Search

Your search keyword '"Rosenblatt, Pascal"' showing total 153 results
Start Over Author "Rosenblatt, Pascal"
153 results on '"Rosenblatt, Pascal"'

2. The formation of the Martian moons

Author

Rosenblatt, Pascal, Hyodo, Ryuki, Pignatale, Francesco C., Trinh, Antony, Charnoz, Sébastien, Dunseath, Kevin M., Terao-Dunseath, Mariko, and Genda, Hidenori

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Almost all the planets of our solar system have moons. Each planetary system has however unique characteristics. The Martian system has not one single big moon like the Earth, not tens of moons of various sizes like for the giant planets, but two small moons: Phobos and Deimos. How did form such a system? This question is still being investigated on the basis of the Earth-based and space-borne observations of the Martian moons and of the more modern theories proposed to account for the formation of other moon systems. The most recent scenario of formation of the Martian moons relies on a giant impact occurring at early Mars history and having also formed the so-called hemispheric crustal dichotomy. This scenario accounts for the current orbits of both moons unlike the scenario of capture of small size asteroids. It also predicts a composition of disk material as a mixture of Mars and impactor materials that is in agreement with remote sensing observations of both moon surfaces, which suggests a composition different from Mars. The composition of the Martian moons is however unclear, given the ambiguity on the interpretation of the remote sensing observations. The study of the formation of the Martian moon system has improved our understanding of moon formation of terrestrial planets: The giant collision scenario can have various outcomes and not only a big moon as for the Earth. This scenario finds a natural place in our current vision of the early solar system when conditions were favorable for giant collisions to occur. The next step in exploration of Martian moon is a sample return mission to test the giant collision scenario for their origin, and to provide tests of models of early solar system dynamics since Mars may retain material exchanged between the inner and outer solar system., Comment: 30 pages, 8 figures, 2 tables. Accepted for publication in the Oxford Research Encyclopedia of Planetary Science

Published
2019
Full Text
View/download PDF

3. On the Impact Origin of Phobos and Deimos IV: Volatile Depletion

Author

Hyodo, Ryuki, Genda, Hidenori, Charnoz, Sébastien, Pignatale, Francesco C., and Rosenblatt, Pascal

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Recent works have shown that Martian moons Phobos and Deimos may have accreted within a giant impact-generated disk whose composition is about an equal mixture of Martian material and impactor material. Just after the giant impact, the Martian surface is heated up to $\sim3000-6000$ K and the building blocks of moons, including volatile-rich vapor, are heated up to $\sim2000$ K. In this paper, we investigate the volatile loss from the building blocks of Phobos and Deimos by hydrodynamic escape of vapor and radiation pressure on condensed particles. We show that a non-negligible amount of volatiles ($> 10\%$ of the vapor with temperature $> 1000$ K via hydrodynamic escape, and moderately volatile dusts that condense at $\sim700-2000$ K via radiation pressure) could be removed just after the impact during their first signle orbit from their pericenters to apocenters. Our results indicate that bulk Phobos and Deimos are depleted in volatile elements. Together with future explorations such as JAXA's MMX (Martian Moons eXploration) mission, our results would be used to constrain the origin of Phobos and Deimos., Comment: 15 pages, 8 figures. Accepted for publication in ApJ

Published
2018
Full Text
View/download PDF

4. On the impact origin of Phobos and Deimos III: resulting composition from different impactors

Author

Pignatale, Francesco C., Charnoz, Sébastien, Rosenblatt, Pascal, Hyodo, Ryuki, Nakamura, Tomoki, and Genda, Hidenori

