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- 2020
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172. Vesta Mineralogy after Dawn Global Observations
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ChristinaDeSanctis, Maria, Ammannito, E, Capaccioni, F, Cparia, M. T, Carraro, F, Fonte, S, Frigeri, A, Longobardo, A, Marchi, S, Palomba, E, Tosi, F, Zambon, F, Combe, J. P, McCord, T. B, McFadden, L. A, McSween, H, Mittlefehldt, D. W, Pieters, C. M, Jaumann, R, Stephan, K, Raymond, C. A, and Russell, C. T
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Astrophysics - Abstract
The Dawn mission has completed its mapping phases at Vesta and millions of spectra have been acquired by the Visible and InfraRed Mapping Spectrometer, VIR(1). VIR characterizes and maps the mineral distribution on Vesta -strengthening the Vesta HED linkage- and provides new insights into Vesta s formation and evolution(2,3). VIR spectra are dominated by pyroxene absorptions near 0.9 and 2.0 m and large thermal emission beyond 3.5 m. Although almost all surface materials exhibit howardite-like spectra, some large regions can be interpreted to be richer in eucritic (basaltic) material and others richer in diogenititic (Mg-orthopyroxenitic) material. The Rheasilvia basin contains Mg-pyroxene-rich terrains for example. Vesta' s surface shows considerable diversity at local scales. Many bright and dark areas(3,4) are associated with various geological features and show remarkably different morphology. Moreover, VIR detected statistically significant, but weak, variations at 2.8 m that have been interpreted as indicating the presence of OH-bearing phases on the surface(5). The OH distribution is uneven with large regions lacking this absorption feature. Associations of 2.8 m band with morphological structures indicate complex process responsible for OH. Vesta exhibits large spectral variations that often correlate with geological structures, indicating a complex geological and evolutionary history, more similar to that of the terrestrial planets than to other asteroids visited by spacecrafts.
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- 2012
173. Analysis of Temperature Maps of Selected Dawn Data Over the Surface of Vesta
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Tosi, F, Capria, M. T, DeSanctis, M. C, Palomba, E, Grassi, D, Capaccioni, F, Ammannito, E, Combe, J.-Ph, Sunshine, J. M, McCord, T. B, Li, Y.-Y, Titus, T. N, Russell, C. T, Raymond, C. A, Mittlefehldt, D. W, Toplis, M. J, Forni, O, and Sykes, M. V
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Geophysics - Abstract
The thermal behavior of areas of unusual albedo at the surface of Vesta can be related to physical properties that may provide some information about the origin of those materials. Dawn s Visible and Infrared Mapping Spectrometer (VIR) [1] hyperspectral cubes can be used to retrieve surface temperatures. Due to instrumental constraints, high accuracy is obtained only if temperatures are greater than 180 K. Bright and dark surface materials on Vesta are currently investigated by the Dawn team [e.g., 2 and 3 respectively]. Here we present temperature maps of several local-scale features that were observed by Dawn under different illumination conditions and different local solar times.
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- 2012
174. Comparison of Observed Surface Temperatures of 4 Vesta to the KRC Thermal Model
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Titus, T. N, Becker, K. J, Anderson, J. A, Capria, M. T, Tosi, F, DeSanctis, M. C, Palomba, E, Grassi, D, Capaccioni, F, Ammannito, E, Combe, J.-P, McCord, T. B, Li, J.-Y, Russell, C. T, Ryamond, C. A, Mittlefehldt, D, Toplis, M, Forni, O, and Sykes, M. V
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Astronomy - Abstract
In this work, we will compare ob-served temperatures of the surface of Vesta using data acquired by the Dawn [1] Visible and Infrared Map-ping Spectrometer (VIR-MS) [2] during the approach phase to model results from the KRC thermal model. High thermal inertia materials, such as bedrock, resist changes in temperature while temperatures of low thermal inertia material, such as dust, respond quickly to changes in solar insolation. The surface of Vesta is expected to have low to medium thermal inertia values, with the most commonly used value being extremely low at 15 TIU [4]. There are several parameters which affect observed temperatures in addition to thermal inertia: bond albedo, slope, and surface roughness. In addition to these parameters, real surfaces are rarely uniform monoliths that can be described by a single thermal inertia value. Real surfaces are often vertically layered or are mixtures of dust and rock. For Vesta's surface, with temperature extremes ranging from 50 K to 275 K and no atmosphere, even a uniform monolithic surface may have non-uniform thermal inertia due to temperature dependent thermal conductivity.
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- 2012
175. Spectral Characterization of Bright Materials on Vesta
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Capaccioni, Fabrizio, DeSanctis, M. C, Ammannito, E, Li, Jian-Yang, Longobardo, A, Mittlefehldt, David W, Palomba, E, Pieters, C. M, Schroeder, S. E, Tosi, F, Hiesinger, H, Blewett, D. T, Russell, C. T, and Raymond, C. A
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Lunar And Planetary Science And Exploration - Abstract
The surface of Vesta, as observed by the camera and imaging spectrometer onboard the Dawn spacecraft, displays large surface diversity in terms of its geology and mineralogy with noticeably dark and bright areas on the surface often associated with various geological features and showing remarkably different forms. Here we report our initial attempt to spectrally characterize the areas that are distinctively brighter than their surroundings.
