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28 results on '"R. Trautner"'

1. Dynamics of Subsurface Migration of Water on the Moon

Author

P. Reiss, R. Trautner, Elliot Sefton-Nash, and Tristram Warren

Subjects
Lunar water, Geophysics, Resource (biology), Space and Planetary Science, Geochemistry and Petrology, Earth science, Earth and Planetary Sciences (miscellaneous), Environmental science
Published
2021

2. The Oxford 3D thermophysical model with application to PROSPECT/Luna 27 study landing sites

Author

O. G. King, Neil Bowles, R. Trautner, Elliot Sefton-Nash, Tristram Warren, and Richard Fisackerly

Subjects
Radiometer, 010504 meteorology & atmospheric sciences, Scattering, Astronomy and Astrophysics, Exponential density, Atmospheric sciences, 01 natural sciences, Stability (probability), law.invention, Orbiter, Impact crater, Space and Planetary Science, law, 0103 physical sciences, Thermal model, 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences, Diviner
Abstract

A 3D thermal model that includes a discrete subsurface exponential density profile, surface shadowing and scattering effects has been developed to simulate surface and subsurface temperatures across the Moon. Comparisons of the modelled surface temperatures with the Lunar Reconnaissance Orbiter’s Diviner Lunar Radiometer Experiment (“Diviner”) measured temperatures show significant improvements in model accuracy from the inclusion of shadowing and scattering effects, with model errors reduced from ~10 K to ~2 K for mid-latitude craters. The 3D thermal model is used to investigate ice stability at potential landing sites near the lunar south pole, studied for Roscosmos’ ‘Luna Resource’ (Luna 27) lander mission on which the ESA PROSPECT payload is planned to fly. Water ice is assumed to be stable for long periods of time (>1 Gyr) if temperatures remain below 112 K over diurnal and seasonal cycles. Simulations suggest ice can be stable at the surface in regions near to potential landing sites in permanently shaded regions and can be stable below the surface in partly shaded regions such as pole-facing slopes. The simulated minimum constant subsurface temperature (where the seasonal temperature cycle is attenuated) typically occurs at a depth of ~50 cm and therefore the minimum depth where ice can be stable is A 3D thermal model that includes a discrete subsurface exponential density profile, surface shadowing and scattering effects has been developed to simulate surface and subsurface temperatures across the Moon. Comparisons of the modelled surface temperatures with the Lunar Reconnaissance Orbiter’s Diviner Lunar Radiometer Experiment (“Diviner”) measured temperatures show significant improvements in model accuracy from the inclusion of shadowing and scattering effects, with model errors reduced from ~10 K to ~2 K for mid-latitude craters. The 3D thermal model is used to investigate ice stability at potential landing sites near the lunar south pole, studied for Roscosmos’ ‘Luna Resource’ (Luna 27) lander mission on which the ESA PROSPECT payload is planned to fly. Water ice is assumed to be stable for long periods of time (>1 Gyr) if temperatures remain below 112 K over diurnal and seasonal cycles. Simulations suggest ice can be stable at the surface in regions near to potential landing sites in permanently shaded regions and can be stable below the surface in partly shaded regions such as pole-facing slopes. The simulated minimum constant subsurface temperature (where the seasonal temperature cycle is attenuated) typically occurs at a depth of ~50 cm and therefore the minimum depth where ice can be stable is 0

Published
2020

3. Mechanism of subwavelength imaging with bilayered magnetic metamaterials: Theory and experiment

Author

Laszlo Solymar, Grahame Faulkner, R. Trautner, A. Radkovskaya, Ekaterina Shamonina, Oleksiy Sydoruk, Mikhail Shamonin, David J. Edwards, Christopher J. Stevens, and O. Zhuromskyy

Subjects
Physics, Superlens, business.industry, Physics::Optics, General Physics and Astronomy, Metamaterial, Inductive coupling, Electromagnetic radiation, law.invention, Magnetic field, Lens (optics), Wavelength, Resonator, Optics, law, Optoelectronics, business
Abstract