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The origin of Phobos and Deimos in a giant impact generated disk is gaining larger attention. Although this scenario has been the subject of many studies, an evaluation of the chemical composition of the Mars' moons in this framework is missing. The chemical composition of Phobos and Deimos is unconstrained. The large uncertainty about the origin of the mid-infrared features, the lack of absorption bands in the visible and near-infrared spectra, and the effects of secondary processes on the moons' surface make the determination of their composition very difficult from remote sensing data. Simulations suggest a formation of a disk made of gas and melt with their composition linked to the nature of the impactor and Mars. Using thermodynamic equilibrium we investigate the composition of dust (condensates from gas) and solids (from a cooling melt) that result from different types of Mars impactors (Mars-, CI-, CV-, EH-, comet-like). Our calculations show a wide range of possible chemical compositions and noticeable differences between dust and solids depending on the considered impactors. Assuming Phobos and Deimos as result of the accretion and mixing of dust and solids, we find that the derived assemblage (dust rich in metallic-iron, sulphides and/or carbon, and quenched solids rich in silicates) can be compatible with the observations. The JAXA's MMX (Martian Moons eXploration) mission will investigate the physical and chemical properties of the Maroons, especially sampling from Phobos, before returning to Earth. Our results could be then used to disentangle the origin and chemical composition of the pristine body that hit Mars and suggest guidelines for helping in the analysis of the returned samples., Comment: Accepted for publication in ApJ (13/12/2017)

Published
2017
Full Text
View/download PDF

5. On the Impact Origin of Phobos and Deimos II: True Polar Wander and Disk Evolution

Author

Hyodo, Ryuki, Rosenblatt, Pascal, Genda, Hidenori, and Charnoz, Sébastien

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Phobos and Deimos are the two small Martian moons, orbiting almost on the equatorial plane of Mars. Recent works have shown that they can accrete within an impact-generated inner dense and outer light disk, and that the same impact potentially forms the Borealis basin, a large northern hemisphere basin on the current Mars. However, there is no a priori reason for the impact to take place close to the north pole (Borealis present location) nor to generate a debris disk in the equatorial plane of Mars (in which Phobos and Deimos orbit). In this paper, we investigate these remaining issues on the giant impact origin of the Martian moons. First, we show that the mass deficit created by the Borealis impact basin induces a global reorientation of the planet to realign its main moment of inertia with the rotation pole (True Polar Wander). This moves the location of the Borealis basin toward its current location. Next, using analytical arguments, we investigate the detailed dynamical evolution of the eccentric inclined disk from the equatorial plane of Mars that is formed by the Martian-moon-forming impact. We find that, as a result of precession of disk particles due to the Martian dynamical flattening $J_{2}$ term of its gravity field and particle-particle inelastic collisions, eccentricity and inclination are damped and an inner dense and outer light equatorial circular disk is eventually formed. Our results strengthen the giant impact origin of Phobos and Deimos that can finally be tested by a future sample return mission such as JAXA's Martian Moons eXploration (MMX) mission., Comment: 13 pages, 5 figures. Accepted for publication in ApJ

Published
2017
Full Text
View/download PDF

6. Impact analysis of the transponder time delay on radio-tracking observables

Author

Bertone, Stefano, Poncin-Lafitte, Christophe Le, Rosenblatt, Pascal, Lainey, Valéry, Marty, Jean-Charles, and Angonin, Marie-Christine

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Accurate tracking of probes is one of the key points of space exploration. Range and Doppler techniques are the most commonly used. In this paper we analyze the impact of the transponder delay, $i.e.$ the processing time between reception and re-emission of a two-way tracking link at the satellite, on tracking observables and on spacecraft orbits. We show that this term, only partially accounted for in the standard formulation of computed space observables, can actually be relevant for future missions with high nominal tracking accuracies or for the re-processing of old missions. We present several applications of our formulation to Earth flybys, the NASA GRAIL and the ESA BepiColombo missions., Comment: 19 pages, 4 figures, 2 tables. Accepted for publication in Advances in Space Research