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- 2012
176. Vesta and the HED Meteorites: Comparison of Spectral Properties
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Ammannito, E, De Sanctis, M. C, Fonte, S, Magni, G, Capaccioni, F, Tosi, F, Capria, M. T, Blewett, D, Combe, J. P, Farina, M, McCoord, T. B, Mittlefehldt, D. W, Palomba, E, McSween, H, Pieters, C, Sunshine, J, Titus, T. N, Toplis, M, Russell, C. T, and Raymond, C. A
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Astrophysics - Abstract
We present the main results obtained comparing the visible-near infrared (VIS-NIR) spectra Vesta s surface with howardites, eucrites, diogenites (HEDs). HEDs are commonly associated with Vesta based on spectral similarities. Because of such association, much effort is being made to merge the information from HEDs as well as Vestoids with that from Vesta to characterize the lithologic diversity of the surface of this asteroid and to infer clues regarding its thermal history. The Dawn spacecraft, orbiting around Vesta since July 2011, is performing detailed observations of this body and thus improving our knowledge of its properties. Dawn s scientific payload includes an imaging spectrometer, VIR-MS, sensitive to the VIS-NIR spectral range. VIR-MS began acquiring spectra during the approach phase that started in May 2011 and will continue its observations through July 2012 when the spacecraft will depart Vesta to travel to Ceres. The observations are uniformly distributed in latitude and longitude, allowing a global view of Vesta s crustal spectral properties. Using the information provided by VIR spectra, we studied the distribution of the spectral heterogeneities on the surface and used our findings to perform a comparison with HED spectra in the VIS-NIR spectral range searching for analogies and/or incompatibilities. In our analysis, we utilized a method to compare the results obtained at microscopic scale on HED samples and the one obtained at macroscopic scale on the surface of Vesta. The intent of this study is to improve our understanding of the connection between Vesta and the HEDs, which is one of the primary Dawn scientific objectives. Dawn VIR spectra are characterized by pyroxene absorptions and most of the surface materials exhibit howardite-like spectra. However, some large areas can be interpreted to be material richer in diogenite (based on pyroxenes band depths and band centers) and some others like eucrite-rich howardite terrains. In particular, VIR data strongly indicate in the south polar region (Rheasilvia) the presence of Mg-pyroxene-rich terrains. The hypothesis that Vesta is the HED parent body is consistent with, and strengthened by, the geologic and spectral context for pyroxene distribution provided by VIR on Dawn.
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- 2012
177. Spectroscopic Characterization of Mineralogy Across Vesta: Evidence of Different Lithologies
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De Sanotis, M. C, Ammannito, E, Filacchione, G, Capria, M. T, Tosi, F, Capaccioni, F, Zambon, F, Carraro, F, Fonte, S, Frigeri, A, Jaumann, R, Magni, G, Marchi, S, McCord, T. B, McFadden, L. A, McSween, H. Y, Mittlefehldt, D. W, Nathues, A, Palomba, E, Pieters, C. M, Raymond, C. A, Russell, C. T, and Turrini, D
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Geophysics - Abstract
The average spectrum of Vesta, obtained by VIR in the range 0.25-5.1 microns, shows clear evidence of absorption bands due to pyroxenes and thermal emissions beyond 3.5 11m. Vesta shows considerable variability across its surface in terms of spectral reflectance and emission, band depths, bands widths and bands centers, reflecting a complex geological history. Vesta's average spectrum and inferred mineralogy resemble those of howardite meteorites. On a regional scale, significant deviations are seen: the south polar 500km Rheasilvia impact crater has a higher diogenitic component, and equatorial regions show a higher eucritic component. This lithologic distribution, with a concentration of Mg-pyroxenes in the Rheasilvia area, reinforces the hypothesis of a deeper diogenitic crust excavated by the impact that formed the Rheasilvia crater, and an upper eucritic crust, whose remnants are seen in the equatorial region. This scenario has implications for Vesta differentiation, consistent with magma ocean models. However, serial magmatism models could also have concentrated pyroxene cumulates in plutons emplaced within the lower crust
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- 2012
178. Thermal Behaviour of Unusual Local-Scale Surface Features on Vesta
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Tosi, F, Capria, M. T, De Sanctis, M. C, Palomba, E, Grassi, D, Capaccioni, F, Ammannito, E, Combe, J.-Ph, Sunshine, J. M, McCord, T. B, Titus, T. N, Russell, C. T, Raymond, C. A, Mittlefehldt, D. W, Toplis, M. J, Forni, O, and Sykes, M. V
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Astrophysics - Abstract
On Vesta, the region of the infrared spectrum beyond approximately 3.5 micrometers is dominated by the thermal emission of the asteroid's surface, which can be used to determine surface temperature by means of temperature-retrieval algorithms. The thermal behavior of areas of unusual albedo seen at the local scale can be related to physical properties that can provide information about the origin of those materials. Dawn's Visible and Infrared Mapping Spectrometer (VIR) hyperspectral cubes are used to retrieve surface temperatures, with high accuracy as long as temperatures are greater than 180 K. Data acquired in the Survey phase (23 July through 29 August 2011) show several unusual surface features: 1) high-albedo (bright) and low-albedo (dark) material deposits, 2) spectrally distinct ejecta, 3) regions suggesting finer-grained materials. Some of the unusual dark and bright features were re-observed by VIR in the subsequent High-Altitude Mapping Orbit (HAMO) and Low-Altitude Mapping Orbit (LAMO) phases at increased pixel resolution. To calculate surface temperatures, we applied a Bayesian approach to nonlinear inversion based on the Kirchhoff law and the Planck function. These results were cross-checked through application of alternative