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251. Enfermedades de la infancia : explicaciones del Dr. E. Nogueras y Coronas ...

Author

Paredes, José María, imp, Vila da Riva, J, comp, Cordo Orosa, E, comp, Martínez Rocafort, J, comp, Nogueras y Coronas, E, 1882-1925, Paredes, José María, imp, Vila da Riva, J, comp, Cordo Orosa, E, comp, Martínez Rocafort, J, comp, and Nogueras y Coronas, E, 1882-1925

Published
1913

252. New solar axion search using the CERN Axion Solar Telescope with He-4 filling

Author

Arik, M., Aune, S., Barth, K., Belov, A., Braeuninger, H., Bremer, J., Burwitz, V., Cantatore, G., Carmona, J. M., Cetin, S. A., Collar, J. I., Da Riva, E., Dafni, T., Davenport, M., Dermenev, A., Eleftheriadis, C., Elias, N., Fanourakis, G., Ferrer-Ribas, E., Galan, J., Garcia, J. A., Gardikiotis, A., Garza, J. G., Gazis, E. N., Geralis, T., Georgiopoulou, E., Giomataris, I., Gninenko, S., Marzoa, M. Gomez, Hasinoff, M. D., Hoffmann, D. H. H., Iguaz, F. J., Irastorza, I. G., Jacoby, J., Jakovcic, K., Karuza, M., Kavuk, M., Krcmar, M., Kuster, M., Lakic, B., Laurent, J. M., Liolios, A., Ljubicic, A., Luzon, G., Neff, S., Niinikoski, T., Nordt, A., Ortega, I., Papaevangelou, T., Pivovaroff, M. J., Raffelt, G., Rodriguez, A., Rosu, M., Ruz, J., Savvidis, I., Shilon, I., Solanki, S. K., Stewart, L., Tomas, A., Vafeiadis, T., Villar, J., Vogel, J. K., Yildiz, S. C., Zioutas, K., and CAST Collaboration

Abstract

The CERN Axion Solar Telescope (CAST) searches for a -> gamma conversion in the 9 T magnetic field of a refurbished LHC test magnet that can be directed toward the Sun. Two parallel magnet bores can be filled with helium of adjustable pressure to match the x-ray refractive mass m(gamma) to the axion search mass m(a). After the vacuum phase (2003-2004), which is optimal for m(a) less than or similar to 0.02 eV, we used He-4 in 2005-2007 to cover the mass range of 0.02-0.39 eV and He-3 in 2009-2011 to scan from 0.39 to 1.17 eV. After improving the detectors and shielding, we returned to He-4 in 2012 to investigate a narrow m(a) range around 0.2 eV ("candidate setting" of our earlier search) and 0.39-0.42 eV, the upper axion mass range reachable with He-4, to "cross the axion line" for the KSVZ model. We have improved the limit on the axion-photon coupling to g(a gamma) < 1.47 x 10(-10) GeV-1 (95% C.L.), depending on the pressure settings. Since 2013, we have returned to the vacuum and aim for a significant increase in sensitivity.

253. Some remarks on the Neo-Babylonian Royal Inscriptions (626-539 BCE)

Author

Da Riva, Rocío and Universitat de Barcelona

Subjects
Neo-Babylonian period, inscription, buildings, empire, cuneiform, monuments, Mesopotamia, Babylonia, Escriptura cuneïforme, Edificios, Imperio, Cuneiforme, Inscripción, Art mesopotàmic, Monumentos, Neo-babylonian period, Periodo neobabilónico, Babilònia, Babilonia, Monuments, Akkadian cuneiform inscriptions, Inscription, Empire, Mesopotamian art, periodo neobabilónico, inscripción, edificios, imperio, cuneiforme, monumentos, Cuneiform writing, Buildings, Inscripcions accàdies, Cuneiform
Abstract

[spa] El periodo neo-babilónico es uno de los mejor documentados de la antigua Mesopotamia. Se han conservado miles de documentos económicos y administrativos, tanto en archivos institucionales como privados, así como centenares de inscripciones reales y diversas crónicas y textos literarios. En el presente artículo se realiza un repaso de las inscripciones reales, analizando sus características más importantes., [eng] The Neo-Babylonian period is one of the best documented in ancient Mesopotamia. Many thousands of economic and administrative texts have been preserved both from institutional and private archives, as well as hundreds of royal inscriptions, and several chronicles and literary texts. This article offers a review of the royal inscriptions analysing their most important features.

254. Search for Solar Axions by the CERN Axion Solar Telescope with He-3 Buffer Gas: Closing the Hot Dark Matter Gap

Author

Arik, M., Aune, S., Barth, K., Belov, A., Borghi, S., Braeuninger, H., Cantatore, G., Carmona, J. M., Cetin, S. A., Collar, J. I., Da Riva, E., Dafni, T., Davenport, M., Eleftheriadis, C., Elias, N., Fanourakis, G., Ferrer-Ribas, E., Friedrich, P., Galan, J., Garcia, J. A., Gardikiotis, A., Garza, J. G., Gazis, E. N., Geralis, T., Georgiopoulou, E., Giomataris, I., Gninenko, S., Gomez, H., Marzoa, M. Gomez, Gruber, E., Guthoerl, T., Hartmann, R., Hauf, S., Haug, F., Hasinoff, M. D., Hoffmann, D. H. H., Iguaz, F. J., Irastorza, I. G., Jacoby, J., Jakovcic, K., Karuza, M., Koenigsmann, K., Kotthaus, R., Krcmar, M., Kuster, M., Lakic, B., Lang, P. M., Laurent, J. M., Liolios, A., Ljubicic, A., Luzon, G., Neff, S., Niinikoski, T., Nordt, A., Papaevangelou, T., Pivovaroff, M. J., Raffelt, G., Riege, H., Rodriguez, A., Rosu, M., Ruz, J., Savvidis, I., Shilon, I., Silva, P. S., Solanki, S. K., Stewart, L., Tomas, A., Tsagri, M., Van Bibber, K., Vafeiadis, T., Villar, J., Vogel, J. K., and CAST Collaboration

Subjects
Physics::Instrumentation and Detectors, Astrophysics::Earth and Planetary Astrophysics
Abstract

The CERN Axion Solar Telescope has finished its search for solar axions with He-3 buffer gas, covering the search range 0.64 eV less than or similar to ma less than or similar to 1.17 eV. This closes the gap to the cosmological hot dark matter limit and actually overlaps with it. From the absence of excess x rays when the magnet was pointing to the Sun we set a typical upper limit on the axion-photon coupling of g(a gamma) less than or similar to 3.3 x 10(-10) GeV-1 at 95% C.L., with the exact value depending on the pressure setting. Future direct solar axion searches will focus on increasing the sensitivity to smaller values of g(a gamma), for example by the currently discussed next generation helioscope International AXion Observatory.

