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1,261 results on '"Bertaux, J.-L."'

101. Dust measurements in the coma of comet 67P/Churyumov-Gerasimenko inbound to the Sun

Author

Rotundi, A., Sierks, H., Corte, V. Della, Fulle, M., Gutierrez, P. J., Lara, L., Barbieri, C., Lamy, P. L., Rodrigo, R., Koschny, D., Rickman, H., Keller, H. U., López-Moreno, J. J., Accolla, M., Agarwal, J., A'Hearn, M. F., Altobelli, N., Angrilli, F., Barucci, M. A., Bertaux, J.-L., Bertini, I., Bodewits, D., Bussoletti, E., Colangeli, L., Cosi, M., Cremonese, G., Crifo, J.-F., Da Deppo, V., Davidsson, B., Debei, S., De Cecco, M., Esposito, F., Ferrari, M., Fornasier, S., Giovane, F., Gustafson, B., Green, S. F., Groussin, O., Grün, E., Güttler, C., Herranz, M. L., Hviid, S. F., Ip, W., Ivanovski, S., Jerónimo, J. M., Jorda, L., Knollenberg, J., Kramm, R., Kührt, E., Küppers, M., Lazzarin, M., Leese, M. R., López-Jiménez, A. C., Lucarelli, F., Lowry, S. C., Marzari, F., Epifani, E. Mazzotta, McDonnell, J. A. M., Mennella, V., Michalik, H., Molina, A., Morales, R., Moreno, F., Mottola, S., Naletto, G., Oklay, N., Ortiz, J. L., Palomba, E., Palumbo, P., Perrin, J.-M., Rodríguez, J., Sabau, L., Snodgrass, C., Sordini, R., Thomas, N., Tubiana, C., Vincent, J.-B., Weissman, P., Wenzel, K.-P., Zakharov, V., and Zarnecki, J. C.

Published
2015

108. Envisat/GOMOS Stellar Occultation: Inversion Schemes and First Analyses of Real Data

Author

Kyrölä, E., Tamminen, J., Leppelmeier, G. W., Sofieva, V. F., Hassinen, S., Bertaux, J. L., Hauchecorne, A., Dalaudier, F., Cot, C., Korablev, O., Fussen, D., Vanhellemont, F., d’Andon, O. Fanton, Barrot, G., Mangin, A., Theodore, B., Guirlet, M., Etanchaud, F., Snoeij, P., Koopman, R., Saavedra, L., Fraisse, R., Kirchengast, Gottfried, editor, Foelsche, Ulrich, editor, and Steiner, Andrea K., editor

Published
2004
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112. Evidence of Non‐Thermal Hydrogen in the Exosphere of Mars Resulting in Enhanced Water Loss.

Author

Bhattacharyya, D., Clarke, J. T., Mayyasi, M., Shematovich, V., Bisikalo, D., Chaufray, J. Y., Thiemann, E., Halekas, J., Schmidt, C., Bertaux, J. L., Chaffin, M. S., and Schneider, N. M.

Subjects
MARTIAN atmosphere, MARS (Planet), SOLAR wind, CHARGE exchange, SOLAR activity, ATMOSPHERIC layers, UPPER atmosphere
Abstract

