Search

Your search keyword '"Lainey V"' showing total 334 results
Start Over Author "Lainey V"
334 results on '"Lainey V"'

101. Precise CCD positions of Galilean satellite-pairs

Author

Peng, Q., He, H., Lainey, V., Vienne, A., Unité de Mécanique (UME), École Nationale Supérieure de Techniques Avancées (ENSTA Paris), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), 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 de Lille-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)

Subjects
[PHYS]Physics [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2012
Full Text
View/download PDF

102. GETEMME - A Mission to Explore the Martian Satellites and the Limits of Solar System Physics

Author

Oberst, J., Lainey, V., Le Poncin-Lafitte, C., German Aerospace Centre (DLR) and the Technical University of Berlin, Germany, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), 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 de Lille-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, and Université Paris sciences et lettres (PSL)

Subjects
Getemme, laser ranging, Martian satellites, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Solar System Physics
Abstract

International audience; We propose a mission to Mars and its satellites Phobos and Deimos, within the ESA COSMIC VISION program. A spacecraft (S/C) shall deploy retroreflectors on each satellite. These reflectors will act as targets for laser ranging from a Martian orbit for a wide range of science applications in Solar System Dynamics and Fundamental Physics.

Published
2011

103. A new astrometric reduction of photographic plates using the DAMIAN digitizer: improving the dynamics of the Jovian system

Author

Robert-Pélissier, Vincent, De Cuyper, Jean-Pierre, Arlot, Jean-Eudes, de Decker, Georges, Guibert, Jean, Lainey, V., Pascu, Dan, Winter, Lars, Zacharias, Norbert, Institut Polytechnique des Sciences Avancées (IPSA), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Royal Observatory of Belgium [Brussels] (ROB), Galaxies, Etoiles, Physique, Instrumentation (GEPI), 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), United States Naval Observatory (USNO), 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 de Lille-Centre National de la Recherche Scientifique (CNRS)

Subjects
planets and satellites, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], astrometry, ephemerides, image processing
Abstract

International audience; The astrometric monitoring of the natural planetary satellites is an important step to assess the formation and the evolution of these systems. However, in order to quantify relevant gravitational effects such as tidal forces, it is necessary to have very accurate observations over a long time interval. Unfortunately, the accuracy is decreasing as one considers older observations. To solve this issue, digitizing of old photographic plates is an attractive method, but a high accuracy in the measurement and the reduction of those plates is absolutely necessary.We have developed methods and algorithms adapted to specific plates provided by USNO, using the DAMIAN digitizer of ROB. From a set of 35 plates taken in 1974, we have been able to produce measurements with an accuracy better than 0.08 μm and after reduction using the UCAC2 catalogue, rms residuals of 35 mas (1.7 μm) for intersatellite positions (when the original reduction provided 100 mas) and of 65 mas for equatorial RA and Dec. positions (which were not possible to get with the original reduction). First results on the dynamics of the satellites and of the planet Jupiter are provided.

Published
2011
Full Text
View/download PDF

105. A new astrometric measurement and reduction of USNO photographic observations of Phobos and Deimos: 1967–1997

Author

UCL - SST/ELI/ELIC - Earth & Climate, Robert, V., Lainey, V., Pascu, D., Pasewaldt, A., Arlot, J.-E., De Cuyper, J.-P., Dehant, Véronique, Thuillot, W., UCL - SST/ELI/ELIC - Earth & Climate, Robert, V., Lainey, V., Pascu, D., Pasewaldt, A., Arlot, J.-E., De Cuyper, J.-P., Dehant, Véronique, and Thuillot, W.

Abstract

Context. Accurate positional measurements of planets and satellites are used to improve our knowledge of both their orbits and their dynamics and to infer the accuracy of the planet and satellite ephemerides. Aims. In the framework of the European FP7 ESPaCE program, we provide the positions of Mars, Phobos, and Deimos taken with the US Naval Observatory 61-inch astrometric reflector and 26-inch refractor from 1967 to 1997. Methods. Four hundred twenty five astrophotographic plates were measured with the digitizer of the Royal Observatory of Belgium and reduced through an optimal process that includes image, instrumental, and spherical corrections using the UCAC4 catalog to provide the most accurate equatorial (RA, Dec) positions. Results. We compared the observed positions of the planet Mars and its satellites with the theoretical positions from INPOP13c and DE430 planetary ephemerides and from NOE MarsSatV1_0 and MAR097 satellite ephemerides. The rms residuals in RA and Dec of one position are less than 62 mas or about 20 km at the opposition of Mars. The rms intersatellite residuals in RA and Dec of one position are less than 40 mas or about 13 km at Mars. This accuracy is comparable to the most recent CCD observations. We also fitted the NOE model to the new computed positions and compared the orbital evolution of Phobos and Deimos with those derived from the same model, but only fitted to spacecraft data. Our results show that astrophotographic plate data can now compete with those of old spacecraft.

Published
2015

106. Constraining multiple systems with GAIA

Author

Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Binzel, Richard P., Beauvalet, L., Lainey, V., Arlot, J.-E., Bancelin, D., Marchis, F., Binzel, Richard P, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Binzel, Richard P., Beauvalet, L., Lainey, V., Arlot, J.-E., Bancelin, D., Marchis, F., and Binzel, Richard P

Abstract

GAIA will provide observations of some multiple asteroid and dwarf systems. These observations are a way to determine and improve the quantification of dynamical parameters, such as the masses and the gravity fields, in these multiple systems. Here we investigate this problem in the cases of Pluto's and Eugenia's system. We simulate observations reproducing an approximate planning of the GAIA observations for both systems, as well as the New Horizons observations of Pluto. We have developed a numerical model reproducing the specific behavior of multiple asteroid system around the Sun and fit it to the simulated observations using least-square method, giving the uncertainties on the fitted parameters. We found that GAIA will improve significantly the precision of Pluto's and Charon's mass, as well as Petit Prince's orbital elements and Eugenia's polar oblateness.