255. 'El yacimiento de Sela (Jordania) La expansión imperial neo-babilónica en el altiplano de Edom a mediados del I milenio a.C.[The Site of Sela (Jordan)]

Author

Da Riva, Rocío and Universitat de Barcelona

Subjects
Jordan, Archaeology, Iron age, Edat del ferro, Jordània, Arqueologia
Abstract

The site of as-Sila has been identified with Edomite Sela, frequently mentioned in the Bible. The site was important in the Iron Age (as demonstrated by the presence of many structures and the Neo-Babylonian cuneiform rock-inscription of king Nabonidus, 556-539 BCE), and also during the Nabatean and Roman periods. The survey work at Sela has revealed a very large site with a considerable number of structures related to water, and architectonic structures of varying sizes: rock-cut houses, remains of rock-cut large buildings, towers, etc. A comprehensive study of the site would help us to analyse the relationship between the Neo-Babylonian Empire and the West (Edom) in the context of Nabonidus' Arabian campaigns.

263. An Alternative Method for Thermal Plume–Induced Aerosol Release and Deposition Calculations in Large Geometries Using fireFoam.

Author

Plagge, Michael, Krause, Ulrich, Da Riva, Enrico, Schäfer, Christoph, and Forkel-Wirth, Doris

Abstract

Being a particle physics laboratory, the European Organization for Nuclear Research (CERN) plans, constructs, and maintains installations emitting ionizing radiation during operation. Activation of present material is a consequence. Hence, fire scenarios for certain CERN installations must take into account the presence of radioactive material. Releases of gaseous, liquid, or solid combustion products, e.g., attached to aerosols, are taken so far into account by a worst case approach. Scenarios taking place in underground installations assume hence a smoke transport coefficient of 100% of release toward the surface level, independent of the local geometry. For a radioactive inventory identified in a certain fire load, this results in a conservative release. To overcome this conservative worst case approach, a computational fluid dynamics model based on FM Global’s fireFoam 2.2.x is proposed. Its Lagrangian library was modified in order to provide aerosol release and deposition information based on more detailed interaction data between Lagrangian particles and their surrounding geometry. Results are shown for a CERN-typical large-scale experimental cavern placed 100 m below surface level. A simple diffusion burner is modeled inside the cavern to create a thermal plume emerging from a 1.5-MW fire over 14 min. Lagrangian particles are used to model aerosols with an aerodynamic diameter of 1, 10, and 100 μm, injected into the emerging thermal plume. Results for particle release and deposition vary according to aerodynamic diameter. In the present case, maximums of ~32% and 39% are found for 1- and 10-μm particles, respectively, being released to the surface level. [ABSTRACT FROM PUBLISHER]

Published
2017
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266. Organización espacial y gestión de los recursos hídricos en el altiplano de Edom durante el I milenio a.C.: el yacimiento de Sela (Tafila, Jordania)

Author

Marsal Aguilera, Roser, Da Riva, Rocío, Moreno Garcia, Juan Carlos, Riera i Mora, Santiago, and Universitat de Barcelona. Facultat de Geografia i Història

Subjects
Jordan, Iron age, Orient Mitjà, Edad del hierro, Jordània, Arqueologia, Ciències Humanes i Socials, Arqueología, Edomitas, Middle East, Archaeology, Edomites, Oriente Medio, Jordania, Edat del ferro, Explotación de recursos hidráulicos, Explotació de recursos hidràulics, Water resources development
Abstract

[spa] La disponibilidad de recursos hídricos para el abastecimiento de las necesidades de las sociedades ha sido fundamental a lo largo del tiempo. Esto es aún es más relevante en aquellos territorios donde el agua es un recurso escaso y limitado. Ante estas dificultades, se han desarrollado continuamente estrategias, métodos y técnicas para gestionar eficientemente estos recursos, conformando distintas “culturas del agua”. Este desarrollo se ha podido observar tanto en las denominadas civilizaciones hidráulicas como en otras comunidades de tipo local-regional sin que hubiera la necesidad de una intervención centralizada o estatal. La gestión local del agua, que incluyó sistemas de captación, conducción, almacenamiento y preservación del agua, garantizó el abastecimiento necesario para la subsistencia de esas sociedades. El yacimiento de Sela, ubicado en la región semiárida del sur de la Transjordania, contiene numerosos vestigios arqueológicos de estructuras hidráulicas. Estas evidencian que existió la necesidad de implementar infraestructuras para la gestión del agua en una región donde su disponibilidad es y fue limitada. El objetivo de este trabajo es el de documentar, analizar y estudiar las diferentes estrategias, mecanismos e instalaciones que permitieron la gestión de los recursos hídricos en Sela, desde la captación hasta el suministro para su uso. A partir de la información obtenida durante las prospecciones arqueológica llevadas a cabo en los años 2015 y 2016, se ha realizado la identificación, documentación y análisis de las instalaciones hidráulicas del yacimiento de forma pormenorizada. Para estudiar la distribución espacial de las instalaciones y establecer sus principales conexiones, se ha elaborado una planimetría arqueológica en 2D y se ha reconstruido un modelo tridimensional de un área concreta del yacimiento. Los datos resultantes se han comparado, tras realizar una investigación bibliográfica, con los datos existentes sobre instalaciones hidráulicas identificadas por parte de cinco proyectos arqueológicos desarrollados en el sur de la Transjordania en diferentes momentos. Complementariamente a este estudio, se ha realizado la caracterización petrográfica y mineralógica de catorce muestras de morteros extraídas de distintas instalaciones hidráulicas, tomando como base un informe previo elaborado por M. Soto (2017). Los resultados obtenidos en este trabajo, han permitido determinar cuáles fueron las posibles fuentes de agua disponibles y han evidenciado la existencia de distintas estrategias, técnicas y métodos para su gestión. El análisis y el estudio de la gran variedad de instalaciones existentes, ha permitido caracterizar los distintos sistemas hidráulicos presentes en el yacimiento de Sela. Las instalaciones que se han conservado, indican que el principal objetivo de la hidrotecnología desarrollada en Sela se basó principalmente en la implementación de instalaciones de acopio, conducción, almacenamiento y preservación del agua para garantizar el mayor volumen y calidad de agua para su consumo. Los resultados obtenidos, junto con su contextualización regional, sugieren que el poblamiento de Sela, desde un punto de vista sociopolítico, económico y cultural, se desarrolló mediante pequeños grupos locales. La ausencia de una red hidráulica jerarquizada y centralizada, así como su composición, basada principalmente en pequeñas unidades de captación, conducción y almacenamiento del agua, sugieren un uso familiar y doméstico de estas instalaciones. Estos sistemas han permitido formular distintas hipótesis en torno al modelo de ocupación del asentamiento sobre la base de la tecnología del agua, teniendo en cuenta nuevos factores: la disponibilidad y acceso a los recursos hídricos, la cantidad de estructuras y la variedad de sistemas, dispositivos, así como el diseño de las redes hidráulicas. La propuesta expuesta en este trabajo se ha realizado desde una perspectiva diacrónica, puesto que las instalaciones hidráulicas analizadas no han podido ser asignadas a un periodo cronológico específico dentro de las distintas fases de ocupación del yacimiento. Finalmente, pese a las limitaciones con las que se ha encontrado este estudio como es la imposibilidad de fechar mediante técnicas absolutas las instalaciones hidráulicas y su estado de conservación, el presente estudio pone de relieve la singularidad y el gran potencial del registro arqueológico de Sela para el conocimiento de la gestión de los recursos hídricos en el sur de la Transjordania y de sus implicaciones socioeconómicas, políticas y culturales a lo largo del tiempo., [eng] The availability of water resources has been essential over time. This is even more outstanding in those territories where water is a scarce and limited resource. Faced with these difficulties, several strategies, methods, and techniques have been continuously developed to efficiently manage these resources, shaping different “water cultures”. This development has been observed both in the so-called hydraulic civilisations and in other local-regional communities without the need for centralised or state intervention. Local water management, which included systems for the collection, conduction, storage, and preservation of water, guaranteed the supply necessary for the subsistence of these societies. The site of Sela, located in the semi-arid region of southern Transjordan, contains numerous archaeological remains of hydraulic structures. This is evidence of the need to implement water management infrastructures in a region where water availability is and was limited. This work aims to document, analyse, and study the different strategies, mechanisms, and facilities that allowed the management of water resources in Sela, from collection to supply for use. Based on the information obtained during the archaeological surveys conducted in 2015 and 2016, the identification, documentation, and analysis of the hydraulic installations were carried out in detail. To study the spatial distribution of the facilities and establish their main connections, a 2D archaeological planimetry has been drawn up and a three-dimensional model of a specific area of the site has been reconstructed. The resulting data has been compared with existing data on hydraulic installations identified by five archaeological projects carried out in the south of the Transjordan at different times. As a complement to this study, a petrographic and mineralogical characterisation of fourteen samples of mortar extracted from different hydraulic installations has been carried out. The results obtained in this work have made it possible to determine the potential sources of water available and have shown the existence of different strategies, techniques, and methods for its management. The analysis and study of the wide variety of existing installations has allowed us to characterise the different hydraulic systems present at the site of Sela. The facilities that have been conserved indicate that the main goal of the hydro-technology developed at Sela was mainly based on the implementation of water collection, conduction, storage, and preservation facilities to guarantee the highest possible volume and quality of water for consumption. The results obtained, together with their regional contextualisation, suggest that the population of Sela, from a socio-political, economic, and cultural point of view, developed through small local groups. The absence of a hierarchical and centralised hydraulic network, as well as its composition, based mainly on small water collection, conduction, and storage units, suggest that these facilities are used by families and households. These systems have allowed us to formulate different hypotheses regarding the model of settlement occupation based on water technology. To that end, it has been taken into account the availability and access to water resources, the number of structures and the variety of systems, devices as well as the design of hydraulic networks. The proposal set out in this work has been made from a diachronic perspective since the hydraulic installations analysed could not be assigned to a specific chronological period within the different phases of occupation of the site. Finally, despite the limitations encountered in this study, such as the impossibility of dating the hydraulic installations using absolute techniques and their state of conservation, the current study highlights the uniqueness and great potential of the archaeological record of Sela with regard of the management of water resources in the south of the Transjordan and its socio-economic, political and cultural implications over time.