Published
2017
Full Text
View/download PDF

7. On the Impact Origin of Phobos and Deimos I: Thermodynamic and Physical Aspects

Author

Hyodo, Ryuki, Genda, Hidenori, Charnoz, Sébastien, and Rosenblatt, Pascal

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Phobos and Deimos are the two small moons of Mars. Recent works have shown that they can accrete within an impact-generated disk. However, the detailed structure and initial thermodynamic properties of the disk are poorly understood. In this paper, we perform high-resolution SPH simulations of the Martian moon-forming giant impact that can also form the Borealis basin. This giant impact heats up the disk material (around $\sim 2000$ K in temperature) with an entropy increase of $\sim 1500$ J K$^{-1}$ kg$^{-1}$. Thus, the disk material should be mostly molten, though a tiny fraction of disk material ($< 5\%$) would even experience vaporization. Typically, a piece of molten disk material is estimated to be meter sized due to the fragmentation regulated by their shear velocity and surface tension during the impact process. The disk materials initially have highly eccentric orbits ($e \sim 0.6-0.9$) and successive collisions between meter-sized fragments at high impact velocity ($\sim 3-5$ km s$^{-1}$) can grind them down to $\sim100 \mu$m-sized particles. On the other hand, a tiny amount of vaporized disk material condenses into $\sim 0.1 \mu$m-sized grains. Thus, the building blocks of the Martian moons are expected to be a mixture of these different sized particles from meter-sized down to $\sim 100 \mu$m-sized particles and $\sim 0.1 \mu$m-sized grains. Our simulations also suggest that the building blocks of Phobos and Deimos contain both impactor and Martian materials (at least 35%), most of which come from the Martian mantle (50-150 km in depth; at least 50%). Our results will give useful information for planning a future sample return mission to Martian moons, such as JAXA's MMX (Martian Moons eXploration) mission., Comment: 11 pages, 6 figures. Accepted for publication in ApJ

Published
2017
Full Text
View/download PDF

8. EnVision: understanding why our most Earth-like neighbour is so different

Author

Ghail, Richard, Wilson, Colin, Widemann, Thomas, Bruzzone, Lorenzo, Dumoulin, Caroline, Helbert, Jörn, Herrick, Robbie, Marcq, Emmanuel, Mason, Philippa, Rosenblatt, Pascal, Vandaele, Ann Carine, and Burtz, Louis-Jerome

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

This document is the EnVision Venus orbiter proposal, submitted in October 2016 in response to ESA's M5 call for Medium-size missions for its Science Programme, for launch in 2029. Why are the terrestrial planets so different? Venus should be the most Earth-like of all our planetary neighbours: its size, bulk composition and distance from the Sun are very similar to those of Earth. Its original atmosphere was probably similar to that of early Earth, with abundant water that would have been liquid under the young sun's fainter output. Even today, with its global cloud cover, the surface of Venus receives less solar energy than does Earth, so why did a moderate climate ensue here but a catastrophic runaway greenhouse on Venus? How and why did it all go wrong for Venus? What lessons can be learned about the life story of terrestrial planets in general, in this era of discovery of Earth-like exoplanets? Were the radically different evolutionary paths of Earth and Venus driven solely by distance from the Sun, or do internal dynamics, geological activity, volcanic outgassing and weathering also play an important part? Following the primarily atmospheric focus of Venus Express, we propose a new Venus orbiter named EnVision, to focus on Venus' geology and geochemical cycles, seeking evidence for present and past activity. The payload comprises a state-of-the-art S-band radar which will be able to return imagery at spatial resolutions of 1 - 30 m, and capable of measuring cm-scale deformation; this is complemented by subsurface radar, IR and UV spectrometers to map volcanic gases, and by geodetic investigations., Comment: ES M5 mission proposal

Published
2017

9. Planetary Radio Interferometry and Doppler Experiment (PRIDE) technique: A test case of the Mars Express Phobos fly-by

Author

Duev, Dmitry A., Pogrebenko, Sergei V., Cimò, Giuseppe, Calvés, Guifré Molera, Bahamón, Tatiana M. Bocanegra, Gurvits, Leonid I., Kettenis, Mark M., Kania, Joseph, Tudose, Valeriu, Rosenblatt, Pascal, Marty, Jean-Charles, Lainey, Valery, de Vicente, Pablo, Quick, Jonathan, Nickola, Marisa, Neidhardt, Alexander, Kronschnabl, Gerhard, Plötz, Christian, Haas, Rüdiger, Lindqvist, Michael, Orlati, Andrea, Ipatov, Alexander V., Kharinov, Mikhail A., Mikhailov, Andrey G., Lovell, Jim, McCallum, Jamie, Stevens, Jamie, Gulyaev, Sergei A., Natush, Tim, Weston, Stuart, Wang, Weihua, Xia, Bo, Yang, Wenjun, Hao, Long-Fei, Kallunki, Juha, and Witasse, Olivier

