16 results on '"Brown, Robert"'
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2. The Spectral Nature of Titan's Major Geomorphological Units
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Solomonidou, A., Coustenis, A., Lopes, R.M.C., Malaska, M. J., Rodriguez, S., Altobelli, N., Drossart, P., Elachi, Charles, Schmitt, B., Janssen, Michael A., Wall, S., Sotin, C., Lawrence, K.J., Radebaugh, J., Stephan, Katrin, Brown, Robert H., LeMouelic, Stephane, Le Gall, Alice, Witasse, Olivier, and Matsoukas, C.
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Planetengeologie ,VIMS ,Cassini ,Titan - Published
- 2018
3. Titan's Major Geomorphological Units: Their Spectral and Morphological Nature
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Solomonidou, A., Coustenis, A., Drossart, P., Brown, Robert H., Stephan, Katrin, Altobelli, N., Sotin, C., Lawrence, K.J., Le Mouelic, S., Rodriguez, S., Schmitt, B., Le Gall, Alice, Elachi, Charles, Lopes, R.M.C., Witasse, Olivier, Radebaugh, J., Wall, S., Malaska, M. J., Janssen, M., and Matsoukas, C.
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Planetengeologie ,VIMS ,Cassini ,Titan - Published
- 2018
4. Transient Broad Specular Reflections from Titan’s North Pole
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Dhingra, Rajani, Barnes, Jason W., Brown, Robert H., Buratti, B.J., Sotin, C., Nicholson, P. D., Baines, K. H., Clark, R. N., Soderblom, Jason M., Jaumann, R., Rodriguez, Sebastien, and Mouélic, S. Le
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Planetengeologie ,Titan - Abstract
Transient Broad Specular Reflections from Titan’s North Pole
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- 2017
5. Constraints on the nature of various Titan Geomorphological Units with Cassini/VIMS and SAR
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Solomonidou, Anezina, Coustenis, Athena, Lopes, Rosaly M. C., Rodriguez, Sébastien, Schmitt, Bernard, Philippe, Sylvain, Malaska, Michael, Lawrence, Kenneth J., Janssen, Michael A., Le Gall, Alice, Jaumann, Ralf, Sohl, Frank, Stephan, Katrin, Drossart, Pierre, Brown, Robert H., Maltagliati, Luca, Bratsolis, Emmanuel, Matsoukas, Christos, Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), ESTER - 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), IMPEC - LATMOS, DLR Institute of Planetary Research, German Aerospace Center (DLR), Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), PLANETO - LATMOS, NASA-California Institute of Technology (CALTECH), and Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112))
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[SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere ,Planetengeologie ,Planetenphysik ,[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP] ,Titan - Abstract
International audience; We investigate the lower atmosphere of Titan from Visual and Infrared Mapping Spectrometer (VIMS) spectro-imaging data by use of a recently updated radiative transfer code in the near-IR range and RADAR/SAR data for the distinction of geomorphological units. We focus here on the geological major units identified in [1;2] and [3]: mountains, plains, labyrinths, dune fields, and possible cryovolcanic and/or evaporitic features (the latter two are albedo features, [4;5;6]). We infer surface properties (like absolute surface albedo and morphology) and atmospheric contributions, in particular the haze content. We find that the Huygens landing site and the candidate evaporitic regions pair compositionally with the variable plains, thus indicating that units of significant geomorphological differences seem to consist of very similar materials. Similarly for the labyrinth terrains and the undifferentiated plains. On the contrary, many regions from the same geomorphological unit show compositional variations depending on location (i.e. undifferentiated plains). These differences provide implications on the endogenic or exogenic origin of the various units. In previous studies we showed that the processes most likely linked to the formation of the various geomorphological units are aeolian, fluvial, sedimentary, and lacustrine, in addition to the deposition of organics through the atmosphere. Currently, we are working on deriving information on the chemical composition of the aforementioned regions from the extracted surface albedos using an extensive library of ices and tholins [e.g. 7]. This will shed light on the potential formation processes (Solomonidou et al. in prep.). Preliminary results on the chemical composition of the regions that have shown temporal changes (i.e. Tui Regio and Sotra Patera; [6]) are also presented.References: [1] Lopes, R.M.C., et al.: Icarus, 205, 540-558, 2010; [2] Lopes, R.M.C., et al.: Icarus, 270, 162-182, 2016; [3] Malaska, M., et al.: Icarus, 270, 130-161, 2016; [4] Barnes, J., et al.: Pl. Scie., 2:1, 2013; [5] Solomonidou, A., et al.: JGR, 119, 1729-1747, 2014; [6] Solomonidou, A., et al.: Icarus, 270, 85-99, 2016; [7] Schmitt, B., et al.: GhoSST database (ghosst.osug.fr).
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- 2016
6. Tethys – Geological and Spectral Properties
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Stephan, K., Jaumann, R., Wagner, Roland, Clark, R. N., Cruikshank, D. P., Dalle Ore, C., Brown, Robert H., Giese, B., Roatsch, Thomas, Matson, D. L., Baines, K. H., Filacchione, G., Capaccioni, F., Buratti, B.J., Nicholson, P. D., and Rodriguez, S.
