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1. Water Production Rates from SOHO/SWAN Observations of Comets C/2020 S3 (Erasmus), C/2021 A1 (Leonard) and C/2021 O3 (PanSTARRS)

Author

Combi, M. R., Mäkinen, T., Bertaux, J. -L., Quémerais, E., and Ferron, S.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

In 2021 and 2022 the hydrogen comae of three long period comets, C/2020 S3 (Erasmus), C/2021 A1 (Leonard) and C/2021 O3 (PanSTARRS) were observed with the Solar Wind ANisotropies (SWAN) all-sky hydrogen Lyman-alpha camera on the SOlar and Heliosphere Observer (SOHO) satellite. SWAN obtains nearly daily full-sky images of the hydrogen Lyman-alpha distribution of the interstellar hydrogen as it passes through the solar system yielding information about the solar wind and solar ultraviolet fluxes that eats away at it by ionization and charge exchange. The hydrogen comae of comets, when of sufficient brightness, are also observed. Water production rates have been calculated over time for each of these comets. Of particular interest are comet C/2021 O3 (PanSTARRS) which apparently disintegrated a few days before its perihelion at 0.28 au and C/2021 A1 (Leonard) which also disintegrated beginning about 20 days after its perihelion peak. The behavior of comet C/2020 S3 (Erasmus) was more typical without dramatic fading, but still was asymmetric about perihelion, with a more rapid turn on before perihelion and more extended activity well after perihelion., Comment: 20 pages, 4 Figures, 4 Tables more...

Published
2023
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2. 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., Zorzano, M. P., Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), Main Astronomical Observatory of NAS of Ukraine (MAO), National Academy of Sciences of Ukraine (NASU), National Research Institute for Physical-technical and Radiotechnical Measurements (VNIIFTRI), Scientific Production Enterprise Astron Electronics, Faculty of Physics [MSU, Moscow], Lomonosov Moscow State University (MSU), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Tohoku University [Sendai], Moscow Institute of Physics and Technology [Moscow] (MIPT), Catholic University of America, Vernadsky Institute of Geochemistry and Analytical Chemistry (GEOKHI), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Department of Computer Science [Kiruna], Luleå University of Technology (LUT), Instituto Andaluz de Ciencias de la Tierra (IACT), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Universidad de Granada (UGR), The Open University [Milton Keynes] (OU), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Institute of Astronomy of the Russian Academy of Sciences (INASAN), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Universität Bern [Bern], Facultad de Informática [Madrid], Universidad Complutense de Madrid [Madrid] (UCM), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics [Oxford], University of Oxford [Oxford], Centro de Astrobiologia [Madrid] (CAB), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), PLANETO - LATMOS, Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universidad de Granada (UGR), Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universidad de Granada = University of Granada (UGR), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Universität Bern [Bern] (UNIBE), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), University of Oxford, and Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC) more...

Subjects
Cross-dispersion, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Atmosphere, 520 Astronomy, Mars, Echelle, Fourier-spectrometer, 620 Engineering, High-resolution spectrometer, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph]
Abstract

International audience; The Atmospheric Chemistry Suite (ACS) package is an element of the Russian contribution to the ESA-Roscosmos ExoMars 2016 Trace Gas Orbiter (TGO) mission. ACS consists of three separate infrared spectrometers, sharing common mechanical, electrical, and thermal interfaces. This ensemble of spectrometers has been designed and developed in response to the Trace Gas Orbiter mission objectives that specifically address the requirement of high sensitivity instruments to enable the unambiguous detection of trace gases of potential geophysical or biological interest. For this reason, ACS embarks a set of instruments achieving simultaneously very high accuracy (ppt level), very high resolving power (>10,000) and large spectral coverage (0.7 to 17 μm—the visible to thermal infrared range). The near-infrared (NIR) channel is a versatile spectrometer covering the 0.7–1.6 μm spectral range with a resolving power of ∼20,000. NIR employs the combination of an echelle grating with an AOTF (Acousto-Optical Tunable Filter) as diffraction order selector. This channel will be mainly operated in solar occultation and nadir, and can also perform limb observations. The scientific goals of NIR are the measurements of water vapor, aerosols, and dayside or night side airglows. The mid-infrared (MIR) channel is a cross-dispersion echelle instrument dedicated to solar occultation measurements in the 2.2–4.4 μm range. MIR achieves a resolving power of >50,000. It has been designed to accomplish the most sensitive measurements ever of the trace gases present in the Martian atmosphere. The thermal-infrared channel (TIRVIM) is a 2-inch double pendulum Fourier-transform spectrometer encompassing the spectral range of 1.7–17 μm with apodized resolution varying from 0.2 to 1.3 cm−1. TIRVIM is primarily dedicated to profiling temperature from the surface up to ∼60 km and to monitor aerosol abundance in nadir. TIRVIM also has a limb and solar occultation capability. The technical concept of the instrument, its accommodation on the spacecraft, the optical designs as well as some of the calibrations, and the expected performances for its three channels are described. more...

