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14 results on '"Istituto Fisica Spazio Interplanetario"'

6. Erratum: Comet 67P outbursts and quiescent coma at 1.3 au from the Sun: dust properties from Rosetta/VIRTIS-H observations

Author

Dominique Bockelée-Morvan, G Rinaldi, S Erard, C Leyrat, F Capaccioni, P Drossart, G Filacchione, A Migliorini, E Quirico, S Mottola, G Tozzi, G Arnold, N Biver, M Combes, J Crovisier, A Longobardo, M Blecka, M-T Capria, 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), IASI (IASI), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Istituto Fisica Spazio Interplanetario, Dysoxie, suractivité : aspects cellulaires et intégratifs thérapeutiques (DS-ACI / UMR MD2), Aix Marseille Université (AMU)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Consiglio Nazionale delle Ricerche (CNR), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Santé et de la Recherche Médicale (INSERM), and bibliotheque, la.

Subjects
[PHYS]Physics [physics], Asteroiden und Kometen, 010504 meteorology & atmospheric sciences, comets: general, Leitungsbereich PF, comets: individual: 67P/Churyumov-Gerasimenko, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, [PHYS] Physics [physics], 13. Climate action, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], infrared: planetary systems, 010303 astronomy & astrophysics, addenda, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, errata, 0105 earth and related environmental sciences
Abstract

The paper 'Comet 67P outbursts and quiescent coma at 1.3 AU from the Sun: dust properties from Rosetta/VIRTIS-H observations' was published in MNRAS 469, S443 (2017). While performing a follow-up investigation, we discovered a numerical error in the algorithms that were developed to model the infrared continuum emission from a population of dust particles. The results of the scattering models for compact or moderately porous grains (Mie theory) and fluffy grains (Rayleigh-Gans-Debye theory, RGD) are both affected. Though the general conclusions of the paper are unchanged, the quantitative constraints obtained on the dust size distribution in the quiescent coma are slightly different.

Published
2018

7. Equivalent block transmissivity in an irregular 2D polygonal grid for one-phase flow: A sensitivity analysis

Author

Vincent Lagneau, Roberto Bruno, Marco De Lucia, Chantal de Fouquet, Université de Bologne, Centre de Géosciences (GEOSCIENCES), MINES ParisTech - École nationale supérieure des mines de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Istituto Fisica Spazio Interplanetario, Istituto Nazionale di Astrofisica (INAF), De Lucia M., De Fouquet Ch., Lagneau V., Bruno R., and 0 Pre-GFZ, Departments, GFZ Publication Database, Deutsches GeoForschungsZentrum

Subjects
upscaling, 010504 meteorology & atmospheric sciences, Discretization, [SDE.MCG]Environmental Sciences/Global Changes, Flow (psychology), 0207 environmental engineering, 550 - Earth sciences, Geometry, 02 engineering and technology, Geostatistics, 01 natural sciences, Physics::Geophysics, Range (statistics), Sensitivity (control systems), 020701 environmental engineering, Variogram, finite volumes, voronoï mesh, 0105 earth and related environmental sciences, Hydrology, Global and Planetary Change, heterogeneous medium, equivalent permeability, VORONÏ MESH, Grid, flow, General Earth and Planetary Sciences, spatial variability, Spatial variability, Geology
Abstract

International audience; Upscaling is needed to transform the representation of non additive space-dependent variables, such as permeability, from the fine grid of geostatistical simulations (to simulate small scale spatial variability) to the coarser, generally irregular grids for hydrodynamic transport codes. A new renormalisation method is proposed, based on the geometric properties of a Voronoï grid. It is compared to other classic methods by a sensitivity analysis (grid, range and sill of the variogram, random realisation of a simulation); the criterion is the flux of a tracer at the outlet. The effect of the upscaling technique on the results appears to be of second order compared to the spatial discretisation, the choice of variogram, and the realisation.