Published
2015

108. Astrometric positions for 18 irregular satellites of giant planets from 23 years of observations

Author

Gomes-Júnior, A. R., primary, Assafin, M., additional, Vieira-Martins, R., additional, Arlot, J.-E., additional, Camargo, J. I. B., additional, Braga-Ribas, F., additional, da Silva Neto, D. N., additional, Andrei, A. H., additional, Dias-Oliveira, A., additional, Morgado, B. E., additional, Benedetti-Rossi, G., additional, Duchemin, Y., additional, Desmars, J., additional, Lainey, V., additional, and Thuillot, W., additional

Published
2015
Full Text
View/download PDF

109. Implications of rotation, orbital states, energy sources, and heat transport ofr internal processes in icy satellites

Author

Hussmann, H., Choblet, G., Lainey, V., D. L., Matson, Sotin, C., Tobie, G., Hoolst T., Van, Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), and Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU.STU]Sciences of the Universe [physics]/Earth Sciences, ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2010

110. Latest VO developments at Paris VO Data Center

Author

Le Sidaner, P., Dubernet, M. -L, Simon, G., Aboudarham, J., Baillard, A., Barache, C., Boone, F., Chilingarian, I., Dantel-Fort, M., Desert, J. M., Didelon, P., Egret, D., Guibert, J., Hebrard, G., Lainey, V., Magnard, F., Chiara Marmo, Martin, J. M., Pelat, D., Renié, C., Sarkissian, A., Schneider, J., Theureau, G., Vachier, F., Observatoire de Paris - Site de Paris (OP), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), 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), Ingénieurs, Techniciens et Administratifs, 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Physique solaire, Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), CEA- Saclay (CEA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Service d'aéronomie (SA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Groupe Astrométrie et Planétologie (GAP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, D. Barret, F. Casoli, T. Contini, G. Lagache, A. Lecavelier, and and L. Pagani (eds)

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; Paris VO Data Center aims at providing VO access to its databases ressources, at participating to international standards developments, at implementing VO compliant simulation codes and data visuali- sation and analysis softwares. We will present some of the latest VO developments involving ressources from Paris VO Data Center, i.e, the first simple spectra access for data of the Nanay radiotelescope observatory, a validator for Simple Spectra Access protocols and its implementation tools, a Cone-search access to the exoplanet catalog, a pipeline for images processing to make them ”science-ready” in vo-format, implemen- tation of Simple Image Access using Geographic Information System in databases. Developments involving other ressources may be found in their own contributions to this meeting.

Published
2006

111. Phobos' acceleration and Mars interior

Author

Rivoldini, A., Lainey, V., Verhoeven, O., Mocquet, A., Hoolst T., Van, Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), and Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2006

112. Implementing Ephemerides Facilities in the VizieR and Aladin Tools

Author

Berthier, J., Vachier, F., Lainey, V., Thuillot, W., Arlot, J. -E, Fernique, P., Ochsenbein, F., Francoise Genova, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), 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 de Lille-Centre National de la Recherche Scientifique (CNRS), Laboratoire Gemini (LG), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Tsvetkov, M., Golev, V., Murtagh, F., Molina, and R.

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; The Institut de mecanique celeste et de calcul des ephemerides (IMCCE, Paris Observatory) is willing to provide information on Solar System objects to the Astronomical Virtual Observatory. The first step is the interconnection of IMCCE ephemerides servers with the Vizier and Aladin tools of the Centre de donnees astronomiques de Strasbourg (CDS). The services have been made interoperable, using the International Virtual Observatory standard VOTable. A request related to the position of asteroids made by users of Aladin or Vizier is transmitted to the ephemerides servers of IMCCE and the answer is quickly and automatically returned. Equipped with this new facility, Aladin allows in particular users to explore photographic archives stored at CDS, observatory archives accessible through Aladin, or to process their own images, in order to identify asteroids. The ephemerides are obtained from a numerical integration using as initial conditions the orbital data extracted from the Lowell database of asteroids. This work is still in development but, at this stage, the method is well established and we intend to give access to this tool in a few months.

Published
2006

113. VO Paris Federation

Author

Simon, G., Dubernet, M. L., Le Sidaner, P., Aboudarham, J., Barache, C., Berthier, J., Boone, F., Borsenberger, J., Caillat, M., Igor Chilingarian, Crovisier, J., Dantel-Fort, M., Debatz, B., Dedieu, C., Egret, D., Gontier, A. M., Guibert, J., Guillaume, D., Haigron, R., Hennebelle, P., Jegouzo, I., Lainey, V., Le Bourlot, J., Le Petit, F., Martin, J. M., Micheneau, P., Moreau, N., Pelat, D., Perault, M., Prugniel, P., Renié, C., Roques, F., Royer, F., Schneider, J., Tajahmady, F., Theureau, G., Thuillot, W., Tran-Minh, F., Vachier, F., Vetois, J., Viallefond, F., Baillard, A., Bertin, E., Desert, J. M., Ferlet, R., Hebrard, G., Magnard, F., Malapert, J. -C, Marquette, J. B., Marmo, C., Mellier, Y., Sarkissian, A., Mccracken, H., Lesquoy, E., Didelon, P., 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), Ingénieurs, Techniciens et Administratifs, 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, 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), Physique solaire, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Groupe Astrométrie et Planétologie (GAP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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), Service d'aéronomie (SA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), CEA- Saclay (CEA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), C. Gabriel, C. Arviset, D. Ponz and E. Solano, eds., Henry, Florence, and C. Gabriel, C. Arviset, D. Ponz and E. Solano, eds.