Published
2018
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3. The Atmospheric Chemistry Suite (ACS) of Three Spectrometers for the ExoMars 2016 Trace Gas Orbiter

Author

Korablev, O., Montmessin, Franck, Trokhimovskiy, A., Fedorova, A.A., Shakun, A.V., Grigoriev, A.V., Moshkin, B.E., Ignatiev, N.I., Forget, F., Lefevre, F., Anufreychik, A., Dzuban, I., Ivanov, Y.S., Kalinnikov, Y.K., Kozlova, T. O., Kungurov, A., Markov, V., Martynovich, F., Mazlov, I., Merzlyakov, D., Moiseev, P.P., Nikolskiy, Y., Patrakeev, A., Patsaev, D., Santos-Skripo, A., Sazonov, O., Semena, N., Shashkin, V., Sidorov, A., Stepanov, A.V., Stupin, I., Timonin, D., Titov, A.Y., Viktorov, A., Zharkov, A., Alteri, F., Arnold, G., Belyaev, D.A., Bertaux, J.-L., Betsis, D.S., Duxbury, N., Encrenaz, T., Fouchet, T., Gerard, J.-C., Grassi, D., Guerlet, S., Hargtogh, P., Kasaba, Y., Khatuntsev, I., Krasnopolsky, V.A., Kuzmin, R.O., Lellouch, E., Lopez-Valverde, M.A., Luginin, M., Määttänen, A., Marcq, M., 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., Zazova, L.V., Zelenyi, L.M., Zorzano, M.P., Russian Science Foundation, Ministerio de Economía y Competitividad (España), Svedhem, H., and Russel, C.T. more...

Subjects
Leitungsbereich PF, Mars · Atmosphere · High-resolution spectrometer · Fourier-spectrometer ·Echelle · Cross-dispersion
Abstract

The Atmospheric Chemistry Suite (ACS) package is an element of the Russian contribution to the ESA-Roscosmos ExoMars 2016 Trace Gas Orbiter (TGO) mission. ACS consists of three separate infrared spectrometers, sharing common mechanical, electrical, and thermal interfaces. This ensemble of spectrometers has been designed and developed in response to the Trace Gas Orbiter mission objectives that specifically address the requirement of high sensitivity instruments to enable the unambiguous detection of trace gases of potential geophysical or biological interest. For this reason, ACS embarks a set of instruments achieving simultaneously very high accuracy (ppt level), very high resolving power (>10,000) and large spectral coverage (0.7 to 17 μm—the visible to thermal infrared range). The near-infrared (NIR) channel is a versatile spectrometer covering the 0.7–1.6 μm spectral range with a resolving power of ∼20,000. NIR employs the combination of an echelle grating with an AOTF (Acousto-Optical Tunable Filter) as diffraction order selector. This channel will be mainly operated in solar occultation and nadir, and can also perform limb observations. The scientific goals of NIR are the measurements of water vapor, aerosols, and dayside or night side airglows. The mid-infrared (MIR) channel is a cross-dispersion echelle instrument dedicated to solar occultation measurements in the 2.2–4.4 μm range. MIR achieves a resolving power of >50,000. It has been designed to accomplish the most sensitive measurements ever of the trace gases present in the Martian atmosphere. The thermal-infrared channel (TIRVIM) is a 2-inch double pendulum Fourier-transform spectrometer encompassing the spectral range of 1.7–17 μm with apodized resolution varying from 0.2 to 1.3 cm. TIRVIM is primarily dedicated to profiling temperature from the surface up to ∼60 km and to monitor aerosol abundance in nadir. TIRVIM also has a limb and solar occultation capability. The technical concept of the instrument, its accommodation on the spacecraft, the optical designs as well as some of the calibrations, and the expected performances for its three channels are described., ExoMars is a space mission by ESA and Roscosmos. The development and fabrication of ACS was funded by Roscosmos with contributions from LATMOS (France) funded by CNES. Science operations are funded by Roscosmos and ESA. AAF, NII, DAB, JLB, DSB, ML acknowledge the grant #14.W03.31.0017 of Ministry for Education and Science of Russian Federation for science support of the ACS experiment. AT, AVS, and BEM acknowledge support from Russian Science Foundation (grant RSF 16-12-10453), whichenabledassessmentofmeasurementcharacteristicsoftheinstrument andtheassociated modeling. LMZ acknowledges RSF funding (grant RSF 16-42-01103). Other authors affiliated with IKI acknowledge FANO, contracts 0120.06 02993 (0028-2014-0004) and 0120.03 03422 (0028-2014-0007). MRP acknowledges funding under the UK Space Agency grant ST/I003061/1 and ST/P001262/1. LV acknowledges the support of Ministerio de Economía y Competitividad of Spain under project ESP2016-79135-R. We are grateful to Richard Zurek and an anonymous reviewer for useful comments and suggestions, which helped improving this paper. We thank Sylvain Cnudde, Evgeny Germanyuk, and Ekaterina Korableva for help in rendering graphics. We also express our sincere gratitude to the space agencies, countries, companies, and project teams who made the ExoMars 2016 mission possible. more...