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The closest ever fly-by of the Martian moon Phobos, performed by the European Space Agency's Mars Express spacecraft, gives a unique opportunity to sharpen and test the Planetary Radio Interferometry and Doppler Experiments (PRIDE) technique in the interest of studying planet - satellite systems. The aim of this work is to demonstrate a technique of providing high precision positional and Doppler measurements of planetary spacecraft using the Mars Express spacecraft. The technique will be used in the framework of Planetary Radio Interferometry and Doppler Experiments in various planetary missions, in particular in fly-by mode. We advanced a novel approach to spacecraft data processing using the techniques of Doppler and phase-referenced very long baseline interferometry spacecraft tracking. We achieved, on average, mHz precision (30 {\mu}m/s at a 10 seconds integration time) for radial three-way Doppler estimates and sub-nanoradian precision for lateral position measurements, which in a linear measure (at a distance of 1.4 AU) corresponds to ~50 m., Comment: 9 pages, 14 figures. Astronomy and Astrophysics, accepted on 2016/05/31

Published
2016
Full Text
View/download PDF

14. DePhine – The Deimos and Phobos Interior Explorer

Author

Oberst, Jürgen, Wickhusen, Kai, Willner, Konrad, Gwinner, Klaus, Spiridonova, Sofya, Kahle, Ralph, Coates, Andrew, Herique, Alain, Plettemeier, Dirk, Díaz-Michelena, Marina, Zakharov, Alexander, Futaana, Yoshifumi, Pätzold, Martin, Rosenblatt, Pascal, Lawrence, David J., Lainey, Valery, Gibbings, Alison, and Gerth, Ingo

Published
2018
Full Text
View/download PDF

25. Lander radioscience for obtaining the rotation and orientation of Mars

Author

Dehant, Veronique, Folkner, William, Renotte, Etienne, Orban, Daniel, Asmar, Sami, Balmino, Georges, Barriot, Jean-Pierre, Benoist, Jeremy, Biancale, Richard, Biele, Jens, Budnik, Frank, Burger, Stefaan, de Viron, Olivier, Häusler, Bernd, Karatekin, Özgur, Le Maistre, Sébastien, Lognonné, Philippe, Menvielle, Michel, Mitrovic, Michel, Pätzold, Martin, Rivoldini, Attilio, Rosenblatt, Pascal, Schubert, Gerald, Spohn, Tilman, Tortora, Paolo, Van Hoolst, Tim, Witasse, Olivier, and Yseboodt, Marie

Published
2009
Full Text
View/download PDF

26. Géodésie planétaire: Application au champ de gravité du système martien et la formation des lunes de Mars

Author

Rosenblatt, Pascal, Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Nantes, and Pr. Christophe Sotin

Subjects
Géodésie Spatiale – Géodésie planétaire – Intérieur des planètes – Mars – Lune de Mars – Phobos – Deimos, Space geodesy – Planetary geodesy – Planetary interior – Mars – Martian moons – Phobos – Deimos, [SDU]Sciences of the Universe [physics]
Published
2021

27. GETEMME—a mission to explore the Martian satellites and the fundamentals of solar system physics

Author

Oberst, Jürgen, Lainey, Valéry, Poncin-Lafitte, Christophe Le, Dehant, Veronique, Rosenblatt, Pascal, Ulamec, Stephan, Biele, Jens, Spurmann, Jörn, Kahle, Ralph, Klein, Volker, Schreiber, Ulrich, Schlicht, Anja, Rambaux, Nicolas, Laurent, Philippe, Noyelles, Benoît, Foulon, Bernard, Zakharov, Alexander, Gurvits, Leonid, Uchaev, Denis, Murchie, Scott, Reed, Cheryl, Turyshev, Slava G., Gil, Jesus, Graziano, Mariella, Willner, Konrad, Wickhusen, Kai, Pasewaldt, Andreas, Wählisch, Marita, and Hoffmann, Harald