Subjects
[PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], PADC
Abstract

International audience; VO Paris Federation is a partnership between Paris Obser-vatory, IAP, IPSL and CEA. Its objectives are to provide VO access toits databases ressources, contribute to international standards develop-ments, implement VO compliant simulation codes and data visualisa-tion and analysis software. The various activities are organised into por-tals whose functions are (i) to provide visibility and information on theprojects and (ii) to encourage collaborations. The portals are linked tothematic activities and resources: solar system (ephemerides, astrometry,physical characteristic of small bodies of the solar system, planetology),reference systems, exoplanet database, legacy (archives from the Nan ̧cayRadio Telescope, some specific data from the DENIS and EROS surveys,MAMA), solar physics, stellar and galactic databases and services, atomicand molecular databases and services, simulation codes and data analysis.

Published
2005

114. Io's acceleration vs. Observational accuracy

Author

Lainey, V., Tobie, G., Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), and Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2004

118. Astrometric Observations of Phobos and Deimos During the 1971 Opposition of Mars

Author

NAVAL OBSERVATORY WASHINGTON DC, robert, V, Lainey, V, Pascu, D, Arlot, J, De Cuyper, J, Dehant, V, Thuillot, W, NAVAL OBSERVATORY WASHINGTON DC, robert, V, Lainey, V, Pascu, D, Arlot, J, De Cuyper, J, Dehant, V, and Thuillot, W

Abstract

Context. Accurate positional measurements of planets and satellites are used to improve our knowledge of their dynamics and to infer the accuracy of planet and satellite ephemerides. Aims. In the framework of the FP7 ESPaCE project, we provide the positions of Mars, Phobos, and Deimos taken with the U.S. Naval Observatory 26-inch refractor during the 1971 opposition of the planet. Methods. These plates were measured with the digitizer of the Royal Observatory of Belgium and reduced through an optimal process that includes image, instrumental, and spherical corrections to provide the most accurate data. Results. We compared the observed positions of the planet Mars and its satellites with the theoretical positions from INPOP10 and DE430 planetary ephemerides, and from NOE and MAR097 satellite ephemerides. The rms residuals in RA and Dec. of one position is less than 60 mas, or about 20 km at Mars. This accuracy is comparable to the most recent CCD observations. Moreover, it shows that astrometric data derived from photographic plates can compete with those of old spacecraft (Mariner 9, Viking 1 and 2)., Published in Astronomy & Astrophysics, October 6, 2014. The original document contains color images.

Published
2014

120. The science case for an orbital mission to Uranus: Exploring the origins and evolution of ice giant planets

Author

Arridge, C. S., Achilleos, N., Agarwal, J., Agnor, C. B., Ambrosi, R., Andre, N., Badman, S. V., Baines, K., Banfield, D., Barthelemy, M., Bisi, M. M., Blum, J., Bocanegra-Bahamon, T., Bonfond, B. ., Bracken, C., Brandt, P., Briand, C., Briois, C., Brooks, S., Castillo-Rogez, J., Cavalie, T., Christophe, B., Coates, A. J., Collinson, G., Cooper, J. F., Costa-Sitja, M., Courtin, R., Daglis, I. A., De Pater, I., Desai, M., Dirkx, D., Dougherty, M. K., Ebert, R. W., Filacchione, G., Fletcher, L. N., Fortney, J., Gerth, I., Grassi, D., Grodent, D., Grun, E., Gustin, J., Hedman, M., Helled, R., Henri, P., Hess, S., Hillier, J. K., Hofstadter, M. H., Holme, R., Horanyi, M., Hospodarsky, G., Hsu, S., Irwin, P., Jackman, C. M., Karatekin, O., Kempf, S., Khalisi, E., Konstantinidis, K., Kruger, H., Kurth, W. S., Labrianidis, C., Lainey, V., Lamy, L. L., Laneuville, M., Lucchesi, D., Luntzer, A., MacArthur, J., Maier, A., Masters, A., McKenna-Lawlor, S., Melin, H., Milillo, A., Moragas-Klostermeyer, G., Morschhauser, A., Moses, J. I., Mousis, O., Nettelmann, N., Neubauer, F. M., Nordheim, T., Noyelles, B., Orton, G. S., Owens, M., Peron, R., Plainaki, C., Postberg, F., Rambaux, N., Retherford, K., Reynaud, S., Roussos, E., Russell, C. T., Rymer, Am., Sallantin, R., Sanchez-Lavega, A., Santolik, O., Saur, J., Sayanagi, Km., Schenk, P., Schubert, J., Sergis, N., Sittler, E. C., Smith, A., Spahn, F., Srama, R., Stallard, T., Sterken, V., Sternovsky, Z., Tiscareno, M., Tobie, G., Tosi, F., Trieloff, M., Turrini, D., Turtle, E. P., Vinatier, S., Wilson, R., Zarkat, P., Arridge, C. S., Achilleos, N., Agarwal, J., Agnor, C. B., Ambrosi, R., Andre, N., Badman, S. V., Baines, K., Banfield, D., Barthelemy, M., Bisi, M. M., Blum, J., Bocanegra-Bahamon, T., Bonfond, B. ., Bracken, C., Brandt, P., Briand, C., Briois, C., Brooks, S., Castillo-Rogez, J., Cavalie, T., Christophe, B., Coates, A. J., Collinson, G., Cooper, J. F., Costa-Sitja, M., Courtin, R., Daglis, I. A., De Pater, I., Desai, M., Dirkx, D., Dougherty, M. K., Ebert, R. W., Filacchione, G., Fletcher, L. N., Fortney, J., Gerth, I., Grassi, D., Grodent, D., Grun, E., Gustin, J., Hedman, M., Helled, R., Henri, P., Hess, S., Hillier, J. K., Hofstadter, M. H., Holme, R., Horanyi, M., Hospodarsky, G., Hsu, S., Irwin, P., Jackman, C. M., Karatekin, O., Kempf, S., Khalisi, E., Konstantinidis, K., Kruger, H., Kurth, W. S., Labrianidis, C., Lainey, V., Lamy, L. L., Laneuville, M., Lucchesi, D., Luntzer, A., MacArthur, J., Maier, A., Masters, A., McKenna-Lawlor, S., Melin, H., Milillo, A., Moragas-Klostermeyer, G., Morschhauser, A., Moses, J. I., Mousis, O., Nettelmann, N., Neubauer, F. M., Nordheim, T., Noyelles, B., Orton, G. S., Owens, M., Peron, R., Plainaki, C., Postberg, F., Rambaux, N., Retherford, K., Reynaud, S., Roussos, E., Russell, C. T., Rymer, Am., Sallantin, R., Sanchez-Lavega, A., Santolik, O., Saur, J., Sayanagi, Km., Schenk, P., Schubert, J., Sergis, N., Sittler, E. C., Smith, A., Spahn, F., Srama, R., Stallard, T., Sterken, V., Sternovsky, Z., Tiscareno, M., Tobie, G., Tosi, F., Trieloff, M., Turrini, D., Turtle, E. P., Vinatier, S., Wilson, R., and Zarkat, P.