We present a theoretical and experimental study of a bilayered metamaterial structure for subwavelength imaging of magnetic field. The simplest version of such a structure consists of one or two linear arrays of capacitively loaded split pipe resonators. Its subwavelength physics is governed by strongly anisotropic magnetic coupling between individual resonators and by propagation of magnetoinductive waves with wavelength much shorter than the wavelength of the electromagnetic radiation in free space. It is shown that magnetoinductive waves propagating in the lateral direction are undesirable because they spread the image. Good subwavelength imaging is achieved when, due to the strong interlayer coupling, a stop band in the vicinity of the resonant frequency appears in the dispersion characteristics. The imaging properties of the single and double lens are compared and it is shown that the double lens has a superior performance. Excellent agreement is obtained between experimental and theoretical results for the magnetic field in the image plane in the operation frequency range of 30-60 MHz. It is shown that the same mechanism is responsible for image formation using bilayered planar metamaterial structures and a design of such a lens comprising two planar layers with a total of 542 elements is provided. The conclusions are not restricted to the radio frequency region because the elements can be scaled down. © 2007 American Institute of Physics.

Published
2016

4. Observations of the surface of Titan by the Radar Altimeters on the Huygens Probe

Author

Håkan Svedhem, Nicolas Floury, Ralph D. Lorenz, J.-P. Lebreton, Wlodek Kofman, Alain Herique, Olivier Witasse, Francesca Ferri, R. Trautner, Dirk Plettemeier, Peter Falkner, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), ESA/ESTEC, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), 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]), Technische Universität Dresden = Dresden University of Technology (TU Dresden), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), 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 d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-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 d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), and Universita degli Studi di Padova

Subjects
010504 meteorology & atmospheric sciences, Astronomy and Astrophysics, Terrain, 01 natural sciences, Planetary Data System, Space-based radar, law.invention, Radar observations, symbols.namesake, Amplitude, Intermediate frequency, Space and Planetary Science, law, [SDU]Sciences of the Universe [physics], 0103 physical sciences, symbols, Altimeter, Radar, Titan (rocket family), Titan, 010303 astronomy & astrophysics, Instrumentation, Geology, 0105 earth and related environmental sciences, Remote sensing
Abstract

International audience; Results from the radar altimeters on board the Huygens probe are reported, noting the content of data archived on the NASA Planetary Data System and its ESA counterpart. These instruments provide unique high-resolution information on the topography and electrical properties of the Titan surface over a ∼15 km track across a boundary between a bright highland and the dark dissected alluvial terrain on which the probe landed. The highland appears ∼100 m higher than the dark terrain. The dark terrain has a fairly high nadir radar backscatter, consistent with terrestrial lakebeds and alluvial surfaces, and shows small (5–10 m) elevation fluctuations. Possible signatures of surface or volume scattering in the backscatter amplitude and intermediate frequency spectrum are discussed. A previously-undocumented characteristic of the Automatic Gain Control (AGC) on the flight altimeter is noted.

Published
2016

5. Herstellung und Charakterisierung eines extrinsischen faseroptischen Elementarsensors zur Temperaturmessung Manufacture and Characterization of an Extrinsic Elementary Fiber-Optical Sensor for Temperature Measurement

Author

Bernhard Schmaus, R. Trautner, and Mikhail Shamonin

Subjects
chemistry.chemical_compound, Materials science, chemistry, business.industry, Indium phosphide, Optoelectronics, Fiber, Electrical and Electronic Engineering, business, Instrumentation, Temperature measurement, Characterization (materials science)
Abstract

Zusammenfassung Es werden Herstellung und Charakterisierung eines faseroptischen Elementarsensors zur Temperaturmessung vorgestellt. Der Sensorkopf in Form eines Prismas aus Indiumphosphid nutzt die Temperaturabhängigkeit der Absorptionskante des Halbleitermaterials. Aufgrund der Abmessungen des Prismas im Grenzbereich von Feinmechanik zu Mikrosystemtechnik ist ein angepasstes Herstellungsverfahren notwendig.

Published
2008

6. A new numerical model for the simulation of ELF wave propagation and the computation of eigenmodes in the atmosphere of Titan: Did Huygens observe any Schumann resonance?