Atomic H is a direct tracer of water loss at Mars. The recent discovery of annual enhancements in its escape rate near perihelion, in excess of the previously established theory, indicates that Mars has lost substantial amounts of water to space. However, these loss rates are often estimated assuming thermal properties for the exospheric H atoms and are therefore a lower limit. Past analyses of spacecraft observations delivered indirect evidence for the existence of an energetic non‐thermal H population without a clear detection. Here, we present the unambiguous observational signature of non‐thermal H at Mars, consistent with solar wind charge exchange as the primary driver for its production. The calculated non‐thermal escape rates are as high as ∼26% of the thermal rate near aphelion and solar minima. An active Sun would increase the present‐day escape rate and a younger energetic Sun likely contributed toward the significant historic loss of water from Mars. Plain Language Summary: The total water lost by Mars is determined by calculating the number of H atoms permanently escaping its upper atmosphere into space at present and extrapolating it back in time. The present‐day escape rate of H does not account for energetic H atoms, which were postulated to exist but not previously observed to date. Such a population would enhance the H escape rate further, thereby increasing the total volume of the water lost by Mars. This work presents the first confirmed signature of energetic H atoms in the atmosphere of Mars and finds that interaction of the neutral H population in its uppermost atmospheric layer, that is, its exosphere, with the solar wind results in its creation. The amount of energetic H atoms produced depends on the Mars' atmospheric conditions such as temperature and density of neutral H atoms in the exosphere, solar activity, and Mars' position around the Sun. Since the younger Sun was much more active than today, it is likely that the interaction of an early Martian exosphere with the stronger solar wind resulted in the loss of a larger fraction of H atoms into space than has been estimated to date. Key Points: Observations of H brightness at high altitude in Mars' atmosphere during aphelion solar minimum show an abrupt slope change above 5,000 kmHot H atoms produced via solar wind charge exchange can reproduce the observed profiles, providing evidence for nonthermal hydrogenSince this escape scales with solar wind flux, elevated loss rates early in Mars' history could result in much larger overall water loss [ABSTRACT FROM AUTHOR]

Published
2023
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117. Images of Asteroid 21 Lutetia: A Remnant Planetesimal from the Early Solar System

Author

Sierks, H., Lamy, P., Barbieri, C., Koschny, D., Rickman, H., Rodrigo, R., A'Hearn, M. F., Angrilli, F., Barucci, M. A., Bertaux, J.-L., Bertini, I., Besse, S., Carry, B., Cremonese, G., Da Deppo, V., Davidsson, B., Debei, S., De Cecco, M., De Leon, J., Ferri, F., Fornasier, S., Fulle, M., Hviid, S. F., Gaskell, R. W., Groussin, O., Gutierrez, P., Ip, W., Jorda, L., Kaasalainen, M., Keller, H. U., Knollenberg, J., Kramm, R., Kührt, E., Küppers, M., Lara, L., Lazzarin, M., Leyrat, C., Moreno, J. J. Lopez, Magrin, S., Marchi, S., Marzari, F., Massironi, M., Michalik, H., Moissl, R., Naletto, G., Preusker, F., Sabau, L., Sabolo, W., Scholten, F., Snodgrass, C., Thomas, N., Tubiana, C., Vernazza, P., Vincent, J.-B., Wenzel, K.-P., Andert, T., Pätzold, M., and Weiss, B. P.

Published
2011

119. E-Type Asteroid (2867) Steins as Imaged by OSIRIS on Board Rosetta

Author

Keller, H. U., Barbieri, C., Koschny, D., Lamy, P., Rickman, H., Rodrigo, R., Sierks, H., A'Hearn, M. F., Angrilli, F., Barucci, M. A., Bertaux, J.-L, Cremonese, G., Da Deppo, V., Davidsson, B., De Cecco, M., Debei, S., Fornasier, S., Fulle, M., Groussin, O., Gutierrez, P. J., Hviid, S. F., Ip, W.-H., Jorda, L., Knollenberg, J., Kramm, J. R., Kührt, E., Küppers, M., Lara, L.-M., Lazzarin, M., Moreno, J. Lopez, Marzari, F., Michalik, H., Naletto, G., Sabau, L., Wenzel, K.-P., Bertini, I., Besse, S., Ferri, F., Kaasalainen, M., Lowry, S., Marchi, S., Mottola, S., Sabolo, W., Schröder, S. E., Spjuth, S., and Vernazza, P.

Published
2010
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120. The Atmospheric Chemistry Suite (ACS) of Three Spectrometers for the ExoMars 2016 Trace Gas Orbiter