Abstract

Giant planets helped to shape the conditions we see in the Solar System today and they account for more than 99% of the mass of the Sun's planetary system. They can be subdivided into the Ice Giants (Uranus and Neptune) and the Gas Giants (Jupiter and Saturn), which differ from each other in a number of fundamental ways. Uranus, in particular is the most challenging to our understanding of planetary formation and evolution, with its large obliquity, low self-luminosity, highly asymmetrical internal field, and puzzling internal structure. Uranus also has a rich planetary system consisting of a system of inner natural satellites and complex ring system, five major natural icy satellites, a system of irregular moons with varied dynamical histories, and a highly asymmetrical magnetosphere. Voyager 2 is the only spacecraft to have explored Uranus, with a flyby in 1986, and no mission is currently planned to this enigmatic system. However, a mission to the uranian system would open a new window on the origin and evolution of the Solar System and would provide crucial information on a wide variety of physicochemical processes in our Solar System. These have clear implications for understanding exoplanetary systems. In this paper we describe the science case for an orbital mission to Uranus with an atmospheric entry probe to sample the composition and atmospheric physics in Uranus' atmosphere. The characteristics of such an orbiter and a strawman scientific payload are described and we discuss the technical challenges for such a mission. This paper is based on a white paper submitted to the European Space Agency's call for science themes for its large-class mission programme in 2013. (C) 2014 Published by Elsevier Ltd.