Author

V. Brown, Peter Falkner, Fernando Simões, Bruno P. Besser, Marcello Fulchignoni, Rafael Rodrigo, Michel Hamelin, R. Trautner, R. Grard, Konrad Schwingenschuh, Francesca Ferri, Jean-Jacques Berthelier, R. Hofe, Håkan Svedhem, Irmgard Jernej, M. Chabassiere, C. Beghin, Tetsuya Tokano, Gregorio J. Molina-Cuberos, J. J. López-Moreno, and J. M. Jeronimo

Subjects
Physics, Schumann resonances, Wave propagation, Astronomy and Astrophysics, Geophysics, Electromagnetic radiation, symbols.namesake, Space and Planetary Science, Physics::Space Physics, symbols, Extremely low frequency, Astrophysics::Earth and Planetary Astrophysics, Atmospheric electricity, Ionosphere, Atmosphere of Titan, Titan (rocket family)
Abstract

The propagation of extremely low frequency (ELF) electromagnetic waves in the Earth's ionospheric cavity and the associated resonance phenomena have been extensively studied, in relation with lightning activity. We perform a similar investigation for Titan, the largest moon of Saturn. There are important differences between Earth and Titan, as far as the cavity geometry, the atmospheric electron density profile, and the surface conductivity are concerned. We present an improved 3D finite element model that provides an estimate of the lowest eigenfrequencies, associated quality factors (Q-factors), and ELF electric field spectra. The data collected by the electric antenna of the Permittivity, Waves, and Altimetry (PWA) instrument reveals the existence of a narrow-band signal at about 36 Hz during the entire descent of Huygens upon Titan. We assess the significance of these measurements against the model predictions, with due consideration to the experimental uncertainties.

Published
2007

7. Multicore soc for on-board payload signal processing

Author

G.K. Rauwerda, Gerard J.M. Smit, Sabih H. Gerez, Karel H.G. Walters, R. Trautner, and S. Baillou

Subjects
POSIX Threads, Multi-core processor, Payload, Computer science, business.industry, Interface (computing), EWI-20430, IR-77933, SpaceWire, Network on a chip, Embedded system, METIS-278866, User interface, Field-programmable gate array, business
Abstract

This paper introduces a new generic platform for onboard payload signal processing. The system is built up around an NoC with a bridge to an AMBA system which supports easy integration with existing AMBA based platforms. With the use of a pthreads interface the platform allows for simple programming and easy extension. For prototyping purposes, an implementation has been made on an FPGA together with a range of I/O options to assess its capabilities. SpaceWire and other interfaces support the extension of the demonstrator platform across multiple boards and allow to connect it to onboard networks and systems. This paper shows that novel and established chip architectures can be integrated in a way that combines their benefits, and represents a promising candidate architecture for future on-board processing platforms.

Published
2011

8. Rosetta Lander ('Philae') Investigations

Author

J.-P. Bibring, H. Rosenbauer, H. Boehnhardt, S. Ulamec, J. Biele, S. Espinasse, B. Feuerbacher, P. Gaudon, P. Hemmerich, P. Kletzkine, D. Moura, R. Mugnuolo, G. Nietner, B. Pätz, R. Roll, H. Scheuerle, K. Szegö, K. Wittmann, Philae team, G. Klingelhöfer, J. Brückner, C. d’Uston, R. Gellert, R. Rieder, J. Gironés López, P. Lamy, Y. Langevin, A. Soufflot, M. Berthé, J. Borg, F. Poulet, S. Mottola, Fred Goesmann, Helmut Rosenbauer, Reinhard Roll, Cyril Szopa, Francois Raulin, Robert Sternberg, Guy Israel, Uwe Meierhenrich, Wolfram Thiemann, Guillermo Munoz-Caro, Tilman Spohn, Karsten Seiferlin, Axel Hagermann, Jörg Knollenberg, Andrew J. Ball, Doris Breuer, Marek Banaszkiewicz, Johannes Benkhoff, Stanislaw Gadomski, Wojciech Gregorczyk, Jerzy Grygorczuk, Marek Hlond, Günter Kargl, Ekkehard Kührt, Norbert Kömle, Konrad Kossacki, Jacek Krasowski, Wojciech Marczewski, John C. Zarnecki, A. D. Morse, G. H. Morgan, D. J. Andrews, S. J. Barber, M. R. Leese, S. Sheridan, I. P. Wright, C. T. Pillinger, Stefano Mottola, Gabriele Arnold, Hans-Georg Grothues, Ralf Jaumann, Harald Michaelis, Gerhard Neukum, Jean-Pierre Bibring, H.U. Auster, I. Apathy, G. Berghofer, A. Remizov, K.H. Fornacon, K.H. Glassmeier, G. Haerendel, I. Hejja, E. Kührt, W. Magnes, D. Moehlmann, U. Motschmann, I. Richter, C.T. Russell, J. Rustenbach, K. Sauer, K. Schwingenschuh, I. Szemerey, R. Waesch, F. Bernelli Zazzera, P. Bologna, C. Dainese, A. Ercoli Finzi, P.G. Magnani, F. Malnati, A. Olivieri, E. Re, K. J. Seidensticker, D. Möhlmann, W. Schmidt, K. Thiel, W. Arnold, H.-H. Fischer, M. Kretschmer, A. Péter, R. Trautner, and S. Schieke