Author

Korablev, O., Montmessin, F., Trokhimovskiy, A., Fedorova, A. A., Shakun, A. V., Grigoriev, A. V., Moshkin, B. E., Ignatiev, N. I., Forget, F., Lefèvre, F., Anufreychik, K., Dzuban, I., Ivanov, Y. S., Kalinnikov, Y. K., Kozlova, T. O., Kungurov, A., Makarov, V., Martynovich, F., Maslov, I., Merzlyakov, D., Moiseev, P. P., Nikolskiy, Y., Patrakeev, A., Patsaev, D., Santos-Skripko, A., Sazonov, O., Semena, N., Semenov, A., Shashkin, V., Sidorov, A., Stepanov, A. V., Stupin, I., Timonin, D., Titov, A. Y., Viktorov, A., Zharkov, A., Altieri, F., Arnold, G., Belyaev, D. A., Bertaux, J. L., Betsis, D. S., Duxbury, N., Encrenaz, T., Fouchet, T., Gérard, J.-C., Grassi, D., Guerlet, S., Hartogh, P., Kasaba, Y., Khatuntsev, I., Krasnopolsky, V. A., Kuzmin, R. O., Lellouch, E., Lopez-Valverde, M. A., Luginin, M., Määttänen, A., Marcq, E., Martin Torres, J., Medvedev, A. S., Millour, E., Olsen, K. S., Patel, M. R., Quantin-Nataf, C., Rodin, A. V., Shematovich, V. I., Thomas, I., Thomas, N., Vazquez, L., Vincendon, M., Wilquet, V., Wilson, C. F., Zasova, L. V., Zelenyi, L. M., and Zorzano, M. P.

Published
2017
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124. SWAN: A Study of Solar Wind Anisotropies on SOHO With Lyman Alpha Sky Mapping

Author

Bertaux, J. L., Kyrölä, E., Quémerais, E., Pellinen, R., Lallement, R., Schmidt, W., Berthé, M., Dimarellis, E., Goutail, J. P., Taulemesse, C., Bernard, C., Leppelmeier, G., Summanen, T., Hannula, H., Huomo, H., Kehlä, V., Korpela, S., Leppälä, K., Strömmer, E., Torsti, J., Viherkanto, K., Hochedez, J. F., Chretiennot, G., Peyroux, R., Holzer, T., Fleck, B., editor, Domingo, V., editor, and Poland, A., editor

Published
1995
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126. Upgrades to the MAVEN Echelle Data Reduction Pipeline: New Calibration Standard and Improved Faint Emission Detection Algorithm at Lyman‐α.

Author

Mayyasi, M., Clarke, J., Bertaux, J.‐L., Deighan, J., Bhattacharyya, D., Chaffin, M., Jain, S., Schneider, N., and Curry, S.

Subjects
DATA reduction, MARTIAN atmosphere, SYNCOPE, ULTRAVIOLET spectrometers, CALIBRATION, SPECTROGRAPHS
Abstract

The Mars Atmosphere and Volatile Evolution (MAVEN) mission instrument suite includes an ultraviolet echelle spectrograph with high‐spectral resolution designed to resolve D and H Lyman‐α emissions. The high‐spectral resolution mode was previously characterized in the lab and in the cruise phase to Mars and had been calibrated using observations and models of interplanetary hydrogen Lyman‐α emissions. This work presents improved characterizations of the high‐spectral resolution mode using in‐orbit observations that allow for more robust detections of the faint D Lyman‐α emission line. Additionally, the instrument was re‐calibrated using simultaneous and comparable observations made with the Hubble Space Telescope high‐spectral resolution instrument. Comparisons to Lyman‐α observations made with the low‐resolution UV channel on the spectrometer, that had been calibrated with stars, showed consistency in the brightness values for measurements obtained at similar observational conditions. The combined upgrades to the faint‐emission fitting and new calibration techniques of the MAVEN echelle channel have resulted in an improved data‐reduction pipeline with favorable implications for the science utility of D and H Lyman‐α emissions. Plain Language Summary: The MAVEN high resolution echelle (ECH) instrument has been used to observe ultraviolet emissions from Mars. Measurements made with MAVEN/ECH were made available to the public by using a data reduction pipeline that had been developed with in‐lab and theoretical analysis to convert observations into a form that was useable by the broader scientific community. Since MAVEN's orbit insertion in 2014, the ECH detector has been better characterized with lessons learned from in‐orbit performance. These improvements produced a new data reduction pipeline that has enhanced the detection of faint D Lyman‐α emissions that are critical to interpreting water loss from the upper atmosphere of Mars. Key Points: MAVEN/ECH uses HST/STIS, the only other UV echelle instrument deployed to space, for calibration and independent verificationThe MAVEN/ECH data reduction algorithm has been upgraded to improve detection of faint D Lyman‐α emissionsThe scientific implications of this work include doubling the previous data set of D measurements available for reliable interpretation [ABSTRACT FROM AUTHOR]