Published
2014

121. The science case for an orbital mission to Uranus:exploring the origins and evolution of ice giant planets

Author

Arridge, C. S., Achilleos, N., Agarwal, J., Agnor, C. B., Ambrosi, R., Andre, N., Badman, S. V., Baines, K., Banfield, D., Barthelemy, M., Bisi, M. M., Blum, J., Bocanegra-Bahamon, T., Bonfond, B. ., Bracken, C., Brandt, P., Briand, C., Briois, C., Brooks, S., Castillo-Rogez, J., Cavalie, T., Christophe, B., Coates, A. J., Collinson, G., Cooper, J. F., Costa-Sitja, M., Courtin, R., Daglis, I. A., De Pater, I., Desai, M., Dirkx, D., Dougherty, M. K., Ebert, R. W., Filacchione, G., Fletcher, L. N., Fortney, J., Gerth, I., Grassi, D., Grodent, D., Grun, E., Gustin, J., Hedman, M., Helled, R., Henri, P., Hess, S., Hillier, J. K., Hofstadter, M. H., Holme, R., Horanyi, M., Hospodarsky, G., Hsu, S., Irwin, P., Jackman, C. M., Karatekin, O., Kempf, S., Khalisi, E., Konstantinidis, K., Kruger, H., Kurth, W. S., Labrianidis, C., Lainey, V., Lamy, L. L., Laneuville, M., Lucchesi, D., Luntzer, A., MacArthur, J., Maier, A., Masters, A., McKenna-Lawlor, S., Melin, H., Milillo, A., Moragas-Klostermeyer, G., Morschhauser, A., Moses, J. I., Mousis, O., Nettelmann, N., Neubauer, F. M., Nordheim, T., Noyelles, B., Orton, G. S., Owens, M., Peron, R., Plainaki, C., Postberg, F., Rambaux, N., Retherford, K., Reynaud, S., Roussos, E., Russell, C. T., Rymer, Am., Sallantin, R., Sanchez-Lavega, A., Santolik, O., Saur, J., Sayanagi, Km., Schenk, P., Schubert, J., Sergis, N., Sittler, E. C., Smith, A., Spahn, F., Srama, R., Stallard, T., Sterken, V., Sternovsky, Z., Tiscareno, M., Tobie, G., Tosi, F., Trieloff, M., Turrini, D., Turtle, E. P., Vinatier, S., Wilson, R., Zarkat, P., Arridge, C. S., Achilleos, N., Agarwal, J., Agnor, C. B., Ambrosi, R., Andre, N., Badman, S. V., Baines, K., Banfield, D., Barthelemy, M., Bisi, M. M., Blum, J., Bocanegra-Bahamon, T., Bonfond, B. ., Bracken, C., Brandt, P., Briand, C., Briois, C., Brooks, S., Castillo-Rogez, J., Cavalie, T., Christophe, B., Coates, A. J., Collinson, G., Cooper, J. F., Costa-Sitja, M., Courtin, R., Daglis, I. A., De Pater, I., Desai, M., Dirkx, D., Dougherty, M. K., Ebert, R. W., Filacchione, G., Fletcher, L. N., Fortney, J., Gerth, I., Grassi, D., Grodent, D., Grun, E., Gustin, J., Hedman, M., Helled, R., Henri, P., Hess, S., Hillier, J. K., Hofstadter, M. H., Holme, R., Horanyi, M., Hospodarsky, G., Hsu, S., Irwin, P., Jackman, C. M., Karatekin, O., Kempf, S., Khalisi, E., Konstantinidis, K., Kruger, H., Kurth, W. S., Labrianidis, C., Lainey, V., Lamy, L. L., Laneuville, M., Lucchesi, D., Luntzer, A., MacArthur, J., Maier, A., Masters, A., McKenna-Lawlor, S., Melin, H., Milillo, A., Moragas-Klostermeyer, G., Morschhauser, A., Moses, J. I., Mousis, O., Nettelmann, N., Neubauer, F. M., Nordheim, T., Noyelles, B., Orton, G. S., Owens, M., Peron, R., Plainaki, C., Postberg, F., Rambaux, N., Retherford, K., Reynaud, S., Roussos, E., Russell, C. T., Rymer, Am., Sallantin, R., Sanchez-Lavega, A., Santolik, O., Saur, J., Sayanagi, Km., Schenk, P., Schubert, J., Sergis, N., Sittler, E. C., Smith, A., Spahn, F., Srama, R., Stallard, T., Sterken, V., Sternovsky, Z., Tiscareno, M., Tobie, G., Tosi, F., Trieloff, M., Turrini, D., Turtle, E. P., Vinatier, S., Wilson, R., and Zarkat, P.

Abstract

Giant planets helped to shape the conditions we see in the Solar System today and they account for more than 99% of the mass of the Sun's planetary system. They can be subdivided into the Ice Giants (Uranus and Neptune) and the Gas Giants (Jupiter and Saturn), which differ from each other in a number of fundamental ways. Uranus, in particular is the most challenging to our understanding of planetary formation and evolution, with its large obliquity, low self-luminosity, highly asymmetrical internal field, and puzzling internal structure. Uranus also has a rich planetary system consisting of a system of inner natural satellites and complex ring system, five major natural icy satellites, a system of irregular moons with varied dynamical histories, and a highly asymmetrical magnetosphere. Voyager 2 is the only spacecraft to have explored Uranus, with a flyby in 1986, and no mission is currently planned to this enigmatic system. However, a mission to the uranian system would open a new window on the origin and evolution of the Solar System and would provide crucial information on a wide variety of physicochemical processes in our Solar System. These have clear implications for understanding exoplanetary systems. In this paper we describe the science case for an orbital mission to Uranus with an atmospheric entry probe to sample the composition and atmospheric physics in Uranus' atmosphere. The characteristics of such an orbiter and a strawman scientific payload are described and we discuss the technical challenges for such a mission. This paper is based on a white paper submitted to the European Space Agency's call for science themes for its large-class mission programme in 2013. (C) 2014 Published by Elsevier Ltd.

Published
2014

122. Dynamical parameter determinations in Pluto’s system

Author

Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Binzel, Richard P., Beauvalet, L., Lainey, V., Arlot, J.-E., Binzel, Richard P, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Binzel, Richard P., Beauvalet, L., Lainey, V., Arlot, J.-E., and Binzel, Richard P

Abstract

Pluto is the multiple system that has been observed the longest. Yet, the masses of its smallest satellites, Nix and Hydra, which were discovered in 2005, are still imprecisely known, because of the short time span and number of available observations. We present a numerical model that takes into account the second order gravity fields and Pluto’s orbital motion in the solar system. We investigated the dynamical parameters that may be reliably determined today. We also assessed the possible improvements on the parameter uncertainties with the future increase of observations, including the New Horizons mission. Fitting our model to simulated data, we show that the precision of observations prevents the quantification of the polar oblateness J2 and equatorial bulge c22 of Pluto and Charon. Similarly, we show that the masses are on the detection limit. In particular, unless 25 observations are made every year, the mass of Nix may be constrained with confidence only with New Horizons data. Hydra’s mass will only be constrained by the probe. The recent discovery of P4 might change this situation, but our knowledge of this object is still too vague to draw any conclusion., United States. National Aeronautics and Space Administration (New Horizons Mission science team)