Published
2017

4. Physical properties of craters on asteroid (21) Lutetia

Author

Jean-Baptiste, Vincent, Sébastien, Besse, Marchi, Simone, Holger, Sierks, Massironi, Matteo, A’Hearn, The OSIRIS Team (M., Angrilli, F., Barbieri, C., Barucci, A., Bertaux, J. -L., Cremonese, G., Da Deppo, V., Davidsson, B., Debei, S., De Cecco, M., Fornasier, S., Fulle, M., Groussin, O., Gutierrez, P., Hviid, S. F., W. -H., Ip, Jorda, L., Keller, H. U., Koschny, D., Knollenberg, J., Kramm, J. R., Kuehrt, E., Lamy, P., Lara, L. M., Lazzarin, M., Lopez-Moreno, J. J., Marzari, F., Michalik, H., Naletto, G., Rickman, H., Rodrigo, R., Sabau, L., Thomas, N., and Wenzel), K. -P. more...

Subjects
Spacecraft, business.industry, Asteroid, Astronomy and Astrophysics, Geophysics, Lutetia, Regolith, Astrobiology, Impact crater, Craters morphology, Space and Planetary Science, Ejecta blanket, Ejecta, Scale (map), business, Event (particle physics), Geology
Abstract

This paper presents an analysis of the physical properties of craters on asteroid (21) Lutetia, derived from images acquired by OSIRIS, the high-resolution cameras onboard ESA's spacecraft Rosetta. Crater morphology on (21) Lutetia fits very well with the general picture of what was known for previously visited small bodies, with a typical depth to diameter ratio of 0.12. We discuss here the distribution of this parameter all across the surface, but also region by region, and see how it can vary from one location to another and help to distinguish between different geological units. In a later section of the paper we study in more details Beatica region where a deep ejecta blanket filled most of the craters, and estimate the thickness profile of this ejecta based on our analysis of the d / D . We find a good agreement with existing scaling laws, and use this to constrain the scale of the original event that reshaped the surface around the North pole of the asteroid. Finally, we report on the observations of avalanches in several crater flanks, and the presence of many asymmetrical craters with flow-like features, and discuss the evidence for widespread fine material all over the surface. more...

Published
2012
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5. Are fractured cliffs the source of cometary dust jets ? Insights from OSIRIS/Rosetta at 67P

Author

Vincent, J. -B., Oklay, N., Pajola, M., Höfner, S., Sierks, H., Hu, X., Barbieri, C., Lamy, P. L., Rodrigo, R., Koschny, D., Rickman, H., Keller, H. U., A'Hearn, M. F., Barucci, M. A., Bertaux, J. -L., Bertini, I., Besse, S., Bodewits, D., Cremonese, G., Da Deppo, V., Davidsson, B., Debei, S., De Cecco, M., El-Maarry, M. R., Fornasier, S., Fulle, M., Groussin, O., Gutiérrez, P. J., Gutiérrez-Marquez, P., Güttler, C., Hofmann, M., Hviid, S. F., Ip, W. -H., Jorda, L., Knollenberg, J., Kovacs, G., Kramm, J. -R., Kührt, E., Küppers, M., Lara, L. M., Lazzarin, M., Lin, Z. -Y., Moreno, J. J. Lopez, Lowry, S., Marzari, F., Massironi, M., Moreno, F., Mottola, S., Naletto, G., Preusker, F., Scholten, F., Shi, X., Thomas, N., Toth, I., and Tubiana, C. more...

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

Dust jets, i.e. fuzzy collimated streams of cometary material arising from the nucleus, have been observed in-situ on all comets since the Giotto mission flew by comet 1P/Halley in 1986. Yet their formation mechanism remains unknown. Several solutions have been proposed, from localized physical mechanisms on the surface/sub-surface (see review in Belton (2010)) to purely dynamical processes involving the focusing of gas flows by the local topography (Crifo et al. 2002). While the latter seems to be responsible for the larger features, high resolution imagery has shown that broad streams are composed of many smaller features (a few meters wide) that connect directly to the nucleus surface. We monitored these jets at high resolution and over several months to understand what are the physical processes driving their formation, and how this affects the surface. Using many images of the same areas with different viewing angles, we performed a 3-dimensional reconstruction of collimated jets, and linked them precisely to their sources on the nucleus. Results.We show here observational evidence that the Northern hemisphere jets of comet 67P arise from areas with sharp topographic changes and describe the physical processes involved. We propose a model in which active cliffs are the main source of jet-like features, and therefore the regions eroding the fastest on comets. We suggest that this is a common mechanism taking place on all comets., Comment: Accepted by Astronomy & Astrophysics on 4 December 2015 more...