Published
2021

267. Search for Solar Axions by the CERN Axion Solar Telescope with 3He Buffer Gas: Closing the Hot Dark Matter Gap.

Author

Arik, M., Aune, S., Barth, K., Belov, A., Borghi, S., Bräuninger, H., Cantatore, G., Carmona, J. M., Cetin, S. A., Collar, J. I., Da Riva, E., Dafni, T., Davenport, M., Eleftheriadis, C., Elias, N., Fanourakis, G., Ferrer-Ribas, E., Friedrich, R., Galán, J., and García, J. A.

Subjects
*AXIONS, *SOLAR telescopes, *DARK matter, *PECCEI-Quinn theory, *HUBBLE constant, *EQUATIONS of state
Abstract

The CERN Axion Solar Telescope has finished its search for solar axions with 3He buffer gas, covering the search range 0.64 eV ≲ mα ≲ 1.17 eV. This closes the gap to the cosmological hot dark matter limit and actually overlaps with it. From the absence of excess x rays when the magnet was pointing to the Sun we set a typical upper limit on the axion-photon coupling of gαγ ≲ 3.3 x 10-10 GeV-1 at 95% C.L., with the exact value depending on the pressure setting. Future direct solar axion searches will focus on increasing the sensitivity to smaller values of gαγ, for example by the currently discussed next generation helioscope International AXion Observatory. [ABSTRACT FROM AUTHOR]

Published
2014
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268. New solar axion search using the CERN Axion Solar Telescope with 4He filling.

Author

Arik, M., Aune, S., Barth, K., Belov, A., Bräuninger, H., Bremer, J., Burwitz, V., Cantatore, G., Carmona, J. M., Cetin, S. A., Collar, J. I., Da Riva, E., Dafni, T., Davenport, M., Dermenev, A., Eleftheriadis, C., Elias, N., Fanourakis, G., Ferrer-Ribas, E., and Galán, J.

Subjects
*AXIONS, *SOLAR telescopes, *HELIUM
Abstract

The CERN Axion Solar Telescope (CAST) searches for a → γ conversion in the 9 T magnetic field of a refurbished LHC test magnet that can be directed toward the Sun. Two parallel magnet bores can be filled with helium of adjustable pressure to match the x-ray refractive mass mγ to the axion search mass ma. After the vacuum phase (2003-2004), which is optimal for ma ≲ 0.02 eV, we used 4He in 2005-2007 to cover the mass range of 0.02-0.39 eVand ³He in 2009-2011 to scan from 0.39 to 1.17 eV. After improving the detectors and shielding, we returned to 4He in 2012 to investigate a narrow ma range around 0.2 eV ("candidate setting" of our earlier search) and 0.39-0.42 eV, the upper axion mass range reachable with 4He, to "cross the axion line" for the KSVZ model. We have improved the limit on the axion-photon coupling to gaγ < 1.47 x 10-10 GeV-1 (95% C.L.), depending on the pressure settings. Since 2013, we have returned to the vacuum and aim for a significant increase in sensitivity. [ABSTRACT FROM AUTHOR]

Published
2015
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269. Continuous photodegradation of naphthalene in water catalyzed by TiO2 supported on glass Raschig rings

Author

García-Martínez, M.J., Canoira, L., Blázquez, G., Da Riva, I., Alcántara, R., and Llamas, J.F.

Subjects
*POLYCYCLIC aromatic compounds, *POLYCYCLIC aromatic hydrocarbons, *TITANIUM dioxide, *HYDROCARBONS
Abstract

Abstract: Polycyclic aromatic hydrocarbons (PAH''s) are a class of persistent organic pollutants of special concern since they are carcinogenic and mutagenic. In this paper, the design of a continuously stirred tank reactor is reported for the photodegradation of the simplest and most water-soluble PAH, naphthalene, in water using TiO2 (in the crystalline form of anatase), supported on glass Raschig rings as catalyst, with oxygen as electron acceptor. A first order kinetic rate constant has been calculated for this photodegradation. The irradiated solution after the reaction has been analysed and only traces of 1-naphthol, 1,4-naphthalenedione and phthalates have been found as intermediate products of the photodegradation. [Copyright &y& Elsevier]

Published
2005
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270. High pressure liquid chromatography and electrospray ionization mass spectrometry are advantageously integrated into a two-levels approach to detection and identification of haemoglobin variants.