Published
2009

9. Structure of Titan's low altitude ionized layer from the Relaxation Probe onboard HUYGENS

Author

Irmgard Jernej, Rafael Rodrigo, J. J. López-Moreno, Francesca Ferri, R. Trautner, Gregorio J. Molina-Cuberos, Michel Hamelin, C. Beghin, Jean-Jacques Berthelier, V. Brown, Peter Falkner, Konrad Schwingenschuh, Fernando Simões, R. Godard, J. M. Jeronimo, M. Fulchignoni, R. Grard, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Facultad de Química [Murcia], Universidad de Murcia, Centre d'étude des environnements terrestre et planétaires (CETP), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Research and Scientific Support Department, ESTEC (RSSD), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Department of Mathematics and Computer Science, Royal Military College of Canada, Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Laboratoire de physique et chimie de l'environnement (LPCE), Institut national des sciences de l'Univers (INSU - CNRS)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Università degli Studi di Padova = University of Padua (Unipd), 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), Ministerio de Ciencia y Tecnologı ́a, Spain (contractsESP2003-00357 and ESP2006-02934), European Space Agency (ESA)-European Space Agency (ESA), Université d'Orléans (UO)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Universita degli Studi di Padova

Subjects
010504 meteorology & atmospheric sciences, Cosmic ray, Electron, Cassini-Huygens, 01 natural sciences, Ion, symbols.namesake, Ionization, 0103 physical sciences, Altimeter, Atmosphere of Titan, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, Physics, Geophysics, Computational physics, 13. Climate action, Physics::Space Physics, symbols, General Earth and Planetary Sciences, conductivity, Ionosphere, Titan, Titan (rocket family)
Abstract

International audience; Some of the secrets of the atmosphere of Titan have been unveiled by the Huygens Probe. The Permitivity Wave and Altimetry system detected a hidden ionosphere much below the main ionosphere, that lies between 600 and 2000 km. Theoretical models predicted a low altitude ionosphere produced by cosmic rays that, contrary to magnetospheric particles and UV photons, are able to penetrate down in the atmosphere. Two sensors: Mutual Impedance (MI) and Relaxation Probe (RP) measured the conductivity of the ionosphere by two different methods and were able to discriminate the two branches of electrical conductivity due to the positive and negative charges. The measurements were made from 140 to 40 km and show a maximum of charge densities ≈2 × 109 m−3 positive ions and ≈450 × 106 m−3 electrons at around 65 km. Here we present the altitude distribution of the concentration of positive ions and electrons obtained from the RP and MI sensors.