Published
2015
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7. Hydrocode simulations of the largest crater on asteroid Lutetia

Author

Cremonese, G., Martellato, E., Marzari, F., Kuhrt, E, Scholten, F., Preusker, F., Wünnemann, K., Borin, P., Massironi, M., Simioni, E, Ip, W., A’Hearn, and the OSIRIS Team (M., Angrilli, F., Barbieri, C., Barucci, A., Bertaux, J. -L., Da Deppo, V., Davidsson, B., Debei, S., Dececco, M., Fornasier, S., Fulle, M., Groussin, O., Gutierrez, P., Hviid, S. F., Jorda, L., Keller, H. U., Koschny, D., Knollemberg, J., Kramm, J. R., Lamy, P., Lara, L. M., Lazzarin, M., Lopez-Moreno, J. J., Michalik, H., Naletto, G., Rickman, H., Rodrigo, R., Sabau, L., Sierks, H., Thomas, N., and Wenzel), K. -P. more...

Subjects
North pole, Astronomy, Numerical modeling, Astronomy and Astrophysics, Geodesy, Lutetia, Asteroids, Impact crater, Space and Planetary Science, Asteroid, Impacts, Rosetta, Impact structure, Digital elevation model, Geology, Cratering
Abstract

The flyby of the Main Belt asteroid Lutetia by the Rosetta spacecraft allows the camera OSIRIS to obtain very good images of about half of the body at the maximum resolution of 60 m per pixel. From the images and radio-science experiment, a density of about (3.4±0.3) g/cm3 has been inferred for the asteroid. Many impact craters have been observed on the surface of Lutetia and the largest, named Massilia, has a diameter of about 55 km. Relative to the size of Lutetia (the longest axis is approximately 126 km) the crater represents one of the dominating features on its surface. Whether or not the impact that formed Massilia affected the entire asteroid can be only evaluated via numerical modeling, with hydrocodes, of the impact process. The results of a suite of iSALE simulations are compared with the crater profile derived from the Digital Terrain Model of the observed surface. The best match to the DTM of the crater with hydrocode simulations has allowed to determine a value of 7.5 km for the impactor diameter, which suggests a primordial origin of Lutetia due to the low probability of such an impact event. A second interesting impact structure has been identified nearby Massilia within the North Pole Crater Cluster. The crater has a diameter of 24 km and it lies over a larger crater of the North Pole Crater Cluster. This is strongly suggestive of a very young structure on Lutetia. The numerical simulations of this feature constrain the impactor to be 3.8 km in diameter, assuming the same material properties for target and impactor as in the model of the formation of Massilia. more...

Published
2012

8. The HARPS search for southern extra-solar planets XXXIV. Occurrence, mass distribution and orbital properties of super-Earths and Neptune-mass planets

Author

Mayor, M., Marmier, M., Lovis, C., Udry, S., Ségransan, D., Pepe, F., Benz, W., Bertaux, J. -L., Bouchy, F., Dumusque, X., Curto, G. Lo, Mordasini, C., Queloz, D., and Santos, N. C.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract

We report on the results of an 8-year survey carried out at the La Silla Observatory with the HARPS spectrograph to detect and characterize planets in the super-Earth and Neptune mass regime. The size of our star sample and the precision achieved with HARPS have allowed the detection of a sufficiently large number of low-mass planets to study the statistical properties of their orbital elements, the correlation of the host-star metallicity with the planet masses, as well as the occurrence rate of planetary systems around solar-type stars. A robust estimate of the frequency of systems shows that more than 50% of solar-type stars harbor at least one planet of any mass and with period up to 100 days. Different properties are observed for the population of planets less massive than about 30M-Earth compared to the population of gaseous giant planets. The mass distribution of Super-Earths and Neptune-mass planets (SEN) is strongly increasing between 30 and 15M-Earth. The SEN occurence rate does not exhibit a preference for metal rich stars. Most of the SEN planets belong to multi-planetary systems. The orbital eccentricities of the SEN planets seems limited to 0.45. At the opposite, the occurence rate of gaseous giant planets is growing with the logarithm of the period, and is strongly increasing with the host-star metallicity. About 14% of solar-type stars have a planetary companion more massive than 50M-Earth? on an orbit with a period shorter than 10 years. Orbital eccentricities of giant planets are observed up to 0.9 and beyond. The precision of HARPS-type spectrographs opens the possibility to detect planets in the habitable zone of solar-type stars. Identification of a significant number of super-Earths orbiting solar-type of the Sun vicinity is achieved by Doppler spectroscopy. 37 newly discovered planets are announced in the Appendix of this paper, among which 15 Super-Earths., Comment: 23 pages, 18 figures, and many tables, submitted to A&A more...