Published
2009

8. The light curve of asteroid 21 Lutetia measured by VIRTIS-M during the Rosetta fly-by

Author

Tosi, F., Capaccioni, F., Coradini, A., Erard, S., Filacchione, G., De Sanctis, M.C., Capria, M.T., Giuppi, S., Carraro, F., Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Istituto Fisica Spazio Interplanetario, 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, and 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)

Subjects
[PHYS]Physics [physics], 010504 meteorology & atmospheric sciences, Space and Planetary Science, 0103 physical sciences, Astronomy and Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, 01 natural sciences, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract

International audience

Published
2012

9. Water production in comet 81P/Wild 2 as determined by Herschel/HIFI

Author

Nicolas Biver, Emmanuel Jehin, A. Di Giorgio, Miriam Rengel, M. I. Błęcka, José Cernicharo, Geoffrey A. Blake, S. Philipp, M. de Val-Borro, Christoffel Waelkens, Joris Blommaert, Slawomira Szutowicz, R. Szczerba, Alexander S. Medvedev, Michael Küppers, Pierre Encrenaz, Dariusz C. Lis, Paul Hartogh, Paolo Saraceno, T. Encrenaz, David A. Naylor, Bart Vandenbussche, Dominique Bockelée-Morvan, Raphael Moreno, Luisa Lara, Volker Ossenkopf, P. Zaal, Emmanuel Lellouch, R. Shipman, Martin Emprechtinger, Leen Decin, B. M. Swinyard, T. de Graauw, F. Bensch, Jacques Crovisier, C. Jarchow, R. Schieder, Jean Manfroid, N. Thomas, Marek Banaszkiewicz, T. Klein, M. Kidger, Edwin Bergin, Daphne Stam, Damien Hutsemekers, Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, 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), Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Space Research Centre, Polish Academy of Sciences (Wroclaw), German Aerospace Centre (DLR), Institut d'Astrophysique, Géophysique et Océanographie, Université de Liège, Rosetta Science Operations Centre, Instituto de Astrofisica de Andalucia, CSIC (IAA), STFC Rutherford Appleton Laboratory, Harwell Innovation Campus, Didcot, Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Astronomy Department, University of Michigan, Laboratorio de Astrofísica Molecular, CAB-CSIC/INTA (LAM), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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 de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Instrumentation et télédétection, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Dynamique des milieux interstellaires et plasmas stellaires, Joint ALMA Observatory, Santiago, Science Centre, Department of Physics and Astronomy, University of Lethbridge, Physikalisches Institut, Universität zu Köln, SRON Netherlands Institute for Space Research, Physikalisches Institut, Universität Bern, Centrum Astronomiczne im. M. Kopernika, Torun (CAMK), Istituto Fisica Spazio Interplanetario, INAF, Max-Planck-Institut für Radioastronomie (MPIfR), and Astronomy

Subjects
Electron density, 010504 meteorology & atmospheric sciences, Mean kinetic temperature, SURFACE, Infrared, Comet, FOS: Physical sciences, Astrophysics, Electron, 01 natural sciences, SPACECRAFT, 0103 physical sciences, H2O, Spectral resolution, 010303 astronomy & astrophysics, SATELLITE, 0105 earth and related environmental sciences, Line (formation), Physics, Earth and Planetary Astrophysics (astro-ph.EP), ASTRONOMY, Astronomy and Astrophysics, submillimeter: general, molecular processes, 13. Climate action, Space and Planetary Science, radiative transfer, ODIN, comets: individual: 81P/Wild 2, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Excitation, HIFI, Astrophysics - Earth and Planetary Astrophysics
Abstract

The high spectral resolution and sensitivity of Herschel/HIFI allows for the detection of multiple rotational water lines and accurate determinations of water production rates in comets. In this letter we present HIFI observations of the fundamental 110-101 (557 GHz) ortho and 111-000 (1113 GHz) para rotational transitions of water in comet 81P/Wild 2 acquired in February 2010. We mapped the extent of the water line emission with five point scans. Line profiles are computed using excitation models which include excitation by collisions with electrons and neutrals and solar infrared radiation. We derive a mean water production rate of $1.0 \times 10^{28}$ molecules s$^{-1}$ at a heliocentric distance of 1.61 AU about 20 days before perihelion, in agreement with production rates measured from the ground using observations of the 18-cm OH lines. Furthermore, we constrain the electron density profile and gas kinetic temperature, and estimate the coma expansion velocity by fitting the water line shapes., Accepted for publication in A&A (special issue on HIFI first results)