Author

Caruso, D., Crestani, M., Mitro, N., da Riva, L., Mozzi, R., Sarpau, S., Merlotti, C., and Franzini, C.

Subjects
*HEMOGLOBINS, *NUCLEOTIDE sequence, *MASS spectrometry, *RESEARCH, *BLOOD pigments, *CHROMATOGRAPHIC analysis
Abstract

Detecting and correctly identifying haemoglobin (Hb) variants is typically achieved by a two-levels laboratory approach. We report our experience in dealing with 91 Hb variants, including a number of frequent and a few rare variants. Screening included akaline agarose gel electrophoresis (AGE), ion-exchange automated high-performance liquid chromatography (HPLC) and a test for deoxyhaemoglobin solubility. Identification was based on electrospray ionization–mass spectrometry (ESI–MS). Our results confirmed the advantages of HPLC over AGE for screening, because of the occurrence of some electrophoretically‘silent’ variants. ESI–MS permitted the definitive identification of 90 of the 91 variants included in the study, in some cases (e.g. HbS) through the application of a simple protocol (direct injection of the sample), in other cases requiring the application of more demanding procedures (purification of the variant chain and peptide analysis after enzymatic or chemical cleavage). In an additional case (Hb J-Oxford), ESI–MS assay did not lead to definitive identification, but gave indications for designing the appropriate primers to focus DNA sequence analysis on the specific region of the gene. Deoxyhaemoglobin solubility test was positive only in the presence of HbS. We conclude that HPLC and ESI–MS are advantageously integrated into a two-level analytical system for the detection and confirmation of variant Hbs. [ABSTRACT FROM AUTHOR]

Published
2005
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271. Martian dust storm impact on atmospheric H2O and D/H observed by ExoMars Trace Gas Orbiter

Author

Vandaele, Ann Carine, Korablev, Oleg, Daerden, Frank, Aoki, Shohei, Thomas, Ian R., ALTIERI, FRANCESCA, López-Valverde, Miguel, Villanueva, Geronimo, Liuzzi, Giuliano, Smith, Michael D., Erwin, Justin T., Trompet, Loïc, Fedorova, Anna A., Montmessin, Franck, Trokhimovskiy, Alexander, Belyaev, Denis A., Ignatiev, Nikolay I., Luginin, Mikhail, Olsen, Kevin S., Baggio, Lucio, Alday, Juan, Bertaux, Jean-Loup, Betsis, Daria, Bolsée, David, Clancy, R. Todd, CLOUTIS, EDWARD, Depiesse, Cédric, Funke, Bernd, Garcia-Comas, Maia, Gérard, Jean-Claude, GIURANNA, MARCO, Gonzalez-Galindo, Francisco, Grigoriev, Alexey V., Ivanov, Yuriy S., Kaminski, Jacek, Karatekin, Ozgur, Lefèvre, Franck, Lewis, Stephen, López-Puertas, Manuel, Mahieux, Arnaud, Maslov, Igor, Mason, Jon, Mumma, Michael J., Neary, Lori, Neefs, Eddy, Patrakeev, Andrey, Patsaev, Dmitry, Ristic, Bojan, Robert, Séverine, Schmidt, Frédéric, Shakun, Alexey, Teanby, Nicholas A., Viscardy, Sébastien, Willame, Yannick, Whiteway, James, Wilquet, Valérie, Wolff, Michael J., BELLUCCI, Giancarlo, Patel, Manish R., López-Moreno, Jose-Juan, Forget, François, Wilson, Colin F., Svedhem, Håkan, Vago, Jorge L., Rodionov, Daniel, NOMAD Science Team, Alonso-Rodrigo, Gustavo, Bauduin, Sophie, Carrozzo, Giacomo, Crismani, Matteo, da Pieve, Fabiana, D'AVERSA, EMILIANO, Etiope, Giuseppe, Fussen, Didier, Geminale, Anna, Gkouvelis, Leo, Holmes, James, Hubert, Benoît, Ignatiev, Nicolay I., Kasaba, Yasumasa, Kass, David, Kleinböhl, Armin, LANCIANO, ORIETTA, Nakagawa, Hiromu, Novak, Robert E., Oliva, Fabrizio, Piccialli, Arianna, Renotte, Etienne, Ritter, Birgit, Schneider, Nick, SINDONI, Giuseppe, Thiemann, Ed, Vander Auwera, Jean, Wilquet, Valerie, WOLKENBERG, PAULINA MARIA, Yelle, Roger, ACS Science Team, Anufreychik, Konstantin, Arnold, Gabriele, Duxbury, Natalia, Fouchet, Thierry, GRASSI, Davide, Guerlet, Sandrine, Hartogh, Paul, Khatuntsev, Igor, Kokonkov, Nikita, Krasnopolsky, Vladimir, Kuzmin, Ruslan, Lacombe, Gaétan, Lellouch, Emmanuel, Määttänen, Anni, Marcq, Emmanuel, Martin-Torres, Javier, Medvedev, Alexander, Millour, Ehouarn, Moshkin, Boris, Quantin-Nataf, Cathy, Rodin, Alexander, Shematovich, Valery, Thomas, Nicolas, Trokhimovsky, Alexander, Vazquez, Luis, Vincendon, Matthieu, Young, Roland, Zasova, Ludmila, Zelenyi, Lev, Zorzano, Maria Paz, Parejo, J, Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Main Astronomical Observatory of NAS of Ukraine (MAO), National Academy of Sciences of Ukraine (NASU), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Instituto Universitario de Microgravedad 'Ignacio Da Riva' (IDR), Universidad Politécnica de Madrid (UPM), Spectroscopie de l'atmosphère, Service de Chimie Quantique et Photophysique, Université libre de Bruxelles (ULB), Space Science Institute [Boulder] (SSI), Department of Geography [Winnipeg], University of Winnipeg, NASA Goddard Space Flight Center (GSFC), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Institute of Geophysics [Warsaw], Polska Akademia Nauk = Polish Academy of Sciences (PAN), Royal Observatory of Belgium [Brussels] (ROB), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Agenzia Spaziale Italiana (ASI), Graduate School of Information Sciences [Sendai], Tohoku University [Sendai], Advanced Mechanical and Optical Systems SA (AMOS), Géosciences Paris Sud (GEOPS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], School of Earth Sciences [Bristol], University of Bristol [Bristol], Centre for Research in Earth and Space Science [Toronto] (CRESS), York University [Toronto], Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Department of Physics [Oxford], University of Oxford [Oxford], DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (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), Lomonosov Moscow State University (MSU), 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), 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), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), 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)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Institute for Astrophysics and Computational Sciences [Washington], Catholic University of America, Department of Computer Science, Electrical and Space Engineering [Luleå], Luleå University of Technology (LUT), 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), Moscow Institute of Physics and Technology [Moscow] (MIPT), Institute of Astronomy of the Russian Academy of Sciences (INASAN), University of Bern, Universidad Complutense de Madrid = Complutense University of 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), Centro de Astrobiologia [Madrid] (CAB), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Université Libre de Bruxelles [Bruxelles] (ULB), The Open University [Milton Keynes] (OU), Polska Akademia Nauk (PAN), Royal Observatory of Belgium [Brussels], IMPEC - 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), École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS 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), Universidad Complutense de Madrid [Madrid] (UCM), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Agence Spatiale Européenne = European Space Agency (ESA), University of Oxford, 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), 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), 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), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Ministerio de Ciencia e Innovación (España), European Space Agency, Belgian Science Policy Office, European Commission, UK Space Agency, Agenzia Spaziale Italiana, Ministerio de Ciencia, Innovación y Universidades (España), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Roscosmos, Centre National de la Recherche Scientifique (France), and Russian Government