Published
2008

10. Electron conductivity and density profiles derived from the mutual impedance probe measurements performed during the descent of Huygens through the atmosphere of Titan

Author

Francesca Ferri, Fernando Simões, C. Beghin, Tetsuya Tokano, Gregorio J. Molina-Cuberos, Michel Chabassière, Marcello Fulchignoni, Rafael Rodrigo, Konrad Schwingenschuh, V. Brown, Peter Falkner, Irmgard Jernej, Michel Hamelin, J. J. López-Moreno, J. M. Jeronimo, Jean-Jacques Berthelier, R. Grard, R. Trautner, Centre d'étude des environnements terrestre et planétaires (CETP), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique et chimie de l'environnement (LPCE), Université d'Orléans (UO)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Research and Scientific Support Department, ESTEC (RSSD), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA)-European Space Agency (ESA), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Universita degli Studi di Padova, 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), Departamento de Física [Murcia], Universidad de Murcia, Institut für Geophysik und Meteorologie [Köln], Universität zu Köln, Institut national des sciences de l'Univers (INSU - CNRS)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Università degli Studi di Padova = University of Padua (Unipd), and Universität zu Köln = University of Cologne

Subjects
Permittivity, Electron density, 010504 meteorology & atmospheric sciences, Atmospheric conductivity, Electron, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, Optics, [PHYS.PHYS.PHYS-PLASM-PH]Physics [physics]/Physics [physics]/Plasma Physics [physics.plasm-ph], Ionization, 0103 physical sciences, Altimeter, Atmosphere of Titan, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Huygens probe, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], business.industry, Astronomy and Astrophysics, Atmospheric electricity, Space and Planetary Science, symbols, Titan (rocket family), business, Titan
Abstract

During the descent of the Huygens probe through the atmosphere of Titan, on January 14th, 2005, the permittivity, waves and altimetry (PWA) subsystem, a component of the Huygens atmospheric structure instrument (HASI), detected an ionized layer at altitudes around 63 km with two different instruments, the relaxation probe (RP) and the mutual impedance probe (MIP). A very detailed analysis of both data sets is required, in order to correct for environmental effects and compare the two independent estimates of the electrical conductivity. The present work is dedicated to the MIP data analysis. New laboratory tests have been performed to validate or improve the available calibration results. Temperature effects have been included and numerical models of the MIP sensors and electric circuitry have been developed to take into account the proximity of the Huygens probe body. The effect of the vertical motion of the vessel in the ionized atmosphere is estimated in both analytical and numerical ways. The peculiar performance of the instrument in the altitude range 100–140 km is scrutinized. The existence of a prominent ionized layer, and of enhancements in the conductivity and electron density profiles at 63 km, are discussed in the light of previous theoretical predictions.

Published
2007

12. Electric properties and related physical characteristics of the atmosphere and surface of Titan

Author

Fernando Simões, Jean-Jacques Berthelier, Irmgard Jernej, Michel Hamelin, Tetsuya Tokano, R. Grard, V. Brown, J. M. Jeronimo, M. Chabassiere, Peter Falkner, Francesca Ferri, Håkan Svedhem, Marcello Fulchignoni, J. J. López-Moreno, Rafael Rodrigo, R. Trautner, C. Beghin, Konrad Schwingenschuh, L. M. Lara, Gregorio J. Molina-Cuberos, Research and Scientific Support Department, ESTEC (RSSD), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA)-European Space Agency (ESA), Centre d'étude des environnements terrestre et planétaires (CETP), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Departamento de Física [Murcia], Universidad de Murcia, Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Universita degli Studi di Padova, 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), Laboratoire de physique et chimie de l'environnement (LPCE), Université d'Orléans (UO)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut für Geophysik und Meteorologie [Köln], Universität zu Köln, Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Università degli Studi di Padova = University of Padua (Unipd), Institut national des sciences de l'Univers (INSU - CNRS)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), and Universität zu Köln = University of Cologne

Subjects
Permittivity, Materials science, 010504 meteorology & atmospheric sciences, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Relative permittivity, Astronomy and Astrophysics, Geophysics, 01 natural sciences, Computational physics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, 13. Climate action, Space and Planetary Science, Electrical resistivity and conductivity, [PHYS.PHYS.PHYS-PLASM-PH]Physics [physics]/Physics [physics]/Plasma Physics [physics.plasm-ph], Electric field, 0103 physical sciences, symbols, Atmospheric electricity, Atmosphere of Titan, Ionosphere, Titan (rocket family), 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