Published
2011
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9. E-Type Asteroid (2867) Steins as Imaged by OSIRIS on Board Rosetta

Author

Keller, H. U, Barbieri, Cesare, Koschny, D, Lamy, P, Rickman, H, Rodrigo, R, Sierks, H, Ahearn, M. F, Angrilli, F, Barucci, M. A, Bertaux, J. L, Cremonese, G, Deppo, Da, Davidsson, V, B, Cecco, De, Debei, Stefano, Fornasier, S, Fulle, S, Groussin, M, Gutierrez, O, P. J, Hviid, S. F, Ip, W. H, Jorda, Knollenberg, L, Kramm, J, J. R, Kãœhrt, Kãœppers, E, Lara, M, L. M., Lazzarin, Monica, Moreno, M, Lopez, J., Marzari, Francesco, Michalik, H, Naletto, Giampiero, Sabau, L, Thomas, N, Wenzel, K. P, Bertini, Ivano, Besse, S, Ferri, F, Kaasalainen, M, Lowry, S, Marchi, S, Mottola, S, Sabolo, W, Schrã–der, S. E, Spjuth, S, Vernazza, P., Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Dipartimento di Astronomia [Padova], Università degli Studi di Padova = University of Padua (Unipd), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), Laboratoire d'Astrophysique de Marseille (LAM), 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), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, 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), 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), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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)-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), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Department of Physics and Astronomy [Uppsala], Uppsala University, Scuola Internazionale Superiore di Studi Avanzati / International School for Advanced Studies (SISSA / ISAS), National Central University [Taiwan] (NCU), German Aerospace Center (DLR), European Space Astronomy Centre (ESAC), Institute of Computer and Network Engineering [Braunschweig] (IDA), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Instituto Nacional de Técnica Aeroespacial (INTA), Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE), Tampere University of Technology [Tampere] (TUT), University of Kent [Canterbury], Max-Planck-Institut für Sonnensystemforschung (MPS), Universita degli Studi di Padova, European Space Agency (ESA), and Universität Bern [Bern] more...

Subjects
Asteroid (2867), 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Comet, CRATERS, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], engineering.material, 01 natural sciences, Astrobiology, collisional history, Impact crater, belt, 0103 physical sciences, Rosetta, OSIRIS, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Multidisciplinary, biology, Rubble, Astronomy, Asteroid (2867) Steins, biology.organism_classification, On board, Asteroid, ASTEROID-2867-STEINS, engineering, Asteroid belt, Board Rosetta, Solid rock, Osiris
Abstract

The European Space Agency’s Rosetta mission encountered the main-belt asteroid (2867) Steins while on its way to rendezvous with comet 67P/Churyumov-Gerasimenko. Images taken with the OSIRIS (optical, spectroscopic, and infrared remote imaging system) cameras on board Rosetta show that Steins is an oblate body with an effective spherical diameter of 5.3 kilometers. Its surface does not show color variations. The morphology of Steins is dominated by linear faults and a large 2.1-kilometer-diameter crater near its south pole. Crater counts reveal a distinct lack of small craters. Steins is not solid rock but a rubble pile and has a conical appearance that is probably the result of reshaping due to Yarkovsky-O’Keefe-Radzievskii-Paddack (YORP) spin-up. The OSIRIS images constitute direct evidence for the YORP effect on a main-belt asteroid. more...

Published
2010
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10. HD45364, a pair of planets in a 3:2 mean motion resonance

Author

Correia, A. C. M., Udry, S., Mayor, M., Benz, W., Bertaux, J. -L., Bouchy, F., Laskar, J., Lovis, C., Mordasini, C., Pepe, F., and Queloz, D.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract

Precise radial-velocity measurements with the HARPS spectrograph reveal the presence of two planets orbiting the solar-type star HD45364. The companion masses are 0.187 Mjup and 0.658 Mjup, with semi-major axes of 0.681 AU and 0.897 AU, and eccentricities of 0.168 and 0.097, respectively. A dynamical analysis of the system further shows a 3:2 mean motion resonance between the two planets, which prevents close encounters and ensures the stability of the system over 5 Gyr. This is the first time that such a resonant configuration has been observed for extra-solar planets, although there is an analogue in our Solar System formed by Neptune and Pluto. This singular planetary system may provide important constraints on planetary formation and migration scenarios., Comment: 6 pages, 6 figures more...