Published
2012
Full Text
View/download PDF

32. EnVision Radio Science Experiment

Author

Dumoulin, Caroline, primary, Rosenblatt, Pascal, additional, Tellmann, Silvia, additional, Genova, Antonio, additional, Marty, Jean-Charles, additional, Pätzold, Martin, additional, Oschlisniok, Janusz, additional, Kaspi, Yohai, additional, Galanti, Eli, additional, Withers, Paul, additional, and Fienga, Agnès, additional

Published
2020
Full Text
View/download PDF

33. The science goals of the EnVision Venus orbiter mission

Author

Ghail, Richard, primary, Wilson, Colin, additional, Widemann, Thomas, additional, Titov, Dmitri, additional, Ansan, Veronique, additional, Bovolo, Francesca, additional, Breuer, Doris, additional, Bruzzone, Lorenzo, additional, Campbell, Bruce, additional, Dumoulin, Caroline, additional, Helbert, Jörn, additional, Hensley, Scott, additional, Kiefer, Walter, additional, Komatsu, Goro, additional, Le Gall, Alice, additional, Marcq, Emmanuel, additional, Mason, Philippa, additional, Robert, Séverine, additional, Rosenblatt, Pascal, additional, and Vandaele, Ann Carine, additional

Published
2020
Full Text
View/download PDF

35. Radio Sounding of the Venusian Atmosphere and Ionosphere with EnVision

Author

Tellmann, Silvia, Kaspi, Yohai, Lebonnois, Sébastien, Lefèvre, Franck, Oschlisniok, Janusz, Withers, Paul, Dumoulin, Caroline, Rosenblatt, Pascal, Cardon, Catherine, Rhenish Institute for Environmental Research (RIU), University of Cologne, Weizmann Institute of Science [Rehovot, Israël], 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), 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), Department of Astronomy [Boston], Boston University [Boston] (BU), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), and Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU] Sciences of the Universe [physics], [SDU]Sciences of the Universe [physics], Physics::Space Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Physics::Atmospheric and Oceanic Physics
Abstract

International audience; EnVision is a one of the final candidates for the M5 call of the Cosmic Vision program from ESA. It is dedicated to unravel some of the numerous open questions about Venus' past, current state and future. The Radio Science Experiment on EnVision will perform extensive studies of the gravitational field but also Radio Occultations to sense the Venus atmosphere and ionosphere at a high vertical resolution of only a few hundred metres. These radio occultations provide electron density profiles in the ionosphere and atmospheric density, temperature and pressure profiles in the upper troposphere and mesosphere. Additionally, they allow to study the H2SO4 absorption in the Venus cloud layer.

Published
2019

36. Envision M5 Venus orbiter proposal

Author

Ghail, Richard, Wilson, Colin, Widemann, Thomas, Titov, Dmitrij, Bruzzone, Lorenzo, Helbert, Jörn, Carine Vandaele, Ann, Marcq, Emmanuel, Dumoulin, Caroline, and Rosenblatt, Pascal

Subjects
Envision, M5, Leitungsbereich PF, proposal, orbiter, Venus
Abstract

EnVision [1,2] is a Venus orbiter mission that will determine the nature and current state of geological activity on Venus, and its relationship with the atmosphere, to understand how and why Venus and Earth evolved so differently. Envision is a finalist in ESA’s M5 Space Science mission selection process, and is being developed in collaboration with NASA, with the sharing of responsibilities currently under assessment. It is currently in Phase A study; final mission selection is expected in June 2021. If selected, EnVision will launch by 2032 on an Ariane 6.2 into a six month cruise to Venus, followed by aerobraking, to achieve a near-circular polar orbit for a nominal science phase lasting at least 4 Venus sidereal days (2.7 Earth years).

Published
2019

38. Science of MMX mission: Origin of Martian moons

Author

Hyodo, Ryuki, Genda, Hidenori, Charnoz, Sebastian, and Rosenblatt, Pascal

Abstract

第18回宇宙科学シンポジウム (2018年1月9日-10日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)相模原キャンパス), 相模原市, 神奈川県, 18th Space Science Symposium (January 9-10, 2018. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS)Sagamihara Campus), Sagamihara, Kanagawa Japan, 資料番号: SA6000118102, レポート番号: P-069