The permittivity, waves and altimetry (PWA) instrument was designed for the investigation of the electric properties and other related physical characteristics of the atmosphere of Titan, from an altitude around 140 km down to the surface. PWA carried sensors to measure the atmospheric conductivity, and record electromagnetic and acoustic waves up to frequencies of 11.5 and 6.7 kHz, respectively. PWA also measured the relief roughness during the descent and the permittivity of the surface after touchdown. The measurements and the results of the preliminary analysis are presented. An ionized layer is detected at altitudes above 50 km, using two independent techniques, and the presence of free electrons in the upper atmosphere is confirmed. An electric signal at around 36 Hz is observed throughout the descent, but it is not yet confirmed that this emission is unambiguously related to a resonance of the ionospheric cavity. The relative dielectric constant of Titan's surface material is nearly 2 and the electric conductivity 4×10−10 S m−1. The electric properties of the surface seem to evolve after touch-down, possibly due to a local warming of the landing site by the Huygens Probe body.

Published
2006

13. In situ measurements of the physical characteristics of Titan’s environment

Author

Enrico Flamini, Ari-Matti Harri, Martin C. Towner, R. Trautner, Irmgard Jernej, M. A. Barucci, Francesca Ferri, Athena Coustenis, Giacomo Colombatti, Michel Hamelin, Tetsuya Tokano, Christopher P. McKay, Valerio Pirronello, William J. Borucki, Gregorio J. Molina-Cuberos, A. Lehto, Mark Leese, R. Grard, Francesco Angrilli, G. Bianchini, Giulio Fanti, Håkan Svedhem, Akiva Bar-Nun, T. Mäkinen, B. Hathi, Bortolino Saggin, Andrew J. Ball, P. F. Lion Stoppato, C. Bettanini, V. Gaborit, M. Coradini, Marcello Fulchignoni, J. J. López-Moreno, Rafael Rodrigo, Peter Falkner, Alvin Seiff, Fernando Simões, Paul Withers, John C. Zarnecki, J. A. M. McDonnell, Fritz M. Neubauer, Konrad Schwingenschuh, Stefano Debei, 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), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Università degli Studi di Padova = University of Padua (Unipd), Planetary and Space Sciences Research Institute [Milton Keynes] (PSSRI), Centre for Earth, Planetary, Space and Astronomical Research [Milton Keynes] (CEPSAR), The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Department of Geophysical, Atmospheric and Planetary Sciences [Tel Aviv] (TAU), Tel Aviv University (TAU), NASA Ames Research Center (ARC), Agence Spatiale Européenne = European Space Agency (ESA), European Space Research and Technology Centre (ESTEC), Agenzia Spaziale Italiana (ASI), Centre d'étude des environnements terrestre et planétaires (CETP), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Finnish Meteorological Institute (FMI), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Departamento de Física [Murcia], Universidad de Murcia, Institut für Geophysik und Meteorologie [Köln], Universität zu Köln = University of Cologne, Università degli studi di Catania = University of Catania (Unict), Politecnico di Milano [Milan] (POLIMI), Universita degli Studi di Padova, Department of Geophysics and Planetary Sciences [Tel Aviv], Tel Aviv University [Tel Aviv], Agence Spatiale Européenne (ESA), European Space Agency (ESA), Universität zu Köln, and Università degli studi di Catania [Catania]

Subjects
010504 meteorology & atmospheric sciences, chemistry.chemical_element, Atmospheric sciences, 01 natural sciences, Methane, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], chemistry.chemical_compound, symbols.namesake, Electrical resistivity and conductivity, [PHYS.PHYS.PHYS-PLASM-PH]Physics [physics]/Physics [physics]/Plasma Physics [physics.plasm-ph], 0103 physical sciences, Atmosphere of Titan, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Life on Titan, Multidisciplinary, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Medicine (all), Nitrogen, chemistry, 13. Climate action, symbols, Environmental science, Atmospheric electricity, Ionosphere, Titan (rocket family)
Abstract

On the basis of previous ground-based and fly-by information, we knew that Titan's atmosphere was mainly nitrogen, with some methane, but its temperature and pressure profiles were poorly constrained because of uncertainties in the detailed composition. The extent of atmospheric electricity ('lightning') was also hitherto unknown. Here we report the temperature and density profiles, as determined by the Huygens Atmospheric Structure Instrument (HASI), from an altitude of 1,400 km down to the surface. In the upper part of the atmosphere, the temperature and density were both higher than expected. There is a lower ionospheric layer between 140 km and 40 km, with electrical conductivity peaking near 60 km. We may also have seen the signature of lightning. At the surface, the temperature was 93.65 +/- 0.25 K, and the pressure was 1,467 +/- 1 hPa.