Published
2009
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11. The HARPS search for southern extra-solar planets. XIII. A planetary system with 3 Super-Earths (4.2, 6.9, & 9.2 Earth masses)

Author

Mayor, M., Udry, S., Lovis, C., Pepe, F., Queloz, D., Benz, W., Bertaux, J. -L., Bouchy, F., Mordasini, C., and Segransan, D.

Subjects
Astrophysics (astro-ph), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

This paper reports on the detection of a planetary system with three Super-Earths orbiting HD40307. HD40307 is a K2V metal-deficient star at a distance of only 13 parsec, part of the HARPS GTO high-precision planet-search programme. The three planets on circular orbits have very low minimum masses of respectively 4.2, 6.9 and 9.2 Earth masses and periods of 4.3, 9.6 and 20.5 days. The planet with the shortest period is the lightest planet detected to-date orbiting a main sequence star. The detection of the correspondingly low amplitudes of the induced radial-velocity variations is completely secured by the 135 very high-quality HARPS observations illustrated by the radial-velocity residuals around the 3-Keplerian solution of only 0.85 m/s. Activity and bisector indicators exclude any significant perturbations of stellar intrinsic origin, which supports the planetary interpretation. Contrary to most planet-host stars, HD40307 has a marked sub-solar metallicity ([Fe/H]=-0.31), further supporting the already raised possibility that the occurrence of very light planets might show a different dependence on host star's metallicity compared to the population of gas giant planets. In addition to the 3 planets close to the central star, a small drift of the radial-velocity residuals reveals the presence of another companion in the system the nature of which is still unknown., Submitted to A&A (6 pages) more...

Published
2008
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12. Evidence for a Large Dust/Ice Ratio in the Nucleus of Comet 9P/Tempel 1

Author

Küppers, Michael, Bertini, Ivano, Fornasier, Sonia, Gutierrez, Pedro J., Hviid, Stubbe F., Jorda, Laurent, Keller, Horst Uwe, Knollenberg, Jörg, Koschny, Detlef, Kramm, Rainer, Lara, Luisa-Maria, Sierks, Holger, Thomas, Nicolas, Barbieri, Cesare, Lamy, Philippe, Rickman, Hans, Rodrigo, Rafael, A'Hearn, M. F., Angrilli, F., Bailey, M. E., Barthol, P., Barucci, M. A., Bertaux, J.-L., Burns, J. A., Cremonese, G., Curdt, W., De Cecco, M., Debei, S., Fulle, M., Gliem, F., Ip, W.-H., Kührt, E., Llebaria, A., Lopez Moreno, J. J., Marzari, F., Naletto, G., Sabau, L., Sanz Andrés, A., Sivan, J. P., Tondello, G., and Wenzel, K.-P. more...

Subjects
Deep Impact, dust/ice ratio, comets
Published
2005

13. A large dust/ice ratio in the nucleus of comet 9P/Tempel 1

Author

Kueppers, M., Bertini, Ivano, Fornasier, Sonia, Gutierrez, P. J., Hviid, S. F., Jorda, L., Keller, H. U., Knollenberg, J., Koschny, D., Kramm, R., Lara, L. M., Sierks, H., Thomas, N., Barbieri, Cesare, Lamy, P., Rickman, H., Rodrigo, R., A'Hearn, M. F., Angrilli, F., Bailey, M. E., Barthol, P., Barucci, M. A., Bertaux, J. L., Burns, J. A., Cremonese, G., Curdt, W., DE CECCO, M., Debei, Stefano, Fulle, M., Gliem, F., W. H., Ip, Khrt, E., Llebaria, A., LOPEZ MORENO, J. J., Marzari, Francesco, Naletto, Giampiero, Sabau, L., SANZ ANDRS, A., Sivan, J. P., Tondello, Giuseppe, Wenzel, K. P., Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Dipartimento di Astronomia [Padova], Universita degli Studi di Padova, 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), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Uppsala Astronomical 0bservatory (UAO), Uppsala University, 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), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Università degli Studi di Padova = University of Padua (Unipd), and 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) more...

