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  • News on "Geoparticles" | UnivEarthS
    Gamma ray instrumentation development Young team project Experimental geophysics Valorization project Data distribution visualisation and cloud computing PUBLICATIONS EDUCATIONAL Nanosatellite student project IGOsat UnivEarthS JOB OPPORTUNITY Experimental Dark Matter Search Post Doctoral Research Fellow IGOSat internship PhD position Effect of the North South dichotomy on the thermal structure and evolution of Mars Search this site October Mon Tue Wed Thu Fri Sat Sun 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31 Sign in Password forgotten Home News on Geoparticles Neutrino Geoscience 2015 Workshop 10 June 2015 15 19 The 2015 edition of the Neutrino Geoscience workshop will take place at IPGP from june 15th to 17th http www ipgp fr fr evenements neutrino geoscience 2015 conference En savoir plus Postdoctoral position at the interface of neutrino physics with geoscience 14 April 2014 10 42 The French excellence programme LabEx UnivEarthS has an opening for a postodoctoral position at the interface of neutrino physics with geoscience The activity will be based at the AsrtoParticle and Cosmology APC Laboratory in Paris and close collaboration with the Institut de Physique

    Original URL path: http://www.univearths.fr/en/node/news_i2 (2015-10-10)
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  • I3 : Fundamental physics and Geophysics in space | UnivEarthS
    Presentation Team Results experiences News Publications Through the space projects they have been or are pursuing IPGP and APC have acquired an expertise in precision measurements of distances times and acceleration in astrophysics fundamental physics in space Planetary surface Earth surface and ocean bottom as well as a leading role in France in the coordination of missions closely associated to these techniques e g French LISA office LISA France and the French Planetary seismometer selected onboard the NASA INSIGHT mission The techniques involved are necessarily associated with high technology and often extreme precision requiring unprecedented levels of noise control often in harsh conditions and measurements at very low frequency and space compliant instruments These techniques represent the path to the future and developing them will allow progress not only in the understanding of the most fundamental aspects of our environment whether it is the Earth solar system planets or the Universe at large but also in the technological prospects for forthcoming space missions They are indeed closely related with cutting edge knowledge and technologies such as nanotechnologies high precision distance measurements solid state physics etc The goal of this WP is to continue R D efforts in these domains in order to explore new technologies in acceleration measurements e g with optical or quantum devices including cold atoms high temperature superconducting squids and tunneling diodes in the displacement or gravity sensors head satellite satellite laser and radio ranging furthermore reduce mass and integrate control electronics e g with the development of Asics hybrids and highly integrated 3D packaging precisely understand the physics of extremely low thrust engine e g surface and chemical effects of ion sources used for micro newton thrusters and highly improve insulating structure and packaging by controlling thermal transfers at the nanoscale e g nano thermal coating

    Original URL path: http://www.univearths.fr/en/i3-fundamental-physics-and-geophysics-space?mini=node%2F333%2F2015-09 (2015-10-10)
    Open archived version from archive

  • I3 : Fundamental physics and Geophysics in space | UnivEarthS
    space Presentation Team Results experiences News Publications Through the space projects they have been or are pursuing IPGP and APC have acquired an expertise in precision measurements of distances times and acceleration in astrophysics fundamental physics in space Planetary surface Earth surface and ocean bottom as well as a leading role in France in the coordination of missions closely associated to these techniques e g French LISA office LISA France and the French Planetary seismometer selected onboard the NASA INSIGHT mission The techniques involved are necessarily associated with high technology and often extreme precision requiring unprecedented levels of noise control often in harsh conditions and measurements at very low frequency and space compliant instruments These techniques represent the path to the future and developing them will allow progress not only in the understanding of the most fundamental aspects of our environment whether it is the Earth solar system planets or the Universe at large but also in the technological prospects for forthcoming space missions They are indeed closely related with cutting edge knowledge and technologies such as nanotechnologies high precision distance measurements solid state physics etc The goal of this WP is to continue R D efforts in these domains in order to explore new technologies in acceleration measurements e g with optical or quantum devices including cold atoms high temperature superconducting squids and tunneling diodes in the displacement or gravity sensors head satellite satellite laser and radio ranging furthermore reduce mass and integrate control electronics e g with the development of Asics hybrids and highly integrated 3D packaging precisely understand the physics of extremely low thrust engine e g surface and chemical effects of ion sources used for micro newton thrusters and highly improve insulating structure and packaging by controlling thermal transfers at the nanoscale e g nano thermal

    Original URL path: http://www.univearths.fr/en/i3-fundamental-physics-and-geophysics-space?quicktabs_menu_i3_en=0 (2015-10-10)
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  • INSIGHT mission selected by NASA | UnivEarthS
    Universe Interface projects Geoparticles Fundamental physics and Geophysics in space From dust to planets Former Interface projects Formation and early evolution of Planetary systems The youth of cosmic rays and their emergence in the interstellar clouds Gamma ray instrumentation development Young team project Experimental geophysics Valorization project Data distribution visualisation and cloud computing PUBLICATIONS EDUCATIONAL Nanosatellite student project IGOsat UnivEarthS JOB OPPORTUNITY Experimental Dark Matter Search Post Doctoral Research Fellow