Published
2005

18. RATIO TAUBERIAN THEOREMS FOR LAPLACE TRANSFORMS WITHOUT MONOTONICITY ASSUMPTIONS

Author

R Trautner and Ulrich Stadtmüller

Subjects
Post's inversion formula, Laplace transform, Laplace principle, General Mathematics, Laplace transform applied to differential equations, Mathematical analysis, Two-sided Laplace transform, Inverse Laplace transform, Monotonic function, Mathematics, Abelian and tauberian theorems
Published
1985

20. An Inclusion Relation for Abel, Borel, and Lambert Summability

Author

Wolfgang Gawronski, R. Trautner, and H. Siebert

Subjects
Pure mathematics, Borel's lemma, General Mathematics, Calculus, Inclusion relation, Mathematics
Abstract

In this paper a new type of inclusion theorem concerning Abel, Borel and Lambert summability is established. To state our results we need some definitions and notations. With a formal series ∑k=0∞ak, ak∈ C, and its partial sums snwe associate the seriesThen ∑k=0∞ ak is said to be summable to the value s(a) by Abel's method, if (1.1) is convergent for |v| > 1 and limv→1+A(v)= s,(b) by Lambert's method, if (1.2) is convergent for |v| > 1 and limv→1+L(v)= s,(c) by Borel's method, if (1.3) is convergent for all x ∈ R and limx→+∞B(x)= s

Published
1980

22. ASYMPTOTIC BEHAVIOUR OF DISCRETE LINEAR PROCESSES

Author

R. Trautner and U. Stadtmüller

Subjects
Statistics and Probability, Discrete mathematics, Probability space, Law of large numbers, Applied Mathematics, Linear process, Order (group theory), Limit (mathematics), Statistics, Probability and Uncertainty, Central limit theorem, Mathematics
Abstract

We consider the linear process Yn(ω) =ΣAk(ω) ·Xn-k (ω) on a probability space (Ω, P) and ask for sufficient conditions in order to get a limit theorem for (Yk) if the corresponding limit theorem for (Xk) is true.

Published
1985

26. Habitability on Early Mars and the Search for Biosignatures with the ExoMars Rover.

Author

Vago JL, Westall F, Coates AJ, Jaumann R, Korablev O, Ciarletti V, Mitrofanov I, Josset JL, De Sanctis MC, Bibring JP, Rull F, Goesmann F, Steininger H, Goetz W, Brinckerhoff W, Szopa C, Raulin F, Westall F, Edwards HGM, Whyte LG, Fairén AG, Bibring JP, Bridges J, Hauber E, Ori GG, Werner S, Loizeau D, Kuzmin RO, Williams RME, Flahaut J, Forget F, Vago JL, Rodionov D, Korablev O, Svedhem H, Sefton-Nash E, Kminek G, Lorenzoni L, Joudrier L, Mikhailov V, Zashchirinskiy A, Alexashkin S, Calantropio F, Merlo A, Poulakis P, Witasse O, Bayle O, Bayón S, Meierhenrich U, Carter J, García-Ruiz JM, Baglioni P, Haldemann A, Ball AJ, Debus A, Lindner R, Haessig F, Monteiro D, Trautner R, Voland C, Rebeyre P, Goulty D, Didot F, Durrant S, Zekri E, Koschny D, Toni A, Visentin G, Zwick M, van Winnendael M, Azkarate M, and Carreau C

Abstract

The second ExoMars mission will be launched in 2020 to target an ancient location interpreted to have strong potential for past habitability and for preserving physical and chemical biosignatures (as well as abiotic/prebiotic organics). The mission will deliver a lander with instruments for atmospheric and geophysical investigations and a rover tasked with searching for signs of extinct life. The ExoMars rover will be equipped with a drill to collect material from outcrops and at depth down to 2 m. This subsurface sampling capability will provide the best chance yet to gain access to chemical biosignatures. Using the powerful Pasteur payload instruments, the ExoMars science team will conduct a holistic search for traces of life and seek corroborating geological context information. Key Words: Biosignatures-ExoMars-Landing sites-Mars rover-Search for life. Astrobiology 17, 471-510., Competing Interests: No competing financial interests exist.