methods. Here we present temperature maps of several local-scale features that were observed by Dawn under different illumination conditions and different local solar times. Some bright terrains have an overall albedo in the visible as much as 40% brighter than surrounding areas. Data from the IR channel of VIR show that bright regions generally correspond to regions with lower thermal emission, i.e. lower temperature, while dark regions correspond to areas with higher thermal emission, i.e. higher temperature. This behavior confirms that many of the dark appearances in the VIS mainly reflect albedo variations. In particular, it is shown that during maximum daily insolation, dark features in the equatorial region may rise to temperatures greater than 270 K. However, individual features may show different thermal behaviours, as a result of differences in composition and/or structure (e.g, average grain size of the surface regolith, porosity, etc.). To complement the temperature and near-infrared emissivity derived from the infrared spectra, a separate work is devoted to calculate thermal inertia and other thermal properties using theoretical models which solve the heat equation for airless bodies, and model the distribution of temperatures due to surface roughness variations.
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- 2012
179. Characterization of Mineralogy Across Vesta
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De Sanctis, M. C, Ammannito, E, Capria, M. T, Capaccioni, F, Carraro, F, Fonte, S, Frigeri, A, Magni, G, Marchi, S, Palomba, E, Tosi, F, Zambon, F, McCord, T. B, McFadden, L. A, McSween, H, Mittlefehldt, D. W, Pieters, C. M, Raymond, C. A, and Russell, C. T
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Geophysics - Abstract
Dawn VIR spectra are characterized by pyroxene absorptions and no clear evidence for abundant other minerals are observed at the scale of the present measurements. Even though Vesta spectra are dominated by pyroxenes, spectral variation at regional and local scales are evident and distinct color units are identified. Although almost all of the surface materials exhibit spectra like those of howardites, some large units can be interpreted to be material richer in diogenite (based on pyroxenes band depths and band centers) and some others like eucrite-rich howardite units. VIR data strongly indicate that the south polar region (Rheasilvia) has its own spectral characteristics, indicating the presence of Mg-pyroxene-rich terrains (diogenite-like), while the equatorial areas have swallower band depths and average band centers at slightly longer wavelengths, consistent with more eucrite rich materials. Vesta surface shows considerable diversity at smaller scales (tens of km), in terms of spectral reflectance and emission, band depths and slopes. Many bright and dark spots are present on Vesta. Dark spots have low reflectance at visible wavelengths and are spectrally characterized by shallower 1 and 2 micron bands with respect the surrounding terrains. Bright materials have high reflectance and are often spectrally characterized by deep pyroxenes absorption bands. Vesta presents complex geology/topography and the mineral distribution is often correlated with geological and topographical structures. Ejecta from large craters have distinct spectral behaviors, and materials exposed in the craters show distinct spectra on floors and rims. VIR reveals the mineralogical variation of Vesta s crustal stratigraphy on local and global scales. Maps of spectral parameters show surface and subsurface unit compositions in their stratigraphic context. The hypothesis that Vesta is the HED parent body is consistent with, and strengthened by, the geologic and spectral context for pyroxene distribution provided by Dawn.
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- 2012
180. Search for Olivine Spectral Signatures on the Surface of Vesta
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Palomba, E, De Sanctis, M. C, Ammannito, E, Capaccioni, F, Capria, M. T, Farina, M, Frigeri, A, Longobardo, A, Tosi, F, Zambon, F, McSween, H. Y, Mittlefehldt, D. W, Russell, C. T, Raymond, C. A, Sunshine, J, and McCord, T. B
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Geophysics - Abstract
The occurrence of olivines on Vesta were first postulated from traditional petrogenetic models which suggest the formation of olivine as lower crustal cumulates. An indirect confirmation is given by their presence as a minor component in some samples of diogenite meteorites, the harzburgitic diogenites and the dunitic diogenites, and as olivine mineral clasts in howardites. Another indication for this mineral was given by interpretations of groundbased and Hubble Space Telescope observations that suggested the presence of local olivine-bearing units on the surface of Vesta. The VIR instrument onboard the DAWN mission has been mapping Vesta since July 2011. VIR acquired hyperspectral images of Vesta s surface in the wavelength range from 0.25 to 5.1 m during Approach, Survey and High Altitude Mapping (HAMO) orbits that allowed a 2/3 of the entire asteroid surface to be mapped. The VIR operative spectral interval, resolution and coverage is suitable for the detection and mapping of any olivine rich regions that may occur on the Vesta surface. The abundance of olivine in diogenites is typically lower than 10% but some samples richer in olivine are known. However, we do not expect to have extensive exposures of olivine-rich material on Vesta. Moreover, the partial overlap of olivine and pyroxene spectral signatures will make olivine difficult to detect. Different spectral parameters have been used to map olivine on extraterrestrial bodies, and here we discuss the different approaches used, and develop new ones specifically for Vesta. Our new methods are based on combinations of the spectral parameters relative to the 1 and 2 micron bands (the most prominent spectral features of Vesta surface in the visible and the infrared), such as band center locations, band depths, band areas, band area ratios. Before the direct application to the VIR data, the efficiency of each approach is evaluated by means of analysis of laboratory spectra of HED meteorites, pyroxenes, olivines and their mixtures.