Published
2023
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127. PHEBUS: A double ultraviolet spectrometer to observe Mercury's exosphere

Author

Chassefière, E., Maria, J.-L., Goutail, J.-P., Quémerais, E., Leblanc, F., Okano, S., Yoshikawa, I., Korablev, O., Gnedykh, V., Naletto, G., Nicolosi, P., Pelizzo, M.-G., Correia, J.-J., Gallet, S., Hourtoule, C., Mine, P.-O., Montaron, C., Rouanet, N., Rigal, J.-B., Muramaki, G., Yoshioka, K., Kozlov, O., Kottsov, V., Moisseev, P., Semena, N., Bertaux, J.-L., Capria, M.-Th., Clarke, J., Cremonese, G., Delcourt, D., Doressoundiram, A., Erard, S., Gladstone, R., Grande, M., Hunten, D., Ip, W., Izmodenov, V., Jambon, A., Johnson, R., Kallio, E., Killen, R., Lallement, R., Luhmann, J., Mendillo, M., Milillo, A., Palme, H., Potter, A., Sasaki, S., Slater, D., Sprague, A., Stern, A., and Yan, N.

Published
2010
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132. Extreme Ultraviolet Observations from Voyager 1 Encounter with Jupiter

Author

Broadfoot, A. L., Belton, M. J. S., Takacs, P. Z., Sandel, B. R., Shemansky, D. E., Holberg, J. B., Ajello, J. M., Atreya, S. K., Donahue, T. M., Moos, H. W., Bertaux, J. L., Blamont, J. E., Strobel, D. F., McConnell, J. C., Dalgarno, A., Goody, R., and McElroy, M. B.

Published
1979

133. Extreme Ultraviolet Observations from Voyager 2 Encounter with Jupiter

Author

Sandel, B. R., Shemansky, D. E., Broadfoot, A. L., Bertaux, J. L., Blamont, J. E., Belton, M. J. S., Ajello, J. M., Holberg, J. B., Atreya, S. K., Donahue, T. M., Moos, H. W., Strobel, D. F., McConnell, J. C., Dalgarno, A., Goody, R., McElroy, M. B., and Takacs, P. Z.

Published
1979

134. Extreme Ultraviolet Observations from Voyager 1 Encounter with Saturn

Author

Broadfoot, A. L., Sandel, B. R., Shemansky, D. E., Holberg, J. B., Smith, G. R., Strobel, D. F., McConnell, J. C., Kumar, S., Hunten, D. M., Atreya, S. K., Donahue, T. M., Moos, H. W., Bertaux, J. L., Blamont, J. E., Pomphrey, R. B., and Linick, S.

Published
1981

135. Ultraviolet Spectrometer Observations of Neptune and Triton

Author

Broadfoot, A. L., Atreya, S. K., Bertaux, J. L., Blamont, J. E., Dessler, A. J., Donahue, T. M., Forrester, W. T., Hall, D. T., Herbert, F., Holberg, J. B., Hunten, D. M., Krasnopolsky, V. A., Linick, S., Lunine, J. I., McConnell, J. C., Moos, H. W., Sandel, B. R., Schneider, N. M., Shemansky, D. E., Smith, G. R., Strobel, D. F., and Yelle, R. V.

Published
1989

136. Ultraviolet Spectrometer Observations of Uranus

Author

Broadfoot, A. L., Herbert, F., Holberg, J. B., Hunten, D. M., Kumar, S., Sandel, B. R., Shemansky, D. E., Smith, G. R., Yelle, R. V., Strobel, D. F., Moos, H. W., Donahue, T. M., Atreya, S. K., Bertaux, J. L., Blamont, J. E., McConnell, J. C., Dessler, A. J., Linick, S., and Springer, R.

Published
1986

138. Simulating the density and thermal structure of the middle atmosphere ([approximately equal to]80-130km) of Mars using the MGCM-MTGCM: A comparison with MEX/SPICAM observations

Author

Mcdunn, T.L., Bougher, S.W., Murphy, J., Smith, M.D., Forget, F., Bertaux, J.-L., and Montmessin, F.