Published
2017
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27. In situ measurements of the physical characteristics of Titan's environment.

Author

Fulchignoni M, Ferri F, Angrilli F, Ball AJ, Bar-Nun A, Barucci MA, Bettanini C, Bianchini G, Borucki W, Colombatti G, Coradini M, Coustenis A, Debei S, Falkner P, Fanti G, Flamini E, Gaborit V, Grard R, Hamelin M, Harri AM, Hathi B, Jernej I, Leese MR, Lehto A, Lion Stoppato PF, López-Moreno JJ, Mäkinen T, McDonnell JA, McKay CP, Molina-Cuberos G, Neubauer FM, Pirronello V, Rodrigo R, Saggin B, Schwingenschuh K, Seiff A, Simões F, Svedhem H, Tokano T, Towner MC, Trautner R, Withers P, and Zarnecki JC

Abstract

On the basis of previous ground-based and fly-by information, we knew that Titan's atmosphere was mainly nitrogen, with some methane, but its temperature and pressure profiles were poorly constrained because of uncertainties in the detailed composition. The extent of atmospheric electricity ('lightning') was also hitherto unknown. Here we report the temperature and density profiles, as determined by the Huygens Atmospheric Structure Instrument (HASI), from an altitude of 1,400 km down to the surface. In the upper part of the atmosphere, the temperature and density were both higher than expected. There is a lower ionospheric layer between 140 km and 40 km, with electrical conductivity peaking near 60 km. We may also have seen the signature of lightning. At the surface, the temperature was 93.65 +/- 0.25 K, and the pressure was 1,467 +/- 1 hPa.

Published
2005
Full Text
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28. CASH 2021: commercial access and space habitation.

Author

Aldrin A, Amara A, Aris L, Baierl N, Beatty P, Beaulieu C, Behnke T, Castegini R, Chauhan A, Cojanis P, Dayawansa P, Diop M, Eito K, Engle S, Feretti S, Gassama H, Genova B, Goulding C, Janjua J, Jansaeng T, Jousset F, Kopik A, Laurin C, Leggatt J, Li H, Mezzadri M, Miura A, Nolet S, Ogami S, Patry J, Patten L, Payerne C, Peer G, Prampolini M, Rheaume C, Saary J, Spehar D, Sufi A, Sun B, Thompson JB, Thomson W, Trautner R, Tursunmuratov M, Venet V, Wilems E, Wilson H, Wittwer K, Wokke F, Wu Y, Zhou S, and Zilioli I

Subjects
Agriculture economics, Biotechnology economics, Commerce economics, Forecasting, Humans, Industry, Marketing, Materials Testing, Research, Spacecraft, Technology Transfer, Commerce trends, Recreation, Space Flight economics, Space Flight trends, Weightlessness
Abstract

Issues about commercialization of space have been a growing concern in the past decade for the space community. This paper focuses on the work from a team of 51 students attending the Summer Session Program of the International Space University in Bremen, Germany. CASH 2021 (Commercial Access and Space Habitation) documents a plan that identifies commercial opportunities for space utilization that will extend human presence in space, and will chart the way forward for the next 20 years. The group selected four commercial sectors that show the most promise for the future: tourism, entertainment, space system service, assembly and debris removal, and research and development/production. The content of this document presents the results of their research. Historical activities in each of the commercial sectors are reviewed along with the current market situation. To provide a coherent background for future commercialization possibilities a scenario has been developed. This scenario includes a postulated upon ideal future and includes social, political and economic factors that may affect the space industry over the timeline of the study. The study also presents a roadmap, within the limited optimistic scenario developed, for the successful commercialization of space leading to future human presence in space. A broad range of commercially viable opportunities, not only within the current limits of the International Space Station, but also among the many new developments that are expected by 2021 are discussed., (c2002 International Astronautical Federation. Published by Elsevier Science Ltd. All rights reserved.)

Published
2002
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