Published
2014

126. Théorie dynamique des satellites galiléens

Author

Lainey, V., Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Observatoire de Paris, A.Vienne(L.Duriez), 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 de Lille-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU]Sciences of the Universe [physics], astrometry, dynamique orbitale, éphémérides, astrométrie, orbital dynamics
Abstract

We have developed a new dynamical model of the Galilean system fitted to astrometric observations. A numerical code has been developed for simulating the orbital motion of the satellites. Many perturbations usually neglected have been quantified, improving greatly the modeling of the system. The numerical solution has been fitted to various kinds of observations (photographic, CCD and mutual phenomena) done between 1891 and 2002. More than 2000 observations have been used, including the PHEMU campaigns of 1985 and 1991. A frequency analysis was finally used to obtain an orbital representation under an analytical form. A digital filtering treatment for removing the short periods from the long ones has been developed, hence solving some technical problems such as the length of the sample and the long solar periods. Our theory has an accuracy of a few tens of kilometres over one century and remains valid for more than 1500 years.; Nous avons élaboré une nouvelle théorie dynamique des satellites galiléens ajustée aux observations. Un programme numérique a été développé afin de pouvoir simuler le mouvement des satellites. Nous avons ainsi évalué une grande quantité de perturbations généralement négligées, et ainsi grandement amélioré la modélisation du système. La solution numérique a ensuite été ajustée à plusieurs types d'observations (photographiques, CCD et phénomènes mutuels) entre les années 1891 et 2002. Un total de plus de 2000 observations a été utilisé, dont les observations des campagnes PHEMU de 1985 et 1991. Une analyse en fréquence a finalement été effectuée dans la perspective d'obtenir une représentation sous forme analytique du système. Une méthode de filtrage pour séparer les courtes périodes des longues périodes a été développée pour résoudre des difficultés techniques (longueur d'échantillonnage, longues périodes solaires).Notre théorie a aujourd'hui une fidélité de représentation de quelques dizaines de kilomètres sur un siècle, et reste définie sur plus de 1500 ans.

Published
2002

127. Radioscience simulations in general relativity and in alternative theories of gravity

Author

UCL - SST/ELI - Earth and Life Institute, FUNDP - SMAT_Systèmes dynamiques, Hees, Aurélien, Lamine, B., Reynaud, S., Jaekel, M.-T., Le Poncin-Lafitte, C., Lainey, V., Fuzfa, Andre, Courty, J.-M., Dehant, Véronique, Wolf, P., UCL - SST/ELI - Earth and Life Institute, FUNDP - SMAT_Systèmes dynamiques, Hees, Aurélien, Lamine, B., Reynaud, S., Jaekel, M.-T., Le Poncin-Lafitte, C., Lainey, V., Fuzfa, Andre, Courty, J.-M., Dehant, Véronique, and Wolf, P.

Abstract

This paper deals with tests of general relativity (GR) in the Solar System using tracking observables from planetary spacecraft. We present a new software that simulates the Range and Doppler signals resulting from a given spacetime metric. This flexible approach allows one to perform simulations in GR as well as in alternative metric theories of gravity. The outputs of this software provide templates of anomalous residuals that should show up in real data if the underlying theory of gravity is not GR. Those templates can be used to give a rough estimation of constraints on additional parameters entering alternative theory of gravity and also signatures that can be searched for in data from past or future space missions aiming at testing gravitational laws in the Solar System. As an application of the potentiality of this software, we present some simulations performed for Cassini-like mission in post-Einsteinian gravity and in the context of MOND external field effect. We derive signatures arising from these alternative theories of gravity and estimate expected amplitudes of the anomalous residuals.

Published
2012

128. A New Astrometric Reduction of Photographic Plates Using the DAMIAN Digitizer: Improving the Dynamics of the Jovian System

Author

NAVAL OBSERVATORY WASHINGTON DC, Robert, V., De Cuyper, J., Arlot, J., de Decker, G., Guibert, J., Lainey, V., Pascu, D., Winter, L., Zacharias, N., NAVAL OBSERVATORY WASHINGTON DC, Robert, V., De Cuyper, J., Arlot, J., de Decker, G., Guibert, J., Lainey, V., Pascu, D., Winter, L., and Zacharias, N.

Abstract

The astrometric monitoring of the natural planetary satellites is an important step to assess the formation and the evolution of these systems. However, in order to quantify relevant gravitational effects such as tidal forces, it is necessary to have very accurate observations over a long time interval. Unfortunately, the accuracy is decreasing as one considers older observations. To solve this issue, digitizing of old photographic plates is an attractive method, but a high accuracy in the measurement and the reduction of those plates is absolutely necessary. We have developed methods and algorithms adapted to specific plates provided by USNO, using the DAMIAN digitizer of ROB. From a set of 35 plates taken in 1974, we have been able to produce measurements with an accuracy better than 0.08 micrometers and after reduction using the UCAC2 catalogue, rms residuals of 35 mas (1.7 micrometers) for intersatellite positions (when the original reduction provided 100 mas) and of 65 mas for equatorial RA and Dec. positions (which were not possible to get with the original reduction). First results on the dynamics of the satellites and of the planet Jupiter are provided., Published in Monthly Notices Royal Astronomical Society, Online Early (MNRAS Homepage) (2011). The original document contains color images. Also supported by IMCCE Paris and CNRS Paris.