Subjects
Mars (Planet) -- Models, Mars (Planet) -- Thermal properties, Mars (Planet) -- Analysis, Astronomy -- Models, Astronomy -- Thermal properties, Astronomy -- Analysis, Chert -- Models, Chert -- Thermal properties, Astrogeology -- Models, Astrogeology -- Thermal properties, Astrogeology -- Analysis, Altitudes -- Models, Altitudes -- Thermal properties, Altitudes -- Analysis, Atmosphere -- Models, Atmosphere -- Thermal properties, Atmosphere -- Analysis, Earth -- Atmosphere, Earth -- Models, Earth -- Thermal properties, Earth -- Analysis, Astronomy, Earth sciences
Abstract

To link to full-text access for this article, visit this link: http://dx.doi.org/10.1016/j.icarus.2009.06.034 Byline: T.L. McDunn (a), S.W. Bougher (a), J. Murphy (b), M.D. Smith (c), F. Forget (d), J.-L. Bertaux (e), F. Montmessin (e) Keywords: Mars, Atmosphere; Atmosphere, Structure; Aeronomy Abstract: The objective of this work is to advance the understanding of the structure and dynamics of the middle altitude region of the martian atmosphere. While numerous advancements have been made in the level of scientific understanding of Mars's upper and lower atmospheres over the past several decades, insight into the mechanisms of the middle atmosphere has come at a significantly slower pace due to the small number of datasets available for this region. Over the past decade this has begun to change, with renewed interest by NASA and ESA to send spacecraft to Mars. The result of these recent efforts is a growing database for Mars's middle atmosphere, enabling long-awaited and necessary studies characterizing the middle altitude region. Various numerical models of the martian atmosphere can now be validated and constrained using this database. We utilize the Mars Express/Spectroscopy for the Investigation of the Characteristics of the Atmosphere of Mars (MEX/SPICAM) density and temperature datasets to characterize the middle atmosphere as well as validate and constrain the coupled multi-dimensional Mars General Circulation Model-Mars Thermosphere General Circulation Model (MGCM-MTGCM) at middle altitudes in order to explore the underlying physics controlling the structure and dynamics at these levels. The results of this study stress the importance of proper dust prescription within the MGCM-MTGCM for accurately reproducing the density and thermal structure of the middle and upper atmosphere regions on Mars. Simulations conducted with horizontal dust opacities that are consistent with the SPICAM observation period (i.e. Mars Odyssey/THEMIS opacities) yield modeled densities and temperatures that are closer to the observed values than simulations conducted with 'typical' dust conditions (i.e. Mars Global Surveyor/TES opacities). We show that the MGCM-MTGCM closely reproduces the observed densities during low-dust and high-dust scenarios but displays difficulty during the pre-dust-season 'ramp-up' period (L.sub.s [approximately equal to]120-200[degrees]) during MY27. In addition, we show that the MGCM-MTGCM accurately reproduces the temperature profiles below the mesopause, but, the mesopause altitude is too low and its temperature warmer (5-10K) than observations. This may be related to nightside dynamical heating processes that require further refinement. In addition, CO.sub.2 15-[mu]m cooling rates may be too small, which would be consistent with underestimated atomic O abundances. Author Affiliation: (a) Department of Atmospheric, Oceanic, and Space Sciences, University of Michigan, 2455 Hayward St., Ann Arbor, MI 48109, USA (b) Department of Astronomy, New Mexico State University, P. O. Box 30001, MSC 4500, Las Cruces, New Mexico 88003, USA (c) NASA Goddard Space Flight Center, Greenbelt, MD 20071, USA (d) Laboratoire de Meteorologie Dynamique, Institut Pierre-Simon Laplace, Universite Paris 6, Paris, France (e) Service d'Aeronomie, Institut Pierre-Simon Laplace, Verrieres-le-Buisson, France Article History: Received 24 September 2008; Revised 23 June 2009; Accepted 24 June 2009

Published
2010

139. Venus express: Highlights of the nominal mission

Author

Titov, D. V., Svedhem, H., Taylor, F. W., Barabash, S., Bertaux, J. -L., Drossart, P., Formisano, V., Häusler, B., Korablev, O., Markiewicz, W. J., Nevejans, D., Pätzold, M., Piccioni, G., Sauvaud, J. -A., Zhang, T. L., Witasse, O., Gerard, J. -C., Fedorov, A., Sanchez-Lavega, A., Helbert, J., and Hoofs, R.