Published
2010

10. ATLASGAL - The APEX Telescope Large Area Survey of the Galaxy at 870 microns

Author

Schuller, F., Menten, K. M., Contreras, Y., Wyrowski, F., Schilke, P., Bronfman, L., Henning, T., Walmsley, C. M., Beuther, H., Bontemps, Sylvain, Cesaroni, R., Deharveng, L., Garay, G., Herpin, Fabrice, Lefloch, B., Linz, H., Mardones, D., Minier, V., Molinari, S., Motte, F., Nyman, L. -A., Reveret, V., Risacher, C., Russeil, D., Schneider, N., Testi, L., Troost, T., Vasyunina, T., Wienen, M., Zavagno, Annie, Kovacs, A., Kreysa, E., Siringo, G., Weiss, A., Max-Planck-Institut für Radioastronomie (MPIFR), Departamento de Astronomia (DAS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Istituto Fisica Spazio Interplanetario, ESO, European Southern Observatory (ESO), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and Universidad de Santiago de Chile [Santiago] (USACH)

Subjects
[PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Galaxy Astrophysics
Abstract

(Abridged) Studying continuum emission from interstellar dust is essential to locating and characterizing the highest density regions in the interstellar medium. In particular, the early stages of massive star formation remain poorly understood. Our goal is to produce a large-scale, systematic database of massive pre- and proto-stellar clumps in the Galaxy, to understand how and under what conditions star formation takes place. A well characterized sample of star-forming sites will deliver an evolutionary sequence and a mass function of high-mass, star-forming clumps. This systematic survey at submm wavelengths also represents a preparatory work for Herschel and ALMA. The APEX telescope is ideally located to observe the inner Milky Way. The Large APEX Bolometer Camera (LABOCA) is a 295-element bolometer array observing at 870 microns, with a beam size of 19". Taking advantage of its large field of view (11.4') and excellent sensitivity, we started an unbiased survey of the Galactic Plane, with a noise level of 50-70 mJy/beam: the APEX Telescope Large Area Survey of the Galaxy (ATLASGAL). As a first step, we covered 95 sq. deg. These data reveal 6000 compact sources brighter than 0.25 Jy, as well as extended structures, many of them filamentary. About two thirds of the compact sources have no bright infrared counterpart, and some of them are likely to correspond to the precursors of (high-mass) proto-stars or proto-clusters. Other compact sources harbor hot cores, compact HII regions or young embedded clusters. Assuming a typical distance of 5 kpc, most sources are clumps smaller than 1 pc with masses from a few 10 to a few 100 M_sun. In this introductory paper, we show preliminary results from these ongoing observations, and discuss the perspectives of the survey., Accepted for publication in A&A, 13 pages, 14 figures. Final version after language editing

Published
2009

11. Distribution Of Icy Particles Across Enceladus' Surface As Derived From Cassini-vims Measurements

Author

Robert H. Brown, P. D. Nicholson, Katrin Stephan, Gianrico Filacchione, Gary B. Hansen, Charles A. Hibbitts, Angioletta Coradini, Dale P. Cruikshank, Robert M. Nelson, Caitlin A. Griffith, T. B. McCord, B. J. Buratti, Roland Wagner, Ralf Jaumann, Kevin H. Baines, Christophe Sotin, Roger N. Clark, S. Newman, Giancarlo Bellucci, Institute of Geological Sciences [Berlin], Department of Earth Sciences [Berlin], Free University of Berlin (FU)-Free University of Berlin (FU), Bear Fight Institute, California Institute of Technology (CALTECH), University of Arizona, Istituto Fisica Spazio Interplanetario, NASA Ames Research Center (ARC), Department of Astronomy [Ithaca], Cornell University [New York], and Université de Nantes (UN)

Subjects
Surface (mathematics), [PHYS]Physics [physics], Range (particle radiation), 010504 meteorology & atmospheric sciences, Spectrometer, Infrared, Impact gardening, Astronomy, Mineralogy, Astronomy and Astrophysics, 01 natural sciences, Spectral line, Enceladus, Saturn, satellites, Space and Planetary Science, 0103 physical sciences, Physical Sciences, Particle, 010303 astronomy & astrophysics, Geology, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract

The surface of Enceladus consists almost completely of water ice. As the band depths of water ice absorptions are sensitive to the size of particles, absorptions can be used to map variations of icy particles across the surface. The Visual and Infrared Mapping Spectrometer (VIMS) observed Enceladus with a high spatial resolution during three Cassini flybys in 2005 (orbits EN 003, EN 004 and EN 011). Based on these data we measured the band depths of water ice absorptions at 1.04, 1.25, 1.5, and 2 μm. These band depths were compared to water ice models that represent theoretically calculated reflectance spectra for a range of particle diameters between 2 μm and 1 mm. The agreement between the experimental (VIMS) and model values supports the assumption that pure water ice characterizes the surface of Enceladus and therefore that variations in band depth correspond to variations in water ice particle diameters. Our measurements show that the particle diameter of water ice increases toward younger tectonically altered surface units with the largest particles exposed in relatively “fresh” surface material. The smallest particles were generally found in old densely cratered terrains. The largest particles (∼0.2 mm) are concentrated in the so called “tiger stripes” at the south pole. In general, the particle diameters are strongly correlated with geologic features and surface ages, indicating a stratigraphic evolution of the surface that is caused by cryovolcanic resurfacing and impact gardening.

Published
2008

12. Radon indoor, in rocks and groundwater: data integration for mapping in Emilia-Romagna

Author

Sgallari, S., De Fouquet, Chantal, Bruno, R., Angelini, P., Centre de Géosciences (GEOSCIENCES), MINES ParisTech - École nationale supérieure des mines de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Istituto Fisica Spazio Interplanetario, and Istituto Nazionale di Astrofisica (INAF)

Subjects
[STAT.AP]Statistics [stat]/Applications [stat.AP], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2006

13. Cassini VIMS observations of the Galilean satellites including the VIMS calibration procedure

Author

Jean-Pierre Bibring, Angioletta Coradini, Yves Langevin, G. B. Hansen, Gianrico Filacchione, P. D. Nicholson, Priscilla Cerroni, Robert M. Nelson, M. Combes, Pierre Drossart, Kevin H. Baines, Bonnie J. Buratti, Fabrizio Capaccioni, Giancarlo Bellucci, Dennis L. Matson, Charles A. Hibbitts, Roger N. Clark, Dale P. Cruikshank, Vittorio Formisano, Robert H. Brown, Thomas B. McCord, Bruno Sicardy, E. Bussoletti, Christophe Sotin, Ralf Jaumann, Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), HIGP/SOEST, University of Hawaii, Istituto Fisica Spazio Interplanetario, INAF, Planetary Science Institute, 22 Fiddler's Rd., Winthrop, Istituto Astrofisica Spaziale e Fisica Cosmica, CNR, US Geological Survey, Denver, Department Planetary Science and LPL, University of AZ, Tucson, Jet Propulsion Laboratory, California Institute of Technology (JPL), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), Departement de recherche SPAtiale (DESPA), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), 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), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), NASA Ames Research Center, Astrophysics Branch, Moffett Field, Department of Planetary Exploration, DLR, Department of Astronomy, Cornell University, and Université de Nantes (UN)

Subjects
010504 meteorology & atmospheric sciences, Satellite surfaces, 01 natural sciences, Space mission, Jovian, Jupiter, symbols.namesake, Saturn, 0103 physical sciences, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Remote sensing, Spectrometer, Spacecraft, business.industry, Near-infrared spectroscopy, Astronomy, Astronomy and Astrophysics, Galilean satellites, Galilean moons, Satellites de Glace, 13. Climate action, Space and Planetary Science, Surface composition, Physics::Space Physics, symbols, Astrophysics::Earth and Planetary Astrophysics, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Jupiter system, Geology, Data reduction
Abstract

The Visual and Infrared Mapping Spectrometer (VIMS) observed the Galilean satellites during the Cassini spacecraft's 2000/2001 flyby of Jupiter, providing compositional and thermal information about their surfaces. The Cassini spacecraft approached the jovian system no closer than about 126 Jupiter radii, about 9 million kilometers, at a phase angle of

Published
2004

14. Test of general relativity and measurement of the lense-thirring effect with two earth satellites

Author

Ciufolini I I, Pavlis E, Chieppa F, Fernandes-Vieira E, and Perez-Mercader J

Abstract

The Lense-Thirring effect, a tiny perturbation of the orbit of a particle caused by the spin of the attracting body, was accurately measured with the use of the data of two laser-ranged satellites, LAGEOS and LAGEOS II, and the Earth gravitational model EGM-96. The parameter &mgr;, which measures the strength of the Lense-Thirring effect, was found to be 1.1 +/- 0.2; general relativity predicts &mgr; identical with 1. This result represents an accurate test and measurement of one of the fundamental predictions of general relativity, that the spin of a body changes the geometry of the universe by generating space-time curvature.

Published
1998
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