Published
2011

129. The PHEMU03 catalogue of observations of the mutual phenomena of the Galilean satellites of Jupiter

Author

Arlot, J. -E., Thuillot, W., Ruatti, C., Ahmad, A., Amosse, A., Anbazhagan, P., Andreyev, M., Antov, A., Appakutty, M., Asher, D., Aubry, S., Baron, N., Bassiere, N., Berthe, M., Bogdanovski, R., Bosq, F., Bredner, E., Buettner, D., Buromsky, M., Cammarata, S., Casas, R., Chis, G. D., Christou, A. A., Coquerel, J. -P., Corlan, R., Cremaschini, C., Crussaire, D., Cuypers, J., Dennefeld, M., Descamps, P., Devyatkin, A., Dimitrov, D., Dorokhova, T. N., Dorokhov, N. I., Dourneau, G., Duenas, M., Dumitrescu, A., Emelianov, N., Ferrara, D., Fiel, D., Fienga, A., Flatres, T., Foglia, S., Garlitz, J., Gerbos, J., Gilbert, R., Goncalves, R. M. D., Gonzales, D., Gorda, S. Yu., Gorshanov, D. L., Hansen, M. W., Harrington, M., Irsmambetova, T. R., Ito, Y., Ivanova, V., Izmailov, I. S., Khovritchev, M. Yu., Khrutskaya, E. V., Kieken, J., Kiseleva, T. P., Kuppuswamy, K., Lainey, V., Lavayssiere, M., Lazzarotti, P., Le Campion, J. -F., Lellouch, E., Li, Z. L., Lo Savio, E., Lou, M., Magny, E., Manek, J., Marinello, W., Marino, G., McAuliffe, J. P., Michelli, M., Moldovan, D., Montagnac, S., Moorthy, V., Nickel, O., Nier, J. M., Noel, T., Noyelles, B., Oksanen, A., Parrat, D., Pauwels, T., Peng, Q. Y., Pizzetti, G., Priban, V., Ramachandran, B., Rambaux, N., Rapaport, M., Rapavy, P., Rau, G., Sacre, J. -J., Sada, P. V., Salvaggio, F., Sarlin, P., Sciuto, C., Selvakumar, G., Sergeyev, A., Sidorov, M., Sorescu, S., Spampinato, S. A., Stellmacher, I., Trunkovsky, E., Tejfel, V., Tudose, V., Turcu, V., Ugarte, I., Vantyghem, P., Vasundhara, R., Vaubaillon, J., Velu, C., Venkataramana, A. K., Vidal-Sainz, J., Vienne, A., Vilar, J., Vingerhoets, P., Vollman, W., Arlot, J. -E., Thuillot, W., Ruatti, C., Ahmad, A., Amosse, A., Anbazhagan, P., Andreyev, M., Antov, A., Appakutty, M., Asher, D., Aubry, S., Baron, N., Bassiere, N., Berthe, M., Bogdanovski, R., Bosq, F., Bredner, E., Buettner, D., Buromsky, M., Cammarata, S., Casas, R., Chis, G. D., Christou, A. A., Coquerel, J. -P., Corlan, R., Cremaschini, C., Crussaire, D., Cuypers, J., Dennefeld, M., Descamps, P., Devyatkin, A., Dimitrov, D., Dorokhova, T. N., Dorokhov, N. I., Dourneau, G., Duenas, M., Dumitrescu, A., Emelianov, N., Ferrara, D., Fiel, D., Fienga, A., Flatres, T., Foglia, S., Garlitz, J., Gerbos, J., Gilbert, R., Goncalves, R. M. D., Gonzales, D., Gorda, S. Yu., Gorshanov, D. L., Hansen, M. W., Harrington, M., Irsmambetova, T. R., Ito, Y., Ivanova, V., Izmailov, I. S., Khovritchev, M. Yu., Khrutskaya, E. V., Kieken, J., Kiseleva, T. P., Kuppuswamy, K., Lainey, V., Lavayssiere, M., Lazzarotti, P., Le Campion, J. -F., Lellouch, E., Li, Z. L., Lo Savio, E., Lou, M., Magny, E., Manek, J., Marinello, W., Marino, G., McAuliffe, J. P., Michelli, M., Moldovan, D., Montagnac, S., Moorthy, V., Nickel, O., Nier, J. M., Noel, T., Noyelles, B., Oksanen, A., Parrat, D., Pauwels, T., Peng, Q. Y., Pizzetti, G., Priban, V., Ramachandran, B., Rambaux, N., Rapaport, M., Rapavy, P., Rau, G., Sacre, J. -J., Sada, P. V., Salvaggio, F., Sarlin, P., Sciuto, C., Selvakumar, G., Sergeyev, A., Sidorov, M., Sorescu, S., Spampinato, S. A., Stellmacher, I., Trunkovsky, E., Tejfel, V., Tudose, V., Turcu, V., Ugarte, I., Vantyghem, P., Vasundhara, R., Vaubaillon, J., Velu, C., Venkataramana, A. K., Vidal-Sainz, J., Vienne, A., Vilar, J., Vingerhoets, P., and Vollman, W.

Published
2009

132. First numerical ephemerides of the Martian moons

Author

UCL - SST/ELI/ELIC - Earth & Climate, Lainey, V., Dehant, Véronique, Pätzold, M., UCL - SST/ELI/ELIC - Earth & Climate, Lainey, V., Dehant, Véronique, and Pätzold, M.