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Planetengeologie ,Planetengeodäsie ,VIMS ,Cassini ,Tethys - Published
- 2015
7. Spectral properties of icy satellites
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Stephan, K., Jaumann, R., Wagner, Roland, Clark, R. N., Cruikshank, D. P., Brown, Robert H., Roatsch, Thomas, Buratti, B.J., Matson, D. L., Dalle Ore, C., Filacchione, G., Capaccioni, F., Nicholson, P. D., Baines, K. H., and Sotin, C.
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Planetengeologie ,spectroscopy ,geology ,icy satellites - Published
- 2015
8. Surface changes in mid-latitude regions on Titan
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Solomonidou, Anezina, Coustenis, Athéna, Lopes, Rosaly M. C., Hirtzig, Mathieu, Rodriguez, Sebastien, Stephan, Katrin, Sotin, Christophe, Drossart, Pierre, Lawrence, Kenneth J., Le Mouélic, Stéphane, Bratsolis, Emmanuel, Jaumann, Ralf, Brown, Robert H., Malaska, Michael J., Henry, Florence, Jet Propulsion Laboratory, California Institute of Technology (JPL), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Fondation La main à la pâte, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Deutsches Zentrum für Luft- und Raumfahrt (DLR), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), National and Kapodistrian University of Athens (NKUA), and Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, United States
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Planetengeologie ,Cassini Titan ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,[PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph] - Abstract
International audience; We present a study focused on the mid-latitude and close to the equator surface regions on Titan that present an interest on their spectral behavior and/or morphology. These are regions where spectroscopic anomalies have been reported in the evolution of the brightness and several interpretations have been proposed (cryovolcanic candidates, evaporates, lacustrine, etc [1;2;5]). Also in our work here we have included analysis of some undifferentiated plains (also referred to as 'blandlands'), which are vast expanses of terrains that appear bland in the radar data [3]. By applying a Radiative transfer code [4;2] we have analyzed these regions to look for evolution with time through their spectral behavior. We use as reference point and calibration tool the surface albedo retrieval of the Huygens Landing site (Titan's ground truth) and we also check the variability of the surface albedo of these regions against areas that are not expected to change with time (e.g. dune fields), by retrieving their albedo differences at all wavelengths [2]. We report here surface albedo changes with time for some of these regions of interest that imply connection to exogenic and/or endogenic processes.
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- 2014
9. 10 years of Cassini/VIMS observations at Titan
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Sotin, C., Brown, Robert H., Baines, K. H., Barnes, Jason W., Buratti, B.J., Clark, R. N., Jaumann, R., Le Mouelic, S., Nicholson, P. D., Rodriguez, S., Soderblom, J. M., Soderblom, L.A., and Stephan, K.
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Planetengeologie ,Cassini VIMS Titan - Published
- 2014
10. Titan's lakes and Mare observed by the Visual and Infrared Mapping Spectrometer
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Brown, Robert H., Soderblom, L.A., Sotin, C., Barnes, Jason W., Hayes, A., Lawrence, K.J., Le Mouelic, S., Rodriguez, S., Soderblom, Jason M., Baines, K. H., Buratti, B.J., Clark, R. N., Jaumann, R., Nicholson, P. D., and Stephan, K.
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Planetengeologie ,Titan - Abstract
Titan is the only place, besides Earth, that holds stable liquid bodies at its surface. The large Kraken Mare, first seen by ISS [1], was then observed by the radar instrument that discovered a large number of small lakes as well as two other Mare [2]. The liquid nature of these radar-dark features was later confirmed by the specular reflection observed by the Visual and Infrared Mapping Spectrometer (VIMS) over Kraken Mare [3] and by the very low albedo at 5-micron over Ontario Lacus [4]. The three largest lakes are called Mare and are all located in the North Pole area. It is remarkable that most of these lakes have been observed on the North Pole with only one large lake, Ontario lacus, located in the South Pole area. This observation suggests the influence of orbital parameters on the meteorology and the occurrence of rainfalls to refill the depressions [5]. Ethane was detected by the VIMS instrument as one component of Ontario lacus [4]. These lakes and Mare play a key role in Titan's meteorology as demonstrated by recent global circulation models [6]. Determining the composition and the evolution of those lakes has become a primary science objective of the Cassini extended mission. Since Titan entered northern spring in August 2009, the North Pole has been illuminated allowing observations at optical wavelengths. On June 5, 2010 the Visual and Infrared Mapping Spectrometer (VIMS) onboard the Cassini spacecraft observed the northern pole area with a pixel size from 3 to 7 km. These observations demonstrate that little of the solar flux at 5-micron is scattered by the atmosphere, which allowed us to build a mosaic covering an area of more than 500,000 km2 that overlaps and complements observations made by the Synthetic Aperture Radar (SAR) in 2007. We find that there is an excellent correlation between the shape of the radar dark area, known as Ligeia Mare and the VIMS 5-micron dark unit. Matching most of the radar shoreline, the 2010 VIMS observations suggest that the 125,000-km2 surface area of Ligeia Mare measured by RADAR in 2007 has not significantly changed [7]. The analysis of the 2-micron spectral window confirms the presence of ethane [8]. Because its saturation vapor pressure is several orders of magnitude smaller than that of methane, liquid ethane is expected to be very stable at Titan's surface conditions, which could explain the stability of the shorelines if ethane is the major compound of the lakes. VIMS observations of Ontario Lacus are planned in 2012 before it disappears in the polar night. Several observations of the northern lakes are planned in 2012 as well as observations of the Mare later in the mission. This work has been performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract to NASA. Government sponsorship acknowledged.