Published
2018

39. Mars rotation determination from a moving rover using Doppler tracking data: What could be done?

Author

UCL - SST/ELI/ELIC - Earth & Climate, Le Maistre, Sebastien, Rosenblatt, Pascal, Dehant, Véronique, Marty, Jean-Charles, Yseboodt, Marie, UCL - SST/ELI/ELIC - Earth & Climate, Le Maistre, Sebastien, Rosenblatt, Pascal, Dehant, Véronique, Marty, Jean-Charles, and Yseboodt, Marie

Abstract

This paper is a case study providing some insights on what improvement could be achieved on the Mars Orientation and rotation Parameters (MOP) determination using radio tracking data from a moving rover. Thanks to high-performance mobility systems onboard new generation of rovers like ExoMars 2020, the position of the rover can be precisely known with respect to its previous position. This characteristic, together with the long life of the rovers and their steerable high-gain-antenna communication system, is shown here to provide an unexpected opportunity to improve the MOP determination. This paper presents the results of numerical simulations involving radio-science experiments between the moving rover and the Earth ground stations as well as between the rover and an orbiting spacecraft. The benefits of combining both links (direct-to-Earth and rover-orbiter) for the MOP determination is also assessed. The impacts of the spacecraft position accuracy as well as the frequency band used to communicate with it are quantified. It is shown that, after one Martian year of operation, the polar motion could be determined with 5 milliarcsecond (mas) of precision (formal error) from the rover-orbiter Doppler link, while it cannot be determined with usual equatorial lander-to-Earth radio link. This would allow for the first time the direct detection of the Chandler wobble amplitude in the polar motion of Mars, which is an important quantity to constrain the planet interior and atmospheric models. Although the moving rover Doppler data alone barely improve the current precision on the other MOP (like the length-of-day and nutation), a combination of those together with historical and future lander data would definitely help to fill gaps in the MOP signal and to decorrelate between the estimated parameters, thereby reducing the uncertainties in their determination.

Published
2018

40. DePhine - The Deimos and Phobos Interior Explorer

Author

Oberst, Juergen, Wickhusen, Kai, Willner, Konrad, Gwinner, Klaus, Spiridonova, Sofya, Kahle, Ralph, Coates, Andrew, Herique, Alain, Plettemeier, Dirk, Diaz-Michelena, Marina, Zakharov, Alexander, Futaana, Yoshifumi, Paetzold, Martin, Rosenblatt, Pascal, Lawrence, David J., Lainey, Valery, Gibbings, Alison, Gerth, Ingo, Oberst, Juergen, Wickhusen, Kai, Willner, Konrad, Gwinner, Klaus, Spiridonova, Sofya, Kahle, Ralph, Coates, Andrew, Herique, Alain, Plettemeier, Dirk, Diaz-Michelena, Marina, Zakharov, Alexander, Futaana, Yoshifumi, Paetzold, Martin, Rosenblatt, Pascal, Lawrence, David J., Lainey, Valery, Gibbings, Alison, and Gerth, Ingo

Abstract

DePhine - Deimos and Phobos Interior Explorer - is a mission proposed in the context of ESA's Cosmic Vision program, for launch in 2030. The mission will explore the origin and the evolution of the two Martian satellites, by focusing on their interior structures and diversity, by addressing the following open questions: Are Phobos and Deimos true siblings, originating from the same source and sharing the same formation scenario? Are the satellites rubble piles or solid bodies? Do they possess hidden deposits of water ice in their interiors? The DePhine spacecraft will be inserted into Mars transfer and will initially enter a Deimos quasi-satellite orbit to carry out a comprehensive global mapping. The goal is to obtain physical parameters and remote sensing data for Deimos comparable to data expected to be available for Phobos at the time of the DePhine mission for comparative studies. As a highlight of the mission, close flybys will be performed at low velocities, which will increase data integration times, enhance the signal strength and data resolution. 10-20 flyby sequences, including polar passes, will result in a dense global grid of observation tracks. The spacecraft orbit will then be changed into a Phobos resonance orbit to carry out multiple close flybys and to perform similar remote sensing as for Deimos. The spacecraft will carry a suite of remote sensing instruments, including a camera system, a radio science experiment, a high-frequency radar, a magnetometer, and a Gamma Ray/Neutron Detector. A steerable antenna will allow simultaneous radio tracking and remote sensing observations (which is technically not possible for Mars Express). Additional instrumentation, e.g. a dust detector and a solar wind sensor, will address further science goals of the mission. If Ariane 6-2 and higher lift performance are available for launch (the baseline mission assumes a launch on a Soyuz Fregat), we expect to have greater spacecraft mobility and possibly added payload