Published
2007

136. Astrometric results of observations of mutual occultations and eclipses of the Saturnian satellites in 2009

Author

Arlot, J.-E., primary, Emelyanov, N. V., additional, Lainey, V., additional, Andreev, M., additional, Assafin, M., additional, Braga-Ribas, F., additional, Camargo, J. I. B., additional, Casas, R., additional, Christou, A., additional, Colas, F., additional, Da Silva Neto, D. N., additional, Dechambre, O., additional, Dias-Oliveira, A., additional, Dourneau, G., additional, Farmakopoulos, A., additional, Gault, D., additional, George, T., additional, Gorshanov, D. L., additional, Herald, D., additional, Kozlov, V., additional, Kurenya, A., additional, Le Campion, J. F., additional, Lecacheux, J., additional, Loader, B., additional, Massallé, A., additional, Mc Brien, M., additional, Murphy, A., additional, Parakhin, N., additional, Roman-Lopes, A., additional, Schnabel, C., additional, Sergeev, A., additional, Tsamis, V., additional, Valdés Sada, P., additional, Vieira-Martins, R., additional, and Zhang, X., additional

Published
2012
Full Text
View/download PDF

141. More than 160 near Earth asteroids observed in the EURONEAR network

Author

Birlan, M., primary, Vaduvescu, O., additional, Tudorica, A., additional, Sonka, A., additional, Nedelcu, A., additional, Galad, A., additional, Colas, F., additional, Pozo N., F., additional, Barr D., A., additional, Toma, R., additional, Comsa, I., additional, Rocher, P., additional, Lainey, V., additional, Vidican, D., additional, Asher, D., additional, Opriseanu, C., additional, Vancea, C., additional, Colque, J. P., additional, Soto, C. P., additional, Rekola, R., additional, and Unda-Sanzana, E., additional

Published
2010
Full Text
View/download PDF

143. The PHEMU03 catalogue of observations of the mutual phenomena of the Galilean satellites of Jupiter

Author

Arlot, J.-E., primary, Thuillot, W., additional, Ruatti, C., additional, Ahmad, A., additional, Amossé, A., additional, Anbazhagan, P., additional, Andreyev, M., additional, Antov, A., additional, Appakutty, M., additional, Asher, D., additional, Aubry, S., additional, Baron, N., additional, Bassiere, N., additional, Berthe, M., additional, Bogdanovski, R., additional, Bosq, F., additional, Bredner, E., additional, Buettner, D., additional, Buromsky, M., additional, Cammarata, S., additional, Casas, R., additional, Chis, G. D., additional, Christou, A. A., additional, Coquerel, J.-P., additional, Corlan, R., additional, Cremaschini, C., additional, Crussaire, D., additional, Cuypers, J., additional, Dennefeld, M., additional, Descamps, P., additional, Devyatkin, A., additional, Dimitrov, D., additional, Dorokhova, T. N., additional, Dorokhov, N. I., additional, Dourneau, G., additional, Dueñas, M., additional, Dumitrescu, A., additional, Emelianov, N., additional, Ferrara, D., additional, Fiel, D., additional, Fienga, A., additional, Flatres, T., additional, Foglia, S., additional, Garlitz, J., additional, Gerbos, J., additional, Gilbert, R., additional, Goncalves, R. M. D., additional, Gonzãles, D., additional, Gorda, S. Yu., additional, Gorshanov, D. L., additional, Hansen, M. W., additional, Harrington, M., additional, Irsmambetova, T. R., additional, Ito, Y., additional, Ivanova, V., additional, Izmailov, I. S., additional, Khovritchev, M. Yu., additional, Khrutskaya, E. V., additional, Kieken, J., additional, Kiseleva, T. P., additional, Kuppuswamy, K., additional, Lainey, V., additional, Lavayssiére, M., additional, Lazzarotti, P., additional, Le Campion, J.-F., additional, Lellouch, E., additional, Li, Z. L., additional, Lo Savio, E., additional, Lou, M., additional, Magny, E., additional, Manek, J., additional, Marinello, W., additional, Marino, G., additional, McAuliffe, J. P., additional, Michelli, M., additional, Moldovan, D., additional, Montagnac, S., additional, Moorthy, V., additional, Nickel, O., additional, Nier, J. M., additional, Noel, T., additional, Noyelles, B., additional, Oksanen, A., additional, Parrat, D., additional, Pauwels, T., additional, Peng, Q. Y., additional, Pizzetti, G., additional, Priban, V., additional, Ramachandran, B., additional, Rambaux, N., additional, Rapaport, M., additional, Rapavy, P., additional, Rau, G., additional, Sacré, J.-J., additional, Sada, P. V., additional, Salvaggio, F., additional, Sarlin, P., additional, Sciuto, C., additional, Selvakumar, G., additional, Sergeyev, A., additional, Sidorov, M., additional, Sorescu, S., additional, Spampinato, S. A., additional, Stellmacher, I., additional, Trunkovsky, E., additional, Tejfel, V., additional, Tudose, V., additional, Turcu, V., additional, Ugarte, I., additional, Vantyghem, P., additional, Vasundhara, R., additional, Vaubaillon, J., additional, Velu, C., additional, Venkataramana, A. K., additional, Vidal-Sãinz, J., additional, Vienne, A., additional, Vilar, J., additional, Vingerhoets, P., additional, and Vollman, W., additional

Published
2008
Full Text
View/download PDF

145. A project of teaching ground-based astrometry

Author

Arlot, J.-E., primary, Jin, W. J., additional, Zhu, J., additional, Peng, Q. Y., additional, Colas, F., additional, Shen, K. X., additional, Tang, Z. H., additional, Zhu, Z., additional, Lainey, V., additional, Thuillot, W., additional, and Vienne, A., additional

Published
2007
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results