Published
2009
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140. Solar infrared occultation observations by SPICAM experiment on Mars-Express: Simultaneous measurements of the vertical distributions of H.sub.2O, CO.sub.2 and aerosol

Author

Fedorova, A.A., Korablev, O.I., Bertaux, J.-L., Rodin, A.V., Montmessin, F., Belyaev, D.A., and Reberac, A.

Subjects
Atmospheric physics -- Measurement, Atmospheric physics -- Optical properties, Atmospheric physics -- Analysis, Mars (Planet) -- Measurement, Mars (Planet) -- Optical properties, Mars (Planet) -- Analysis, Clouds -- Measurement, Clouds -- Optical properties, Clouds -- Analysis, Water -- Measurement, Water -- Optical properties, Water -- Analysis, Atmospheric density -- Measurement, Atmospheric density -- Optical properties, Atmospheric density -- Analysis, Altitudes -- Measurement, Altitudes -- Optical properties, Altitudes -- Analysis, Planets -- Atmosphere, Planets -- Measurement, Planets -- Optical properties, Planets -- Analysis, Astronomy, Earth sciences
Abstract

To link to full-text access for this article, visit this link: http://dx.doi.org/10.1016/j.icarus.2008.11.006 Byline: A.A. Fedorova (a), O.I. Korablev (a), J.-L. Bertaux (b)(c), A.V. Rodin (a)(d), F. Montmessin (b)(c), D.A. Belyaev (a), A. Reberac (b)(c) Keywords: Mars; atmosphere; Spectroscopy Abstract: The infrared AOTF spectrometer is a part of the SPICAM experiment onboard the Mars-Express ESA mission. The instrument has a capability of solar occultations and operates in the spectral range of 1-1.7 [mu]m with a spectral resolution of [approximately equal to]3.5 cm.sup.-1. We report results from 24 orbits obtained during MY28 at L.sub.s 130[degrees]-160[degrees], and the latitude range of 40[degrees]-55[degrees] N. For these orbits the atmospheric density from 1.43 [mu]m CO.sub.2 band, water vapor mixing ratio based on 1.38 [mu]m absorption, and aerosol opacities were retrieved simultaneously. The vertical resolution of measurements is better than 3.5 km. Aerosol vertical extinction profiles were obtained at 10 wavelengths in the altitude range from 10 to 60 km. The interpretation using Mie scattering theory with adopted refraction indices of dust and H.sub.2O ice allows to retrieve particle size (r.sub.eff[approximately equal to]0.5-1 [mu]m) and number density ([approximately equal to]1 cm.sup.-3 at 15-30 km) profiles. The haze top is generally below 40 km, except the longitude range of 320[degrees]-50[degrees] E, where high-altitude clouds at 50-60 km were detected. Optical properties of these clouds are compatible with ice particles (effective radius r.sub.eff=0.1-0.3[mu]m, number density N[approximately equal to]10 cm.sup.-3) distributed with variance [nu].sub.eff=0.1-0.2[mu]m. The vertical optical depth of the clouds is below 0.001 at 1 [mu]m. The atmospheric density profiles are retrieved from CO.sub.2 band in the altitude range of 10-90 km, and H.sub.2O mixing ratio is determined at 15-50 km. Unless a supersaturation of the water vapor occurs in the martian atmosphere, the H.sub.2O mixing ratio indicates [approximately equal to]5 K warmer atmosphere at 25-45 km than predicted by models. Author Affiliation: (a) Space Research Institute (IKI), 84/32 Profsoyuznaya, 117997 Moscow, Russia (b) Service d'Aeronomie du CNRS, BP 3, 91371, Verrieres-le-Buisson, France (c) Institut Pierre Simon Laplace, Universite de Versailles-Saint-Quentin, 78 Saint Quentin en Yvelines, France (d) Moscow Institute of Physics and Technology, Institutsky dr. 9, 141700 Dolgoprudnyi, Russia Article History: Received 26 November 2007; Revised 28 July 2008; Accepted 3 November 2008