Subjects
[SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, Multidisciplinary, 010504 meteorology & atmospheric sciences, Meteoroid, Comet tail, Comet dust, Comet, comete, Planetary system, 01 natural sciences, Astrobiology, Impact crater, Rosetta, OSIRIS, 13. Climate action, Comet nucleus, 0103 physical sciences, 010303 astronomy & astrophysics, Water vapor, Geology, 0105 earth and related environmental sciences
Abstract

NASA's Deep Impact spacecraft met its intended fate on 4 July this year when it collided with Comet Tempel 1 at a relative velocity of over 36,000 km per hour. Telescopes all around the world and beyond it were trained on the event in order to glean information about the internal structure of a comet. Results from OSIRIS cameras on ESA's Rosetta spacecraft provided continuous coverage from 3 days before to 10 days after the impact. The impact created a crater 60 metres in diameter and the nature of the debris points to the comet as an ‘icy dustball’ rather than the more familiar concept of a ‘dirty snowball’. Comets spend most of their life in a low-temperature environment far from the Sun. They are therefore relatively unprocessed and maintain information about the formation conditions of the planetary system, but the structure and composition of their nuclei are poorly understood. Although in situ1 and remote2 measurements have derived the global properties of some cometary nuclei, little is known about their interiors. The Deep Impact mission3 shot a projectile into comet 9P/Tempel 1 in order to investigate its interior. Here we report the water vapour content (1.5 × 1032 water molecules or 4.5 × 106 kg) and the cross-section of the dust (330 km2 assuming an albedo of 0.1) created by the impact. The corresponding dust/ice mass ratio is probably larger than one, suggesting that comets are ‘icy dirtballs’ rather than ‘dirty snowballs’ as commonly believed4. High dust velocities (between 110 m s-1 and 300 m s-1) imply acceleration in the comet's coma, probably by water molecules sublimated by solar radiation. We did not find evidence of enhanced activity of 9P/Tempel 1 in the days after the impact, suggesting that in general impacts of meteoroids are not the cause of cometary outbursts. more...

Published
2005
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14. The Netlander Panoramic Camera

Author

Jaumann, R., Langevin, Y., Hauber, E., Oberst, J., Grothues, H.-G., Hoffmann, H., Soufflot, A., Bertaux, J.-L., Dimarellis, E., Mottola, S., Bibring, J.-P., Neukum, G., Albertz, J., Masson, P., Pinet, P., Lamy, P., and Formisano, V. more...

Published
2000

17. GOMOS O3, NO2, and NO3 observations in 2002-2008

Author

Erkki Kyrölä, Tamminen, J., Sofieva, V., Bertaux, J. L., Hauchecorne, A., Dalaudier, F., Fussen, D., Vanhellemont, F., Fanton D Andon, O., Barrot, G., Guirlet, M., Fehr, T., Saavedra Miguel, L., Finnish Meteorological Institute (FMI), STRATO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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)-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), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Analytic and Computational Research, Inc. - Earth Sciences (ACRI-ST), European Space Research Institute (ESRIN), European Space Agency (ESA), and Agence Spatiale Européenne = European Space Agency (ESA) more...

Subjects
lcsh:Chemistry, [PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], lcsh:QD1-999, lcsh:Physics, lcsh:QC1-999
Abstract

International audience; The Global Ozone Monitoring by Occultation of Stars (GOMOS) instrument onboard the European Space Agency's ENVISAT satellite measures ozone, NO2, NO3, H2O, O2, and aerosols using the stellar occultation method. Global coverage, good vertical resolution and the self-calibrating measurement method make GOMOS observations a promising data set for building various climatologies and time series. In this paper we present GOMOS nighttime measurements of ozone, NO2, and NO3 during six years 2002-2008. Using zonal averages we show the time evolution of the vertical profiles as a function of latitude. In order to get continuous coverage in time we restrict the latitudinal region to 50° S-50° N. Time development is analysed by fitting constant, annual and semi-annual terms as well as solar and QBO proxies to the daily time series. Ozone data cover the stratosphere, mesosphere and lower thermosphere (MLT). NO2 and NO3 data cover the stratosphere. In addition to detailed analysis of profiles we derive total column distributions using the fitted time series. The time-independent constant term is determined with a good accuracy (better than 1%) for all the three gases. The median retrieval accuracy for the annual and semi-annual term varies in the range 5-20%. For ozone the annual terms dominate in the stratosphere giving early winter ozone maxima at mid-latitudes. Above the ozone layer the annual terms change the phase which results in ozone summer maximum up to 80 km. In the MLT the annual terms dominate up to 80 km where the semiannual terms start to grow. In the equatorial MLT the semi-annual terms dominate the temporal evolution whereas in the mid-latitude MLT annual and semi-annual terms compete evenly. In the equatorial stratosphere the QBO dominates the time development but the solar term is too weak to be determined. In the MLT above 85 km the solar term grows significantly and ozone has 15-20% dependence on the solar cycle. For NO2 below 32 km the annual summer maxima dominates at mid-latitudes whereas in the equatorial region a strong QBO prevails. In northern mid-latitudes a strong solar term appears in the upper stratosphere. For NO3 the annual variation dominates giving rise to summer maxima. The NO3 distribution is controlled by temperature and ozone. more...