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- 2012
11. Enceladus: Correlation of Surface Particle Distribution and Geology
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Jaumann, R., Stephan, K., Brown, Robert H., Clark, R. N., Filacchione, G., Buratti, B.J., Nelson, R.M., Nicholson, P. D., Le Mouelic, S., Rodriguez, S., Hansen, G.B., Roatsch, Thomas, Capaccioni, F., and Sotin, C.
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Planetengeologie ,Enceladus ,Cassini ,Saturn satellite - Abstract
The surface of Enceladus consists almost completely of water ice [1,2]. The band depths of water ice absorptions are sensitive to the size of particles [2,3,4] covering the surface. The Visual and Infrared Mapping Spectrometer [5] observed Enceladus with high spatial resolution during multiple Cassini fly-bys. Based on these data we measured the band depths of water ice absorptions over Enceladus' surface and mapped their distribution. The spatial resolution of VIMS is sufficient to distinguish three major geologic units: heavily cratered terrain, fractured and ridged terrain and complex tectonically deformed regions of troughs and ridges [6], which include the south pole region. Surface ages, as derived from the impact flux models of [7,8] indicate the cratered terrain being oldest while the Sulci the youngest unit [2,9]. From the distribution of particle sizes we can conclude that the largest particle diameters are those inside the tectonically deformed regions, with a decrease in size departing from the fractures. These occur not only at the south pole but also in older tectonic regions [2]. The basic correlation between particle diameter, geologic unit and age suggests the following relative stratigraphic sequence [2,10]: (1) Formation of a primary crust (heavily cratered terrain); (2) Mechanical weathering of the surface particles by microimpacts and sputtering during the last 4 billion years; (3) Tectonic disruption of the surface and deposition of new material with large particles. Although this newly deposited material has undergone mechanical weathering of the particles by microimpacts and sputtering, these particles are larger due to a shorter exposure time; (4) Recent deposition of larger particles in the south polar region. If the larger particles in the tectonically deformed regions have of the same cryovolcanic origin as at the south pole, the volcanic activity must have a temporal evolution. However, there are still different possibilities to explain this observation [2]: (1) The eruption zones may have moved from north to south. (2) Cryovolcanic eruptions might have occurred across the entire surface and later shrunk to a small zone at the south pole, which would be indicative of a probable decrease in internal heat transfer. (3) The intensity of cryovolcanic eruptions had a different temporal evolution at different locations with maximum activity in the south polar region.
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- 2012
12. Spectral properties of fluvial terrain on Titan: An update
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Langhans, Mirjam, Jaumann, Ralf, Stephan, Katrin, Brown, Robert H., Buratti, Bonnie J., Clark, Roger, Baines, Kevin H., Nicholson, Phil D., and Lorenz, Ralph D.
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Planetengeologie ,VIMS ,Spectra ,Titan ,Methane ,Valleys - Published
- 2010
13. Valley formation from methane convective storms on Titan
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Langhans, Mirjam, Jaumann, Ralf, Stephan, Katrin, Brown, Robert H., Buratti, Bonnie J., Clark, Roger, Baines, Kevin H., Nicholson, Phil D., Lorenz, Ralph D., and Sotin, Christophe
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Planetengeologie ,Titan ,Methane ,Valleys - Published
- 2010
14. Specular reflection on Titan: Liquids in Kraken Mare
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Stephan, Katrin, Jaumann, Ralf, Brown, Robert H., Soderblom, Jason M., Soderblom, Laurence A., Barnes, Jason W., Sotin, Christophe, Griffith, Caitlin A., Kirk, Randolph L., Baines, Kevin H., Buratti, Bonnie J., Clark, Roger N., Lytle, Dyer M., Nelson, Robert M., and Nicholson, Phillip D.
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VIMS ,Cassini ,Liquids ,Titan ,Kraken Mare - Published
- 2010
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15. Zur Gestaltung von Rentensystemen der sozialen Sicherheit.
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Brown, Robert L.
- Abstract
Copyright of Internationale Revue für Soziale Sicherheit is the property of Wiley-Blackwell and its content may not be copied or emailed to multiple sites or posted to a listserv without the copyright holder's express written permission. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)
- Published
- 2008
- Full Text
- View/download PDF
16. Das Innere von Grönland
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Brown, Robert
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Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Statistics::Computation - Abstract
von Robert Brown
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- 1870
- Full Text
- View/download PDF
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