Subjects
Martian, Ice cloud, Multidisciplinary, 010504 meteorology & atmospheric sciences, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Storm, Atmosphere of Mars, Atmospheric sciences, 01 natural sciences, Trace gas, chemistry.chemical_compound, chemistry, 13. Climate action, Dust storm, 0103 physical sciences, Environmental science, Semiheavy water, 010303 astronomy & astrophysics, Water vapor, 0105 earth and related environmental sciences, Sciences exactes et naturelles
Abstract

A publisher correction to this article was published on 17 April 2019, Global dust storms on Mars are rare1,2 but can affect the Martian atmosphere for several months. They can cause changes in atmospheric dynamics and inflation of the atmosphere3, primarily owing to solar heating of the dust3. In turn, changes in atmospheric dynamics can affect the distribution of atmospheric water vapour, with potential implications for the atmospheric photochemistry and climate on Mars4. Recent observations of the water vapour abundance in the Martian atmosphere during dust storm conditions revealed a high-altitude increase in atmospheric water vapour that was more pronounced at high northern latitudes5,6, as well as a decrease in the water column at low latitudes7,8. Here we present concurrent, high-resolution measurements of dust, water and semiheavy water (HDO) at the onset of a global dust storm, obtained by the NOMAD and ACS instruments onboard the ExoMars Trace Gas Orbiter. We report the vertical distribution of the HDO/H2O ratio (D/H) from the planetary boundary layer up to an altitude of 80 kilometres. Our findings suggest that before the onset of the dust storm, HDO abundances were reduced to levels below detectability at altitudes above 40 kilometres. This decrease in HDO coincided with the presence of water-ice clouds. During the storm, an increase in the abundance of H2O and HDO was observed at altitudes between 40 and 80 kilometres. We propose that these increased abundances may be the result of warmer temperatures during the dust storm causing stronger atmospheric circulation and preventing ice cloud formation, which may confine water vapour to lower altitudes through gravitational fall and subsequent sublimation of ice crystals3. The observed changes in H2O and HDO abundance occurred within a few days during the development of the dust storm, suggesting a fast impact of dust storms on the Martian atmosphere. © 2019, The Author(s), under exclusive licence to Springer Nature Limited., This project acknowledges funding by the Belgian Science Policy Office (BELSPO), with financial and contractual coordination by the ESA Prodex Office (PEA 4000103401, 4000121493); by the Spanish MICINN through its Plan Nacional and by European funds under grants ESP2015-65064-C2-1-P and ESP2017-87143-R (MINECO/FEDER); by the UK Space Agency through grants ST/R005761/1, ST/P001262/1, ST/R001405/1, ST/S00145X/1, ST/R001367/1, ST/P001572/1 and ST/R001502/1; and the Italian Space Agency through grant 2018-2-HH.0. The IAA/CSIC team acknowledges financial support from the State Agency for Research of the Spanish MCIU through the 'Center of Excellence Severo Ochoa' award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). This work was supported by the Belgian Fonds de la Recherche Scientifique - FNRS under grant number 30442502 (ET_HOME). The ACS experiment is led by IKI, Space Research Institute in Moscow, assisted by LATMOS in France. The project acknowledges funding by Roscosmos and CNES. The science operations of ACS are funded by Roscosmos and ESA. IKI affiliates acknowledge funding under grant number 14.W03.31.0017 and contract number 0120.0 602993 (0028-2014-0004) of the Russian government.

Published
2019
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272. --nite ridin' on da riva.

Author

Arkansas State University. Wind Ensemble. Performer, Contorno, Nicholas J. Arranger, Houseknecht, Bruce. Arranger, O'Neal, Thomas J. Conductor, Chesnokov, P. G. (Pavel Grigorʹevich), 1877-1944. Prichastnykh, op. 25. Spasenie sodelal; arranged., Grafulla, C. S. (Claudio S.), 1810-1880. Calvary quick-step., Grainger, Percy, 1882-1961. British folk-music settings. band. Molly on the shore,, Grainger, Percy, 1882-1961. British folk-music settings. band. Ye banks and braes o' bonnie Doon,, Grainger, Percy, 1882-1961. In a nutshell suite. Cornstalks march; arranged., O'Connor, Tom, 1943- Nite ridin' on da riva., Stamp, Jack. Prayer and jubilation., Wallace, William Vincent, 1812-1865. Maritana. Alas! those chimes so sweetly stealing; arranged., Wood, Haydn, 1882-1959. Mannin veen., and Youtz, Gregory, 1956- Scherzo for a bitter moon.

Published
1997

273. Invading Mesopotamia, from Alexander the Great to Antiochus VII

Author

Monerie, Julien, Histoire et Archéologie de l'Orient Cunéiforme (HAROC), Archéologies et Sciences de l'Antiquité (ArScAn), Université Paris 1 Panthéon-Sorbonne (UP1)-Université Paris 8 Vincennes-Saint-Denis (UP8)-Université Paris Nanterre (UPN)-Ministère de la Culture et de la Communication (MCC)-Institut national de recherches archéologiques préventives (Inrap)-Centre National de la Recherche Scientifique (CNRS)-Université Paris 1 Panthéon-Sorbonne (UP1)-Université Paris 8 Vincennes-Saint-Denis (UP8)-Université Paris Nanterre (UPN)-Ministère de la Culture et de la Communication (MCC)-Institut national de recherches archéologiques préventives (Inrap)-Centre National de la Recherche Scientifique (CNRS), Université Paris 1 Panthéon-Sorbonne (UP1), Université Paris 1 Panthéon-Sorbonne (UP1)-Université Paris 8 Vincennes-Saint-Denis (UP8)-Université Paris Nanterre (UPN)-Ministère de la Culture et de la Communication (MCC)-Institut national de recherches archéologiques préventives (Inrap)-Centre National de la Recherche Scientifique (CNRS), R. Da Riva / M. Lang / S. Fink, and Monerie, Julien

Subjects
[SHS.HIST] Humanities and Social Sciences/History, [SHS.HIST]Humanities and Social Sciences/History
Abstract