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- 2012
181. Overview of Vesta Mineralogy Diversity
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DeSanctis, M. C, Ammannito, E, Capria, M. T, Capaccioni, F, Carraro, F, Fonte, S, Frigeri, A, Magni, G, Marchi, S, Palomba, E, Tosi, F, Zambon, F, McCord, T. B, McFadden, L. A, McSween, H, Mittlefehldt, D. W, Pieters, C. M, Raymond, C. A, and Russell, C. T
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Geophysics - Abstract
4 Vesta is known to have a surface of basaltic material through visible/near-infrared reflectance spectroscopy (1). Vesta s spectrum has strong absorption features centered near 0.9 and 1.9 m, indicative of Fe-bearing pyroxenes. The spectra of HED (howardite, eucrite and diogenite) meteorites have similar features (1). This led to the hypothesis that Vesta was the parent body of the HED clan (2,3) and the discovery of a dynamical Vesta family of asteroids (Vestoids) provides a further link between Vesta and HEDs (4). Data from the Dawn VIR (Visible InfraRed mapping Spectrometer) (5) characterize and map the mineral distribution on Vesta, strengthen the Vesta - HED linkage and provide new insights into Vesta s formation and evolution.
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- 2012
182. Correction of the VIR-visible data set from the Dawn mission
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Rousseau, B., primary, Raponi, A., additional, Ciarniello, M., additional, Ammannito, E., additional, Carrozzo, F. G., additional, De Sanctis, M. C., additional, Fonte, S., additional, Frigeri, A., additional, and Tosi, F., additional
- Published
- 2019
- Full Text
- View/download PDF
183. Macro vs. Micro: Relating the Spectral Properties of Vesta and the HED Meteorite
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Ammannito, E, Coradini, A, DeSanctis, M. C, Filacchione, G, Fonte, S, Magni, G, Capaccioni, F, Capria, M. T, Tosi, F, Blewett, D. T, Combe, J. P, Farina, M, Mittlefehldt, D. W, Palomba, E, Pieters, C. M, Sunshine, J, Titus, T. N, Toplis, M. J, Russell, C. T, Raymond, C. A, and McSween, H. Y., Jr
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Astronomy - Abstract
We present the main results obtained comparing the visible-near infrared (VIS-NIR) spectra Vesta s surface with howardites, eucrites, diogenites (HED). HEDs are commonly associated with Vesta s composition based on spectral similarities. Because of such association, much effort is being made to merge the information from HEDs as well as Vestoids - with that from Vesta to characterize the lithologic diversity of the surface of this asteroid and to infer clues regarding its thermal history. However, while the HEDs are a class of meteorites well studied in the laboratory, the only spectral data available for Vesta until now were telescopic observations which are limited in terms of observation conditions, spatial resolution and Signal to Noise Ratio. The Dawn spacecraft, orbiting around Vesta since July 2011, is performing detailed observations of this body and thus improving our knowledge of its properties. Dawn s scientific payload includes an imaging spectrometer, VIR-MS, sensitive to the VIS-NIR spectral range. VIR-MS began acquiring spectra during the approach phase started in May 2011 and will continue its observations through July 2012 when the spacecraft will depart Vesta to travel to Ceres. The VIR-MS spatial resolution depends upon the mission phase (approach, survey, high altitude, low altitude). However, spectra acquired by VIR-MS have already exceeded the spatial resolution of ground-based telescopic observations, with resolution in the approach phase ranging from 2.5 up to 0.8 km/pixel. Moreover, the observations are uniformly distributed in latitude and longitude allowing us to have a global view of Vesta s crust spectral properties. Using the information provided by VIR spectra, we studied the distribution of the spectral heterogeneities on the surface and we used our findings to perform a comparison with HEDs spectra in the VIS-NIR spectral range searching for analogies and/or incompatibilities. In our analysis, we focused on a method to compare the results obtained at microscopic scale on HEDs samples and the one obtained at macroscopic scale on the surface of Vesta. Finally, we discuss our results in the context of vestan thermal history. The intent of this study is to improve our understanding of the connection between Vesta and the HED samples, which is one of the primary Dawn scientific objectives. This work is supported by an Italian Space Agency (ASI) grant and by NASA through the Dawn project and a Dawn at Vesta Participating Scientist grant.