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18. Spicam: Spectroscopy for the investigation of the characteristics of the atmosphere of Mars

Author

Bertaux, J. -L, Korablev, O., Fonteyn, D., Perrier, S., Fedorova, A., Montmessin, F., Leblanc, F., Lebonnois, S., Lefèvre, F., Quémerais, E., pascal RANNOU, Chaurray, J. Y., Forget, F., Sandel, B., Stern, A., Müller, C., Dimarellis, E., Dubois, J. P., Guibert, S., Souchon, G., Leclère, M., Semelin, F., Reberac, A., Barthelemy, M., Lebrun, J. C., Taulemesse, C., Ransbeeck, E., Gondet, B., Kiselev, A., Rodin, A., Stepanov, A., Kalinnikov, Yu, Grigoriev, A., Hauchecorne, A., Cabane, M., Chassefière, E., Cernogora, G., Levasseur-Regourd, A. C., Maziere, M., Neefs, E., Simon, P. C., Fussen, D., Nevejans, D., Arijs, E., Hourdin, F., Talagrand, O., Witasse, O., Kyrölä, E., and Tamminen, J. more...

20. The High-Resolution Fiber-Fed Echelle Spectrograph for the SAO RAS 6-m Telescope: First Spectra

Author

Valyavin, G. G., Musaev, F. A., Perkov, A. V., Bychkov, V. D., Yushkin, M. V., Galazutdinov, G. A., Drabek, S. V., Shergin, V. S., Sazonenko, D. A., Kukushkin, D. E., Bakholdin, A. V., Bertaux, J. -L, Tavrov, A. V., Oleg Korablev, Starkov, A. A., Arkhipova, L. N., Larionov, S., Semenko, E. A., Burlakova, T. E., Kravchenko, V. M., Kudryavtsev, D. O., Pritychenko, A. M., Kryukov, P. G., Semjonov, S. L., Valeev, A. F., Romanyuk, I. I., and Fabrika, S. N. more...

21. GOMOS validation

Author

Kyrölä, E., Tamminen, J., Viktoria Sofieva, Hassinen, S., Leppelmeier, G. W., Bertaux, J. L., Hauchecorne, A., Dalaudier, F., Cot, C., Fanton D Andon, O., Barrot, G., Mangin, A., Guirlet, M., Theodore, B., Koopman, R., Fraisse, R., Fussen, D., Vanhellemont, F., Finnish Meteorological Institute (FMI), 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), Analytic and Computational Research, Inc. - Earth Sciences (ACRI-ST), European Space Research Institute (ESRIN), Agence Spatiale Européenne = European Space Agency (ESA), Astrium [Toulouse], EADS - European Aeronautic Defense and Space, Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), and IEEE more...

Subjects
[PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph]
Abstract

International audience; GOMOS (Global Ozone Monitoring by Occultation of Stars) on Envisat measures ozone, NO/sub 2/, NO/sub 3/, H/sub 2/O, aerosols, neutral air density, and temperature in the stratosphere and mesosphere by detecting the absorption of starlight in UV, visible and infrared wavelengths. During bright limb conditions, GOMOS also observes scattered solar radiation. GOMOS delivers ozone concentration profiles at altitudes 15-100 km with a vertical resolution of about 1.5 km and with a global coverage. As a self-calibrating method, stellar occultation measurements provide a basis for a long-term monitoring of ozone profiles. We present results achieved during the first year of the GOMOS validation program. The validation is based on comparisons with lidars, ozone sondes, balloon borne instruments, other satellites as well as with climatological and meteorological data. more...

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23. Gomos overview

Author

Kyrölä, E., Tamminen, J., Sofieva, V., Bertaux, J. L., Alain Hauchecorne, Dalaudier, F., Fussen, D., Vanhellemont, F., D Andon, O. F., Barrot, G., Mangin, A., Guirlet, M., Saavedra, L., Snoeij, P., Fehr, T., Meijer, Y., and Fraisse, R. more...

26. OSIRIS observations of metre-size bright exposures of H2O ice at the surface of comet 67P/C-G

Author

Pommerol, A., Fornasier, S., Thomas, N., El-Maarry, M. R., Pajola, M., Groussin, O., Auger, A. -T, Oklay, N., Feller, C., Davidsson, B., Gracia, A., Jost, B., Raphael Marschall, Poch, O., Barucci, M. A., Bertaux, J. L., La Forgia, F., Keller, H. U., Kührt, E., Lowry, S. C., ITA, USA, GBR, FRA, and DEU more...

Abstract

Since the beginning of Rosetta's orbital observations, over a hundred small bright spots have been identified in images returned by its OSIRIS NAC camera, in all types of morphological regions on the nucleus. This abstract focuses on such analysis. more...