International audience

Published
2019

274. No detection of methane on Mars from early ExoMars Trace Gas Orbiter observations

Author

Korablev, Oleg, Avandaele, Ann Carine, Montmessin, Franck, Fedorova, Anna A., Trokhimovskiy, Alexander, Forget, François, Lefèvre, Franck, Daerden, Frank, Thomas, Ian R., Trompet, Loïc, Erwin, Justin T., Kasaba, Yasumasa, Kass, David, Khatuntsev, Igor, Kleinböhl, Armin, Kokonkov, Nikita, Krasnopolsky, Vladimir, Kuzmin, Ruslan, Lacombe, Gaétan, LANCIANO, ORIETTA, Lellouch, Emmanuel, Oliva, Fabrizio, Lewis, Stephen, Luginin, Mikhail, Liuzzi, Giuliano, López-Puertas, Manuel, López-Valverde, Miguel, Määttänen, Anni, Mahieux, Arnaud, Marcq, Emmanuel, Martin-Torres, Javier, Maslov, Igor, Patsaev, Dmitry, Medvedev, Alexander, Millour, Ehouarn, Moshkin, Boris, Mumma, Michael J., Nakagawa, Hiromu, Novak, Robert E., Piccialli, Arianna, Quantin-Nataf, Cathy, Renotte, Etienne, Ritter, Birgit, Rodin, Alexander, Schmidt, Frédéric, Schneider, Nick, Shematovich, Valery, Aoki, Shohei, Smith, Michael D., Teanby, Nicholas A., Thiemann, Ed, Thomas, Nicolas, Vander Auwera, Jean, Vazquez, Luis, Villanueva, Geronimo, Vincendon, Matthieu, Whiteway, James, Wilquet, Valérie, Robert, Séverine, Wolff, Michael J., WOLKENBERG, PAULINA MARIA, Yelle, Roger, Young, Roland, Zasova, Ludmila, Zorzano, Maria Paz, Neary, Lori, Viscardy, Sébastien, Grigoriev, Alexey V., Ignatiev, Nikolay I., Shakun, Alexey, Patrakeev, Andrey, Belyaev, Denis A., Bertaux, Jean-Loup, Olsen, Kevin S., Baggio, Lucio, Alday, Juan, Ivanov, Yuriy S., Ristic, Bojan, Mason, Jon, Willame, Yannick, Depiesse, Cédric, Hetey, Laszlo, Berkenbosch, Sophie, Clairquin, Roland, Queirolo, Claudio, Beeckman, Bram, Neefs, Eddy, Patel, Manish R., BELLUCCI, Giancarlo, López-Moreno, Jose-Juan, Wilson, Colin F., Etiope, Giuseppe, Zelenyi, Lev, Svedhem, Håkan, Vago, Jorge L., ACS Science Team, NOMAD Science Team, Alonso-Rodrigo, Gustavo, ALTIERI, FRANCESCA, Anufreychik, Konstantin, Arnold, Gabriele, Bauduin, Sophie, Bolsée, David, CARROZZO, FILIPPO GIACOMO, Clancy, R. Todd, CLOUTIS, EDWARD, Crismani, Matteo, da Pieve, Fabiana, D'AVERSA, EMILIANO, Duxbury, Natalia, Encrenaz, Therese, Fouchet, Thierry, Funke, Bernd, Fussen, Didier, Garcia-Comas, Maia, Gérard, Jean-Claude, GIURANNA, MARCO, Gkouvelis, Leo, Gonzalez-Galindo, Francisco, GRASSI, Davide, Guerlet, Sandrine, Hartogh, Paul, Holmes, James, Hubert, Benoît, Kaminski, Jacek, Karatekin, Ozgur, Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (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), 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), 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), Department of Physics [Oxford], University of Oxford [Oxford], Main Astronomical Observatory of NAS of Ukraine (MAO), National Academy of Sciences of Ukraine (NASU), School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Istituto Nazionale di Geofisica e Vulcanologia - Sezione di Roma (INGV), Istituto Nazionale di Geofisica e Vulcanologia, Faculty of Environmental Science and Engineering [Cluj-Napoca], Babes-Bolyai University [Cluj-Napoca] (UBB), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Instituto Universitario de Microgravedad 'Ignacio Da Riva' (IDR), Universidad Politécnica de Madrid (UPM), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Spectroscopie de l'atmosphère, Service de Chimie Quantique et Photophysique, Université libre de Bruxelles (ULB), Space Science Institute [Boulder] (SSI), Department of Geography [Winnipeg], University of Winnipeg, NASA Goddard Space Flight Center (GSFC), Lomonosov Moscow State University (MSU), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), 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)-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, Institute of Geophysics [Warsaw], Polska Akademia Nauk = Polish Academy of Sciences (PAN), Royal Observatory of Belgium [Brussels] (ROB), Graduate School of Information Sciences [Sendai], Tohoku University [Sendai], Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institute for Astrophysics and Computational Sciences [Washington], Catholic University of America, Agenzia Spaziale Italiana (ASI), Department of Computer Science, Electrical and Space Engineering [Luleå], Luleå University of Technology (LUT), 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), Advanced Mechanical and Optical Systems SA (AMOS), Moscow Institute of Physics and Technology [Moscow] (MIPT), Géosciences Paris Sud (GEOPS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Institute of Astronomy of the Russian Academy of Sciences (INASAN), School of Earth Sciences [Bristol], University of Bristol [Bristol], University of Bern, Universidad Complutense de Madrid = Complutense University of 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), Centre for Research in Earth and Space Science [Toronto] (CRESS), York University [Toronto], Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Belgian Science Policy Office, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Centre National de la Recherche Scientifique (France), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Roscosmos, Russian Government, Agenzia Spaziale Italiana, European Space Agency, IMPEC - 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), École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), The Open University [Milton Keynes] (OU), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Université Libre de Bruxelles [Bruxelles] (ULB), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Polska Akademia Nauk (PAN), Royal Observatory of Belgium [Brussels], Universidad Complutense de Madrid [Madrid] (UCM), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), University of Oxford, Agence Spatiale Européenne = European Space Agency (ESA), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), 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), and 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)

Subjects
Martian, Multidisciplinary, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010504 meteorology & atmospheric sciences, Chemistry, Atmosphere of Mars, Mars Exploration Program, 01 natural sciences, 7. Clean energy, Methane, Trace gas, law.invention, Astrobiology, Atmosphere, Orbiter, chemistry.chemical_compound, 13. Climate action, law, Atmospheric chemistry, 0103 physical sciences, 010303 astronomy & astrophysics, Sciences exactes et naturelles, 0105 earth and related environmental sciences
Abstract