- Published
- 2011
184. Regolith Properties of Asteroid 21 Lutetia Constrained by Combined Data Sets of the MIRO and VIRTIS Instruments During the Rosetta Spacecraft Flyby
- Author
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Keihm, S, Tosi, F, Kamp, L, Capaccioni, F, Grassi, D, Gulkis, S, and Coradini, A
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Lunar And Planetary Science And Exploration - Abstract
During the July 10, 2010 flyby of Asteroid 21 Lutetia by the Rosetta spacecraft, maps of surface and subsurface temperatures were derived from the VIRTIS and MIRO instruments respectively. Both data sets indicated a porous surface layer with an extremely low, lunar-like thermal inertia. However, comparisons of the VIRTIS-measured and MIRO-modelled surface temperatures revealed offsets of 10- 30 K, indicative of self-heating or "beaming" effects that were not taken into account in the MIRO thermal modeling. Inclusion of a model of hemispherical craters at all scales 1 cm and larger, covering 50% of the surface, removes most of the offsets in the VIRTIS, MIRO surface temperature determinations.
- Published
- 2011
185. Dawn Maps the Surface Composition of Vesta
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Prettyman, T, Palmer, E, Reedy, R, Sykes, M, Yingst, R, McSween, H, DeSanctis, M. C, Capaccinoni, F, Capria, M. T, Filacchione, G, Magni, G, Ammannito, E, Carraro, F, Coradini, A, Fonte, S, Noschese, R, Tosi, F, Blewett, D, Denevi, B, Lawrence, D, Buratti, B, Raymond, C. A, Combe, J. P, McCord, T, and Forni, O
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Lunar And Planetary Science And Exploration - Abstract
By 7-October-2011, the Dawn mission will have completed Survey orbit and commenced high altitude mapping of 4-Vesta. We present a preliminary analysis of data acquired by Dawn's Framing Camera (FC) and the Visual and InfraRed Spectrometer (VIR) to map mineralogy and surface temperature, and to detect and quantify surficial OH. The radiometric calibration of VIR and FC is described. Background counting data acquired by GRaND are used to determine elemental detection limits from measurements at low altitude, which will commence in November. Geochemical models used in the interpretation of the data are described. Thermal properties, mineral-, and geochemical-data are combined to provide constraints on Vesta s formation and thermal evolution, the delivery of exogenic materials, space weathering processes, and the origin of the howardite, eucrite, and diogenite (HED) meteorites.
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- 2011
186. Vesta Mineralogy: VIR maps Vesta's surface
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Coradina, A, DeSanctis, M, Ammannito, E, Capaccioni, F, Capria, T, Carraro, F, Cartacci, M, Filacchione, G, Fonte, S, Magni, G, Noschese, R, Tosi, F, Barucci, A, Federico, C, Frigeri, A, Fulchigoni, M, Langevin, Y, Marchi, S, Palomba, E, Turrini, D, McCord, T, McFadden, L. A, Pieters, C, Raymond, C. A, and Russell, C. T
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Geophysics - Abstract
The Dawn mission will have completed Survey orbit around 4 Vesta by the end of August 2011. We present a preliminary analysis of data acquired by the Visual and InfraRed Spectrometer (VIR) to map Vesta mineralogy. Thermal properties and mineralogical data are combined to provide constraints on Vesta's formation and thermal evolution. delivery of exogenic materials, space weathering processes, and origin of the howardite. eucrite, and diogenite (HED) meteorites.
- Published
- 2011
187. Analysis of night-side dust activity on comet 67P observed by VIRTIS-M: a new method to constrain the thermal inertia on the surface
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Rinaldi, G., Formisano, M., Kappel, D., Capaccioni, F., Bockelée-Morvan, D., Cheng, Y.-C., Vincent, J.-B., Deshapriya, P., Arnold, G., Capria, M., Ciarniello, M., D’Aversa, E., D'aversa, E, De Sanctis, M., Doose, L., Erard, S., Federico, C., Filacchione, G., Fink, U., Leyrat, C., Longobardo, A., Magni, G., Migliorini, A., Mottola, S., Naletto, G., Raponi, A., Taylor, F., Tosi, F., Tozzi, G., Salatti, M., IASI (IASI), Consiglio Nazionale delle Ricerche (CNR), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy [Taiwan] (IANCU), National Central University [Taiwan] (NCU), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique et Mécanique Textiles (LPMT), ENSITM-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Matériaux et nanosciences d'Alsace (FMNGE), Institut de Chimie du CNRS (INC)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), IASF-Roma - Istituto di Astrofisica Spaziale e Fisica cosmica - Roma, Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Instituto de Estudos Avançados (IEAV), Institut, DLR Institute of Planetary Research, German Aerospace Center (DLR), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Universita degli Studi di Padova, INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto di Fisica dello Spazio Interplanetario (IFSI), Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-ENSITM-Matériaux et Nanosciences Grand-Est (MNGE), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Padova = University of Padua (Unipd), and Bockelée-Morvan, Dominique