Published
2018

41. BIRDY - Interplanetary CubeSat for planetary geodesy of Small Solar System Bodies (SSSB)

Author

Hestroffer, Daniel, Agnan, Marco, Segret, Boris, Quinsac, Gary, Vannitsen, Jordan, Rosenblatt, Pascal, Miau, Jiun-Jih, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), 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 de Lille-Centre National de la Recherche Scientifique (CNRS), Planetology and Environments from Ground Astrometry and Space Exploration (PEGASE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, National Cheng Kung University (NCKU), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatoire Royal de Belgique (ORB), and Henry, Florence

Subjects
[PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; We are developing the Birdy concept of a scientific interplanetary CubeSat, for cruise, or proximity operations around a Small body of the Solar System (asteroid, comet, irregular satellite). The scientific aim is to characterise the body's shape, gravity field, and internal structure through imaging and radio-science techniques. Radio-science is now of common use in planetary science (flybys or orbiters) to derive the mass of the scientific target and possibly higher order terms of its gravity field. Its application to a nano-satellite brings the advantage of enabling low orbits that can get closer to the body's surface, hence increasing the SNR for precise orbit determination (POD), with a fully dedicated instrument. Additionally, it can be applied to two or more satellites, on a leading-trailing trajectory, to improve the gravity field determination. However, the application of this technique to CubeSats in deep space, and inter-satellite link has to be proven. Interplanetary CubeSats need to overcome a few challenges before reaching successfully their deep-space objectives: link to ground-segment, energy supply, protection against radiation, etc. Besides, the Birdy CubeSat --- as our basis concept --- is designed to be accompanying a mothercraft, and relies partly on the main mission for reaching the target, as well as on data-link with the Earth. However, constraints to the mothercraft needs to be reduced, by having the CubeSat as autonomous as possible. In this respect, propulsion and auto-navigation are key aspects, that we are studying in a Birdy-T engineering model. We envisage a 3U size CubeSat with radio link, object-tracker and imaging function, and autonomous ionic propulsion system. We are considering two case studies for autonomous guidance, navigation and control, with autonomous propulsion: in cruise and in proximity, necessitating DeltaV up to 2m/s for a total budget of about 50m/s. In addition to the propulsion, in-flight orbit determination (IFOD) and maintenance are studied, through analysis of images by an object-tracker and astrometry of solar system objects in front of background stars. Before going to deep-space, our project will start with BIRDY-1 orbiting the Earth, to validate the concepts of adopted propulsion, IFOD and orbit maintenance, as well as the radio-science and POD.

Published
2017

44. Tidal constraints on the interior of Venus

Author

Dumoulin, Caroline, Tobie, Gabriel, Verhoeven, Olivier, Rosenblatt, Pascal, Rambaux, Nicolas, Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire Royal de Belgique (ORB), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), 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 de Lille-Centre National de la Recherche Scientifique (CNRS), Astronomie et systèmes dynamiques (ASD), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Henry, Florence, Royal Observatory of Belgium [Brussels] (ROB), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Physics::Geophysics
Abstract

International audience; As a prospective study for a future exploration of Venus, we propose to systematically investigate the signature of the internal structure in the gravity field and the rotation state of Venus, through the determination of the moment of inertia and the tidal Love number.We test various mantle compositions, core size and density as well as temperature profiles representative of different scenarios for formation and evolution of Venus. The mantle density rho and seismic vP and vS wavespeeds are computed in a consistent manner from given temperature and composition using the Perple X program. This method computes phase equilibria and uses the thermodynamics of mantle minerals developped by Stixrude and Lithgow-Bertelloni (2011).The viscoelastic deformation of the planet interior under the action of periodic tidal forces are computed following the method of Tobie et al. (2005).For a variety of interior models of Venus, the Love number, k2, and the moment of inertia factor are computed following the method described above. The objective is to determine the sensitivity of these synthetic results to the internal structure. These synthetic data are then used to infer the measurement accuracies required on the time-varying gravitational field and the rotation state (precession rate, nutation and length of day variations) to provide useful constraints on the internal structure.We show that a better determination of k2, together with an estimation of the moment of inertia, the radial displacement, and of the time lag, if possible, will refine our knowledge on the present-day interior of Venus (size of the core, mantle temperature, composition and viscosity). Inferring these quantities from a future ex- ploration mission will provide essential constraints on the formation and evolution scenarios of Venus.