Published
2009

143. Rosina – Rosetta Orbiter Spectrometer for Ion and Neutral Analysis

Author

Balsiger, H., Altwegg, K., Bochsler, P., Eberhardt, P., Fischer, J., Graf, S., Jäckel, A., Kopp, E., Langer, U., Mildner, M., Müller, J., Riesen, T., Rubin, M., Scherer, S., Wurz, P., Wüthrich, S., Arijs, E., Delanoye, S., Keyser, J. De, Neefs, E., Nevejans, D., Rème, H., Aoustin, C., Mazelle, C., Médale, J.-L., Sauvaud, J. A., Berthelier, J.-J., Bertaux, J.-L., Duvet, L., Illiano, J.-M., Fuselier, S. A., Ghielmetti, A. G., Magoncelli, T., Shelley, E. G., Korth, A., Heerlein, K., Lauche, H., Livi, S., Loose, A., Mall, U., Wilken, B., Gliem, F., Fiethe, B., Gombosi, T. I., Block, B., Carignan, G. R., Fisk, L. A., Waite, J. H., Young, D. T., and Wollnik, H.

Published
2007
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144. OSIRIS – The Scientific Camera System Onboard Rosetta

Author

Keller, H. U., Barbieri, C., Lamy, P., Rickman, H., Rodrigo, R., Wenzel, K.-P., Sierks, H., A’Hearn, M. F., Angrilli, F., Angulo, M., Bailey, M. E., Barthol, P., Barucci, M. A., Bertaux, J.-L., Bianchini, G., Boit, J.-L., Brown, V., Burns, J. A., Büttner, I., Castro, J. M., Cremonese, G., Curdt, W., Deppo, V. Da, Debei, S., Cecco, M. De, Dohlen, K., Fornasier, S., Fulle, M., Germerott, D., Gliem, F., Guizzo, G. P., Hviid, S. F., Ip, W.-H., Jorda, L., Koschny, D., Kramm, J. R., Kührt, E., Küppers, M., Lara, L. M., Llebaria, A., López, A., López-Jimenez, A., López-Moreno, J., Meller, R., Michalik, H., Michelena, M. D., Müller, R., Naletto, G., Origné, A., Parzianello, G., Pertile, M., Quintana, C., Ragazzoni, R., Ramous, P., Reiche, K.-U., Reina, M., Rodríguez, J., Rousset, G., Sabau, L., Sanz, A., Sivan, J.-P., Stöckner, K., Tabero, J., Telljohann, U., Thomas, N., Timon, V., Tomasch, G., Wittrock, T., and Zaccariotto, M.

Published
2007
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147. Venus Express: Scientific goals, instrumentation, and scenario of the mission

Author

Titov, D. V., Svedhem, H., McCoy, D., Lebreton, J. -P., Barabash, S., Bertaux, J. -L., Drossart, P., Formisano, V., Haeusler, B., Korablev, O. I., Markiewicz, W., Neveance, D., Petzold, M., Piccioni, G., Zhang, T. L., Taylor, F. W., Lellouch, E., Koschny, D., Witasse, O., Warhaut, M., Acomazzo, A., Rodrigues-Cannabal, J., Fabrega, J., Schirmann, T., Clochet, A., and Coradini, M.

Published
2006
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150. Venus Express—The first European mission to Venus

Author

Svedhem, H., Titov, D.V., McCoy, D., Lebreton, J.-P., Barabash, S., Bertaux, J.-L., Drossart, P., Formisano, V., Häusler, B., Korablev, O., Markiewicz, W.J., Nevejans, D., Pätzold, M., Piccioni, G., Zhang, T.L., Taylor, F.W., Lellouch, E., Koschny, D., Witasse, O., Eggel, H., Warhaut, M., Accomazzo, A., Rodriguez-Canabal, J., Fabrega, J., Schirmann, T., Clochet, A., and Coradini, M.

Published
2007
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