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Asteroiden und Kometen ,67P/Churyumov-Gerasimenko -infrared ,010504 meteorology & atmospheric sciences ,Comet ,Imaging spectrometer ,Coma (optics) ,Astrophysics ,[SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph] ,01 natural sciences ,general -comets ,Mantle (geology) ,[SDU] Sciences of the Universe [physics] ,comet ,0103 physical sciences ,Thermal ,comets ,individual ,infrared: planetary systems ,010303 astronomy & astrophysics ,planetary systems ,ComputingMilieux_MISCELLANEOUS ,0105 earth and related environmental sciences ,Physics ,[PHYS]Physics [physics] ,Jet (fluid) ,Range (particle radiation) ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,comets: general ,Leitungsbereich PF ,comets: individual: 67P/Churyumov-Gerasimenko ,Astronomy and Astrophysics ,Plume ,13. Climate action ,Space and Planetary Science ,[SDU]Sciences of the Universe [physics] ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] - Abstract
On 2015 July 18, near perihelion at a heliocentric distance of 1.28 au, the Visible InfraRed Thermal Imaging Spectrometer (VIRTIS-M) on board the Rosetta spacecraft had the opportunity of observing dust activity in the inner coma with a view of the night side (shadowed side) of comet 67P/Churyumov-Gerasimenko. At the time of the measurements we present here, we observe a dust plume that originates on the far side of the nucleus. We are able to identify the approximate location of its source at the boundary between the Hapi and Anuket regions, and we find that it has been in darkness for some hours before the observation. Assuming that this time span is equal to the conductive time scale, we obtain a thermal inertia in the range 25–36 W K−1 m−2 s−1/2. These thermal inertia values can be used to verify with a 3D finite-element method (FEM) numerical code whether the surface and subsurface temperatures agree with the values found in the literature. We explored three different configurations: (1) a layer of water ice mixed with dust beneath a dust mantle of 5 mm with thermal inertia of 36 J m−2 K−1 s−0.5; (2) the same structure, but with thermal inertia of 100 J m−2 K−1 s−0.5; (3) an ice-dust mixture that is directly exposed. Of these three configurations, the first seems to be the most reasonable, both for the low thermal inertia and for the agreement with the surface and subsurface temperatures that have been found for the comet 67P/Churyumov-Gerasimenko. The spectral properties of the plume show that the visible dust color ranged from 16 ± 4.8%/100 nm to 13 ± 2.6%/100 nm, indicating that this plume has no detectable color gradient. The morphology of the plume can be classified as a narrow jet that has an estimated total ejected mass of between 6 and 19 tons when we assume size distribution indices between −2.5 and −3.
- Published
- 2019
188. Analysis of night-side dust activity on comet 67P observed by VIRTIS-M
- Author
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Rinaldi, G., Formisano, M., Kappel, David, Capaccioni, F., Bockelee-Morvan, D., Cheng, Y-C, Vincent, J-B, Deshapriya, P., Arnold, G., Capria, M. T., Ciarniello, M., De Sanctis, M. C., Doose, L., Erard, S., Federico, C., Filacchione, G., Fink, U., Leyrat, C., Longobardo, A., Magni, G., Mighorini, A., Mottola, S., Naletto, G., Raponi, A., Taylor, F., Tosi, F., Tozzi, G. P., and Salatti, M.
- Subjects
Institut für Physik und Astronomie ,ddc:530 - Abstract
On 2015 July 18, near perihelion at a heliocentric distance of 1.28 au, the Visible InfraRed Thermal Imaging Spectrometer (VIRTIS-M) on board the Rosetta spacecraft had the opportunity of observing dust activity in the inner coma with a view of the night side (shadowed side) of comet 67P/Churyumov-Gerasimenko. At the time of the measurements we present here, we observe a dust plume that originates on the far side of the nucleus. We are able to identify the approximate location of its source at the boundary between the Hapi and Anuket regions, and we find that it has been in darkness for some hours before the observation. Assuming that this time span is equal to the conductive time scale, we obtain a thermal inertia in the range 25-36 W K-1 m(-2) s(-1/2). These thermal inertia values can be used to verify with a 3D finite-element method (REM) numerical code whether the surface and subsurface temperatures agree with the values found in the literature. We explored three different configurations: (1) a layer of water ice mixed with dust beneath a dust mantle of 5 mm with thermal inertia of 36 J m(-2) K-1 S-0.5 ; (2) the same structure, but with thermal inertia of 100 J m(-2) K-1 S-0.5; (3) an ice-dust mixture that is directly exposed. Of these three configurations, the first seems to be the most reasonable, both for the low thermal inertia and for the agreement with the surface and subsurface temperatures that have been found for the comet 67P/Churyumov-Gerasimenko. The spectral properties of the plume show that the visible dust color ranged from 16 +/- 4.8%/100 nm to 13 +/- 2.6%/100 nm, indicating that this plume has no detectable color gradient. The morphology of the plume can be classified as a narrow jet that has an estimated total ejected mass of between 6 and 19 tons when we assume size distribution indices between -2.5 and -3.