A publisher correction to this article was published on 17 April 2019, The detection of methane on Mars has been interpreted as indicating that geochemical or biotic activities could persist on Mars today1. A number of different measurements of methane show evidence of transient, locally elevated methane concentrations and seasonal variations in background methane concentrations2–5. These measurements, however, are difficult to reconcile with our current understanding of the chemistry and physics of the Martian atmosphere6,7, which—given methane’s lifetime of several centuries—predicts an even, well mixed distribution of methane1,6,8. Here we report highly sensitive measurements of the atmosphere of Mars in an attempt to detect methane, using the ACS and NOMAD instruments onboard the ESA-Roscosmos ExoMars Trace Gas Orbiter from April to August 2018. We did not detect any methane over a range of latitudes in both hemispheres, obtaining an upper limit for methane of about 0.05 parts per billion by volume, which is 10 to 100 times lower than previously reported positive detections2,4. We suggest that reconciliation between the present findings and the background methane concentrations found in the Gale crater4 would require an unknown process that can rapidly remove or sequester methane from the lower atmosphere before it spreads globally. © 2019, The Author(s), under exclusive licence to Springer Nature Limited., ExoMars is the space mission of ESA and Roscosmos. The ACS experiment is led by IKI, the Space Research Institute in Moscow, assisted by LATMOS in France. The project acknowledges funding by Roscosmos and CNES. The science operations of ACS are funded by Roscosmos and ESA. IKI affiliates acknowledge funding under grant number 14.W03.31.0017 and contract number 0120.0 602993 (0028-2014-0004) of the Russian government. The NOMAD experiment is led by the Royal Belgian Institute for Space Aeronomy (BIRA-IASB), assisted by co-PI teams from Spain (IAA-CSIC), Italy (INAF-IAPS), and the UK (Open University). This project acknowledges funding by the Belgian Science Policy Office (BELSPO), with the financial and contractual coordination of the ESA Prodex Office (PEA 4000103401 and PEA 4000121493), by Spanish MICINN through its Plan Nacional and by European funds under grants ESP2015-65064-C2-1-P and ESP2017-87143-R (MINECO/FEDER), as well as by the UK Space Agency through grants ST/R005761/1, ST/P001262/1, ST/R001405/1, ST/S00145X/1, ST/R001367/1, ST/P001572/1 and ST/R001502/1, and the Italian Space Agency through grant 2018-2-HH.0. This work was supported by the Belgian Fonds de la Recherche Scientifique-FNRS under grant number 30442502 (ET_HOME).

Published
2019
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275. Assyrians and Babylonians in Classical Sources

Author

Fink, Sebastian, Droß-Krüpe, Kerstin, Da Riva, Rocío, Lang, Martin, Fink , Sebastian, Department of Cultures, Centre of Excellence in Ancient Near Eastern Empires (ANEE), and Centre of Excellence Changes in Sacred Texts and Traditions (CSTT)

Subjects
education, 615 History and Archaeology
Published
2019

276. NOMAD, an Integrated Suite of Three Spectrometers for the ExoMars Trace Gas Mission: Technical Description, Science Objectives and Expected Performance

Author

Vandaele, Ann Carine, López-Moreno, José Juan, Patel, Manish R., Bellucci, Giancarlo, Daerden, Frank, Ristic, Bojan, Robert, S., Thomas, Ian R., Wilquet, V., Allen, M., Alonso-Rodrigo, G., Altieri, F., Aoki, Shohei, Bolsée, D., Clancy, T., Cloutis, E., Depiesse, C., Drummond, R., Fedorova, A., Formisano, V., Funke, Bernd, González-Galindo, F., Geminale, A., Gérard, Jean-Claude, Giuranna, M., Hetey, L., Ignatiev, N., Kaminski, J., Karatekin, O., Kasaba, Y., Leese, M., Lefèvre, F., Lewis, S. R., López-Puertas, Manuel, López-Valverde, M. A., Mahieux, A., Mason, J., McConnell, J., Mumma, M., Neary, L., Neefs, E., Renotte, E., Rodriguez-Gomez, J., Sindoni, G., Smith, M., Stiepen, A., Trokhimovsky, A., Vander Auwera, J., Villanueva, Geronimo L., Viscardy, S., Whiteway, J., Willame, Y., Wolff, Michael T., Patel, M., D’aversa, E., Fussen, D., García Comas, Maia, Hewson, W., McConnel, J., Novak, R., Oliva, F., Piccialli, A., Aparicio del Moral, Beatriz, Barzin, P., BenMoussa, A., Berkenbosch, S., Biondi, D., Bonnewijn, S., Candini, G. P., Clairquin, R., Cubas, J., De-Lanoye, S., Giordanengo, B., Gissot, S., Gomez, A., Maes, J., Mazy, E., Mazzoli, A., Meseguer, J., Morales, Rafael, Orban, A., Pastor, Carmen, Perez-Grande, I., Queirolo, C., Saggin, B., Samain, V., Sanz Andres, A., Sanz Mesa, Rosario, Simar, J.-F., Thibert, T., Jerónimo, José María, The NOMAD Team, Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Space Science and Technology Department [Didcot] (RAL Space), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC)-Science and Technology Facilities Council (STFC), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Instituto Universitario de Microgravedad 'Ignacio Da Riva' (IDR), Universidad Politécnica de Madrid (UPM), Space Science Institute [Boulder] (SSI), Department of Geography [Winnipeg], University of Winnipeg, Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Institute of Geophysics [Warsaw], Polska Akademia Nauk = Polish Academy of Sciences (PAN), Royal Observatory of Belgium [Brussels] (ROB), Tohoku University [Sendai], PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (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), Fonds National de la Recherche Scientifique [Bruxelles] (FNRS), York University [Toronto], NASA Goddard Space Flight Center (GSFC), Centre Spatial de Liège (CSL), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Service de Chimie Quantique et Photophysique, Université libre de Bruxelles (ULB), Catholic University of America, Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Agenzia Spaziale Italiana, and Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles)

Subjects
010504 meteorology & atmospheric sciences, Solar occultation, education, Physique atomique et moléculaire, Exploration of Mars, 01 natural sciences, Occultation, law.invention, Orbiter, Mars atmosphere, law, 0103 physical sciences, Nadir, Chimie, natural sciences, 010303 astronomy & astrophysics, Spectroscopy, 0105 earth and related environmental sciences, Remote sensing, Ultraviolet, Martian, Astronomy and Astrophysics, Dust, Atmosphere of Mars, Mars Exploration Program, Nadir observations, ExoMars, Trace gas, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Spectroscopie [électromagnétisme, optique, acoustique], 13. Climate action, Space and Planetary Science, Visible, Environmental science, Infrared, Methane, Composition
Abstract

Open Access This article is distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), The NOMAD (“Nadir and Occultation for MArs Discovery”) spectrometer suite on board the ExoMars Trace Gas Orbiter (TGO) has been designed to investigate the composition of Mars’ atmosphere, with a particular focus on trace gases, clouds and dust. The detection sensitivity for trace gases is considerably improved compared to previous Mars missions, compliant with the science objectives of the TGO mission. This will allow for a major leap in our knowledge and understanding of the Martian atmospheric composition and the related physical and chemical processes. The instrument is a combination of three spectrometers, covering a spectral range from the UV to the mid-IR, and can perform solar occultation, nadir and limb observations. In this paper, we present the science objectives of the instrument and explain the technical principles of the three spectrometers. We also discuss the expected performance of the instrument in terms of spatial and temporal coverage and detection sensitivity.© 2018, The Author(s)., The NOMAD experiment is led by the Royal Belgian Institute for Space Aeronomy (IASB-BIRA), assisted by Co-PI teams from Spain (IAA-CSIC), Italy (INAF-IAPS), and the United Kingdom (Open University). This project acknowledges funding by the Belgian Science Policy Office (BELSPO), with the financial and contractual coordination by the ESA Prodex Office (PEA 4000103401, 4000121493), by Spanish MICINN through its Plan Nacional and by European funds under grant ESP2015-65064-C2-1-P (MINECO/FEDER), as well as by UK Space Agency through grants ST/R005761/1, ST/P001262/1, ST/R001405/1 and ST/R001405/1 and Italian Space Agency through grant 2018-2-HH.0. The research was performed as part of the >Excellence of Science> project >Evolution and Tracers of Habitability on Mars and the Earth> (30442502). SA acknowledge support from the FNRS, Be.