Published
2016
Full Text
View/download PDF

45. Physical librations and possible homogeneity of natural moons from astrometry

Author

Lainey, Valéry, Cooper, Nicholas J., Murray, Carl D., Noyelles, Benoît, Pasewaldt, Andreas, Robert, Vincent, Rosenblatt, Pascal, Thuillot, William, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), 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 de Lille-Centre National de la Recherche Scientifique (CNRS), Planetology and Environments from Ground Astrometry and Space Exploration (PEGASE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, QMUL, UNamur, DLR, Institut Polytechnique des Sciences Avancées (IPSA), and Observatoire Royal de Belgique (ORB)

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; Astrometry is the discipline that aims to provide positions of celestial objects in space with the highest accuracy. Thanks to recent space missions like Mars Express and Cassini, astrometric measurements of moons have allowed the probing of the gravity environment of their systems with unprecedented resolution. Here we focus on the possible determination of physical librations on the rotation of the moons, by modelling their effects on the moons' orbits. Assuming a homogeneous density, a theoretical expectation of the main libration can be computed and compared with possible observed values obtained indirectly from the orbit. In this work, we obtain for Phobos a physical libration of 1.04 /- 0.02 degrees, in agreement with a homogeneous interior. The case of some of the inner moons of Saturn will be addressed, also.

Published
2016

46. Formation of Phobos and Deimos in a giant collision scenario facilitated by a large transient moon

Author

Charnoz, Sébastien, Rosenblatt, Pascal, Dunseath, Kevin M., Terao-Dunseath, Mariko, Trinh, Antony, Hyodo, Ryuki, Genda, Hidenori, Institut de Physique du Globe de Paris (IPGP), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Royal Observatory of Belgium [Brussels], Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Earth-Life Science Institute [Tokyo] (ELSI), Tokyo Institute of Technology [Tokyo] (TITECH), Royal Observatory of Belgium [Brussels] (ROB), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS]Physics [physics], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2016

47. Origin of Phobos and Deimos: an overview

Author

Rosenblatt, Pascal, Charnoz, Sébastien, Dunseath, Kevin M., Dunseath-Terao, Mariko, Trinh, Antony, Hyodo, Ryuki, Genda, Hidenori, Toupin, Stéven, Royal Observatory of Belgium [Brussels] (ROB), Institut de Physique du Globe de Paris (IPGP), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Earth-Life Science Institute [Tokyo] (ELSI), Tokyo Institute of Technology [Tokyo] (TITECH), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), and Royal Observatory of Belgium [Brussels]

Subjects
[PHYS.PHYS.PHYS-ATOM-PH]Physics [physics]/Physics [physics]/Atomic Physics [physics.atom-ph], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2016

48. Formation of Phobos and Deimos in an extended circum-martian accretion disk

Author

Rosenblatt, Pascal, Charnoz, Sébastien, Dunseath, Kevin, Dunseath-Terao, Mariko, Trinh, Antony, Hyodo, Ryuki, Genda, Hidenori, Toupin, Stéven, Royal Observatory of Belgium [Brussels] (ROB), Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Earth-Life Science Institute [Tokyo] (ELSI), Tokyo Institute of Technology [Tokyo] (TITECH), Institute of Geodesy and Geoinformation Science, Technische Universität Berlin, Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), and Royal Observatory of Belgium [Brussels]

Subjects
[PHYS.PHYS.PHYS-ATOM-PH]Physics [physics]/Physics [physics]/Atomic Physics [physics.atom-ph], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2016

Catalog

Books, media, physical & digital resources
See catalog results