- Published
- 2019
189. Dust composition in the innermost coma of comet 67P from the VIRTIS-M spectra: Organic features detection
- Author
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Rinaldi, G., D'Aversa, E., Bockelee-Morvan, D., Raponi, A, Capaccioni, F., Ciarniello, M., Filacchione, G., De Sanctis, M. C., Oliva, F., Kappel, David, Longobardo, A, Tosi, F., Capria, M., and Taylor, F.
- Subjects
Asteroiden und Kometen ,Rosetta ,Comet 67P ,Dust ,VIRTIS - Abstract
The Rosetta/ESA spacecraft followed the comet 67P/Churyumov-Gerasimenko from 2014 August (3.6 au pre-perihelion) to 2016 September (3.6 au post-perihelion). This offered a unique opportunity to analyze the time evolution of the dust properties in the inner coma. Onboard Rosetta, the Visual Infrared and Thermal Imaging Spectrometer (VIRTIS-M) acquired spectra of the dust coma in the spectral range 0.25 to 5 μm.
- Published
- 2019
190. Geometric preprocessing for Rosetta/VIRTIS-M measurements of comet 67P/C-G
- Author
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Kappel, David, Arnold, Gabriele, Moroz, Liubov, Raponi, A., Ciarniello, M., Tosi, F., Erard, S., Leyrat, C., Blecka, M., Filacchione, G., and Capaccioni, F.
- Subjects
Asteroiden und Kometen ,Leitungsbereich PF ,Rosetta ,Comet 67P ,Geometry ,VIRTIS - Abstract
Following earlier surface spectrophotometric analyses of Rosetta/VIRTIS-M measurements of comet 67P/Churyumov-Gerasimenko (hereafter 67P), we refine the instrument's geometric registration model and spatial consistency of the radiometric calibration. For this purpose we compare measured 67P nucleus images from the entire mission to corresponding photometric simulations and determine an optical distortion map between them. The refinements will allow us to improve the retrieval of physical and compositional surface properties of the comet's nucleus.
- Published
- 2019
191. Solar System Ice Giants: Exoplanets in our Backyard
- Author
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Rymer, A, Mandt, K, Hurley, D, Lisse, C, Izenberg, N, Smith, HT, Westlake, J, Bunce, E, Arridge, C, Masters, A, Hofstadter, M, Simon, A, Brandt, P, Clark, G, Cohen, I, Allen, R, Vine, S, Hansen, K, Hospodarsky, G, Kurth, W, Romani, P, Lamy, L, Zarka, P, Cao, H, Paty, C, Hedman, M, Roussos, E, Cruikshank, D, Farrell, W, Fieseler, P, Coates, A, Yelle, R, Parkinson, C, Militzer, B, Grodent, D, Kollmann, P, McNutt, R, André, N, Strange, N, Barnes, J, Dones, L, Denk, T, Rathbun, J, Lunine, J, Desai, R, Cochrane, C, Sayanagi, KM, Postberg, F, Ebert, R, Hill, T, Mueller-Wodarg, I, Regoli, L, Pontius, D, Stanley, S, Greathouse, T, Saur, J, Marouf, E, Bergman, J, Higgins, C, Johnson, R, Thomsen, M, Soderlund, K, Jia, X, Wilson, R, Englander, J, Burch, J, Nordheim, T, Grava, C, Baines, K, Quick, L, Russell, C, Cravens, T, Cecconi, B, Aslam, S, Bray, V, Garcia-Sage, K, Richardson, J, Clark, J, Hsu, S, Achterberg, R, Sergis, N, Paganelli, F, Kempf, S, Orton, G, Portyankina, G, Jones, G, Economou, T, Livengood, T, Krimigi, S, Szalay, J, Jackman, C, Valek, P, Lecacheux, A, Colwell, J, Jasinski, J, Tosi, F, Sulaiman, A, Galand, M, Kotova, A, Khurana, K, Kivelson, M, Strobel, D, Radiota, A, Estrada, P, Livi, S, Azari, A, Yates, J, Allegrini, F, Vogt, M, Felici, M, Luhmann, J, Filacchione, G, and Moore, L
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Astrophysics::High Energy Astrophysical Phenomena ,Physics::Space Physics ,astro-ph.EP ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Physics::Atmospheric and Oceanic Physics - Abstract
Future remote sensing of exoplanets will be enhanced by a thorough investigation of our solar system Ice Giants (Neptune-size planets). What can the configuration of the magnetic field tell us (remotely) about the interior, and what implications does that field have for the structure of the magnetosphere; energy input into the atmosphere, and surface geophysics (for example surface weathering of satellites that might harbour sub-surface oceans). How can monitoring of auroral emission help inform future remote observations of emission from exoplanets? Our Solar System provides the only laboratory in which we can perform in-situ experiments to understand exoplanet formation, dynamos, systems and magnetospheres.
- Published
- 2019
192. Aumento dell'espressione di marker di apoptosi ed autofagia in ostriche concave (Crassostrea gigas) allevate nel Medio Adriatico durante un periodo di mortalità
- Author
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Galosi, L., Roncarati, A., Gennari, L., Tosi, F., Gastaldelli, M., Arcangeli, G., Rossi, G., Mariotti, F., and Magi, G. E.