Published
2018
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277. Observations of Comet 9P/Tempel 1 around the Deep Impact event by the OSIRIS cameras onboard Rosetta

Author

HORST UWE KELLER, Michael, Kppers, Sonia, Fornasier, Gutierrez, PEDRO J., Hviid, STUBBE F., Laurent, Jorda, Jrg, Knollenberg, Lowry, STEPHEN C., Miriam, Rengel, Bertini, Ivano, Gabriele, Cremonese, WING H., Ip, Detlef, Koschny, Rainer, Kramm, Ekkehard, Khrt, Luisa, Maria, Lara, Holger, Sierks, Nicolas, Thomas, Barbieri, Cesare, Philippe, Lamy, Hans, Rickman, Rafael, Rodrigo, Ahearn, MICHAEL F., Francesco, Angrilli, MARIA ANTONELLA BARUCCI, Jean, Loup, Bertaux, VANIA DA DEPPO, Davidsson, BJRN J. R., MARIOLINO DE CECCO, Debei, Stefano, Marco, Fulle, Fritz, Gliem, Olivier, Groussin, LOPEZ MORENO, JOS J., Marzari, Francesco, Naletto, Giampiero, Lola, Sabau, ANGEL SANZ ANDRS, KLAUS PETER WENZEL, Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Università degli Studi di Padova = University of Padua (Unipd), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), 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), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Astrophysics Research Centre [Belfast] (ARC), Queen's University [Belfast] (QUB), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Institute of Space Science [Taiwan], National Central University [Taiwan] (NCU), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE), Department of Astronomy and Space Physics [Uppsala], Uppsala University, Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, Dipartimento di Ingegneria Meccanica [Padova], 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), Department of Information Engineering [Padova] (DEI), Università degli Studi di Trento (UNITN), INAF - Osservatorio Astronomico di Trieste (OAT), Institut für Datentechnik und Kommunikationsnetze, Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Dipartimento di Fisica e Astronomia 'Galileo Galilei', Instituto Nacional de Técnica Aeroespacial (INTA), Instituto de Microgravedad 'Ignacio Da Riva', and Universidad Politécnica de Madrid (UPM)

Subjects
Solar System, 010504 meteorology & atmospheric sciences, TELESCOPE, Comet, Narrow angle, coma, impact processes, surfaces, Osiris, 01 natural sciences, Aeronáutica, Comet Tempel-1, Comets, Impact processes, 0103 physical sciences, comets, RATES, Comets, coma, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, COMET-9P/TEMPEL-1, biology, Spacecraft, business.industry, Astronomy, Astronomy and Astrophysics, biology.organism_classification, Light curve, Astronomía, DUST ENVIRONMENT, [SDU]Sciences of the Universe [physics], 13. Climate action, Space and Planetary Science, dust, ATMOSPHERES, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

17 pp.-- Final full-text version of the paper available at: http://dx.doi.org/10.1016/j.icarus.2006.09.023., The OSIRIS cameras on the Rosetta spacecraft observed Comet 9P/Tempel 1 from 5 days before to 10 days after it was hit by the Deep Impact projectile. The Narrow Angle Camera (NAC) monitored the cometary dust in 5 different filters. The Wide Angle Camera (WAC) observed through filters sensitive to emissions from OH, CN, Na, and OI together with the associated continuum. Before and after the impact the comet showed regular variations in intensity. The period of the brightness changes is consistent with the rotation period of Tempel 1. The overall brightness of Tempel 1 decreased by about 10% during the OSIRIS observations. The analysis of the impact ejecta shows that no new permanent coma structures were created by the impact. Most of the material moved with ~ 200 m/s. Much of it left the comet in the form of icy grains which sublimated and fragmented within the first hour after the impact. The light curve of the comet after the impact and the amount of material leaving the comet (4.5 - 9 x 10e6 of water ice and a presumably larger amount of dust) suggest that the impact ejecta were quickly accelerated by collisions with gas molecules. Therefore, the motion of the bulk of the ejecta cannot be described by ballistic trajectories, and the validity of determinations of the density and tensile strength of the nucleus of Tempel 1 with models using ballistic ejection of particles is uncertain., The OSIRIS imaging system on board Rosetta is managed by the Max-Planck-Institute for Solar System Research in Katlenburg-Lindau (Germany), thanks to an International collaboration between Germany, France, Italy, Spain, and Sweden. We acknowledge the funding of the national space agencies ASI, CNES, DLR, the Spanish Space Program (Ministerio de Educacion y Ciencia), SNSB and ESA. IRAF is distributed by the National Optical Astronomy Observatories, which is operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation. We acknowledge JPL's Horizons online ephemeris generator for providing the comet's position and rate of motion during the observations. This research has made use of NASA's Astrophysics Data System.

Published
2007
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278. Hidrostática de la zona flotante

Author

Martínez Herranz, Isidoro and Da Riva de la Cavada, Ignacio

Subjects
Mecánica, Aeronáutica
Abstract

El comportamiento de masas líquidas en ingravidez es sorprendente; su estudio, complicado. Desde el siglo pasado se viene estudiando de un modo teórico el comportamiento de masas líquidas aisladas (principalmente impulsado por la astrofísica) y el de masas líquidas mantenidas entre dos superficies sólidas o "zonas flotantes" (impulsado por la tecnología de purificación de metales semiconductores por crecimiento cristalino). A primeros de los años 70 y en el marco de las posibilidades que se abrían en Europa para la experimentación en ingravidez con el proyecto de laboratorio espacial SPACELAB, el Profesor Da Riva se interesó en el estudio de las zonas líquidas flotantes. Al finalizar mis estudios de ingeniería en 1975 y habiendo ya trabajado más de un año bajo su dirección, pasé a colaborar en estas investigaciones. El trabajo en estos dos años y medio ha sido importante: producción de una película documental sobre el comportamiento de las zonas flotantes (Febrero 76), presentación de un artículo en el 2o Simposium de Ciencia de los Materiales en el Espacio (Italia, Abril 76), presentación de un artículo en la XX Asamblea Plenaria de la COSPAR (Israel, Junio 77), conferencias, etc. El campo que abarcan estos estudios es muy amplio: hidrostática de las zonas flotantes, movimientos forzados, movimientos libres, experimentación en ingravidez, simulación en tierra, etc. Algunas importantes conclusiones derivadas del análisis de la hidrostática (equilibrio y estabilidad estática) han dado origen a esta Tesis, en donde se ha tratado de completar dichos hallazgos con un estudio más ordenado y metódico de la hidrostática de las zonas flotantes. Si hubiera que señalar el logro más importante que presenta esta Tesis, apuntaríamos que tal vez sea el de mostrar que no era acertado el criterio de estabilidad de las formas no cilíndricas (en particular la zona catenoide) que se suponía antes. Estos estudios se continuarán y tratarán de proporcionar una teoría que sirva para la interpretación de los experimen tos que se van a realizar en la Primera Misión Spacelab (1980) y que permita asesorar a los utilizadores de zonas flotantes a la par que profundizar en el conocimiento de la mecánica de líquidos

Published
1978

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