- Published
- 2019
193. Observing regions of interest on Ganymede and Callisto with JUICE
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Tosi, F., Stephan, Katrin, Palumbo, P., Piccioni, G., Langevin, Y., Altieri, F., Carter, J., Cremonese, G., D’Aversa, E., Della Corte, V., Filacchione, G., Galuzzi, V., Lucchetti, A., Massironi, M., Migliorini, A., Poulet, F., and Roatsch, Thomas
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Planetengeologie ,JUICE - Published
- 2019
194. Seasonal variations of milk quality in Parmigiano-Reggiano cheese manufacture on a period of 10 years
- Author
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Malacarne, M., primary, Fossa, E., additional, Sandri, S., additional, Tosi, F., additional, Summer, A., additional, and Mariani, P., additional
- Published
- 2003
- Full Text
- View/download PDF
195. Surface composition of Hyperion
- Author
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Cruikshank, D. P., Dalton, J. B., Dalle Ore, C. M., Bauer, J., Stephan, K., Filacchione, G., Hendrix, A. R., Hansen, C. J., Coradini, A., Cerroni, P., Tosi, F., Capaccioni, F., Jaumann, R., Buratti, B. J., Clark, R. N., Brown, R. H., Nelson, R. M., McCord, T. B., Baines, K. H., Nicholson, P. D., Sotin, C., Meyer, A. W., Bellucci, G., Combes, M., Bibring, J.-P., Langevin, Y., Sicardy, B., Matson, D. L., Formisano, V., Drossart, P., and Mennella, V.
- Published
- 2007
- Full Text
- View/download PDF
196. Ring-mold craters within Occator Crater, Ceres: evidence for subsurface ice reservoirs
- Author
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Krohn, Katrin, Jaumann, R., Neesemann, Adrian, Otto, Katharina A., Stephan, Katrin, Wagner, Roland, Tosi, F., Zambon, F., Ruesch, Ottaviano, Williams, D.A., Raymond, C.A., and Russell, C.T.
- Subjects
Planetengeologie ,Asteroiden und Kometen ,asteroids ,water-ice ,cryovolcanism ,crater Formation ,small bodies - Published
- 2018
197. Perioperative management of face-to-face craniopagus twins separation
- Author
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PIETRINI, D., VALENTI, M., PUSATERI, A., SCORZONI, M., TOSI, F., FORTE, E., BARBI, S., CARESTA, E., CALDARELLI, M., DI ROCCO, C., and PIASTRA, M.
- Published
- 2005
198. Studies on the mechanism of action of sulphonylureas in type II diabetic subjects: gliquidone
- Author
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Bonora, Enzo, Moghetti, P., Querena, M., Zenere, M., Cacciatori, V., Tosi, F., Travia, D., Zoppini, G., and Muggeo, M.
- Published
- 1992
- Full Text
- View/download PDF
199. Role of the pupillometer in the assessment of pain in the sedation of pediatric patients.
- Author
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TOSI, F., GATTO, A., CAPOSSELA, L., FERRETTI, S., MANCINO, A., CURATOLA, A., CHIARETTI, A., and PULITANÒ, S.
- Abstract
OBJECTIVE: Pupillometry has been used to assess pain intensity and response to analgesic drugs in adults. The aim of this study was to verify the usefulness and effectiveness of the pupillometer to assess pain and depth of sedation in pediatric patients undergoing painful procedures and to optimize pain management by observing pupillary variations induced by opioids. PATIENTS AND METHODS: This is a prospective, monocentric study conducted in the sedation room of the Pediatric Intensive Care Unit of Fondazione Policlinico A. Gemelli in Rome. A population of 22 pediatric patients who underwent painful procedures was enrolled. Eleven children were sedated by opioid drugs. Heart rate, systolic blood pressure, diastolic blood pressure, bispectral index, maximum pupil size (Size), pupil change (CH), Neurological Pupil Index (NPi) were collected over four times: before starting the procedure; before the painful stimulus (when the patient was sedated); when the painful stimulus was applied; at the end of the procedure. A NeurOptics NPi-200 pupillometer was used for the study. RESULTS: Statistical significance in the variation of haemodynamic parameters was less significant than the variation obtained by analyzing the pupillary parameters: a significant change in NPi and CH in the transition from wakefulness to sedation and from the application of the painful stimulus to awakening was found in both study populations, patients who have received opioids and patients who have not received opioids. Changes in the mean CH of the pupil diameter correlate with the depth of sedation and the size values vary in relation to the administration of opioids. CONCLUSIONS: Our findings highlight the potential role of pupillometry as a non-invasive method to objectively quantitate pain response in children to reach an efficient analgesic approach. [ABSTRACT FROM AUTHOR]
- Published
- 2021
200. Assessment of β-cell function during the oral glucose tolerance test by a minimal model of insulin secretion
- Author
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Cretti, A., Lehtovirta, M., Bonora, E., Brunato, B., Zenti, M. G., Tosi, F., Caputo, M., Caruso, B., Groop, L. C., Muggeo, M., and Bonadonna, R. C.
- Published
- 2001
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