    Original URL path: http://www.univearths.fr/en/node/315 (2015-10-10)
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  • I6: From dust to planets | UnivEarthS
    experimental high pressure equilibrium volatilization condensation irradiation adsorption diffusion samples A new platform of experimental cosmochemistry is under construction at IPGP that aims to simulate some key physical processes regarding gas dust interaction Our approach will be developed in 5 tasks What do the age and composition of CAIs and chondrules really tell us about the formation of the solar system How can we constrain irradiation processes in the early solar system from analyses of lunar soil grains and meteoritic chondrules and CAIs Why and how did the isotopic composition of major volatiles elements O N and C change so rapidly in the inner accretion disk What is the origin of highly volatile elements in parent bodies from laboratory simulations of gas dust interactions How and when did the first planetesimals form As disk observations and laboratory measurements will provide constrains on the transport of solids it will be necessary to provide scenarios of large scale transport relying on the physics of gaseous and dusty protoplanetary disks based on numerical simulations On this side AIM is leading the development of a large modeling program focusing on the transport of the first solids in the protoplanetary disk and their incorporation into embryos including turbulent dynamics radiative effects and planet disk interactions Simple chemical and isotopic fractionation models will be included into simulations of turbulent dust transport in order to test different scenarios to interpret isotopic data Three important modeling tasks will be lead Development of a dust transport model in the protoplanetary disk taking into account turbulence and dust condensation refractories near the Sun and volatiles near the snow line Coupling of the dust transport model with a radiative transfer code in order to create synthetic images to space observation of disks Development of a protoplanetary disk thermodynamical model in order to constrain the condition of formation of dust in order to compare with laboratory data Estimation of the irradiation flux of dust in the disk in order to calibrate experiments of fractionation of dust under irradiation Beside the earliest phases of planet formation N body simulations of embryo transport in the disk in the frame of the Nice model will be lead to constrain the radial origin of the building blocks that assembled into the modern terrestrial planets This will lead naturally to interactions with research theme 2 that concerns itself with the initial differentiation and interior structure of the terrestrial planets Differentiation interior structure and geologic evolution of the terrestrial planets The processes that took place during the initial differentiation of the Earth are reasonable well understood the composition of the major chemical reservoirs crust mantle and core are relatively well known and the manner by which internal heat is lost to space via plate tectonics is understood from both observational of modeling perspectives For the other terrestrial planets however our understanding of these processes is considerably more limited and many first order questions remain unresolved For example What is the thickness and composition of the crust of Mercury the Moon and Mars At what depths do the major phase transitions occur in the mantles of Mars and Venus and how do these phase transitions affect mantle convection and plume dynamics What is the size of the metallic core of Mercury Mars and the Moon And what are the abundances of light alloying elements such as sulfur carbon and silicon in the liquid portion of their cores Do Mercury Mars and the Moon possess a solid inner core And is core crystallization the source of energy that is powering the dynamo generated magnetic field of Mercury today What was the energy source that powered the early dynamos of Mars and the Moon and why did their dynamos later shut off To address these and other question this project will rely upon a three pronged approach making use of geophysical data collected by planetary missions high pressure laboratory experiments and numerical and geophysical modeling Members of this research axe are currently involved in several NASA and ESA planetary missions at both the co investigator and principal investigator level including NASA s geophysical missions to the Moon GRAIL and Mars InSight and ESA s orbital missions to Mercury BepiColumbo and Jupiter JUICE Furthermore members of our project have recently finished the construction of a world class high pressure geo materials laboratory that is currently making its first measurements Together these datasets will offer us a unique perspective to unravel the above listed questions concerning the differentiation interior evolution and geologic evolution of the terrestrial planets The first two years of the UnivEarthS I1 project funded our analyses of lunar gravitational data acquired during the primary mission of the Gravity Recovery and Interior Laboratory GRAIL mission Results from our group have shown that the crust of the Moon is significantly thinner than once thought that the crust has been highly fractured by billions of years of impact cratering and that lateral variations in crustal temperature have had a dramatic influence on the morphology of giant impact basins During this initial stage of analysis the UnivEarthS funded a LabEx postdoc and contributed to the publications of two articles in the journal Science We now have at our disposal gravitational data from the extended mission which has a spatial resolution that is two times better than that acquired during the primary mission Over the following three years we aim to study processes that were previously beyond reach such as the gravitational signature of magnetic anomalies and magmatic intrusions and the subsurface structure of medium sized simple and complex impact craters For these studies we ask that the UnivEarthS LabEx fund a post doc in additional to our initial demand three years ago At the time the initial UnivEarthS proposal was selected our group anticipated on providing a seismometer to the Japanese lunar geophysical mission SELENE 2 with a launch near 2018 Since this time NASA selected the Martian geophysical mission InSight which will be launched and land on Mars in 2016 Members of our research group are providing at the principal investigator level the sole instrument that is above the mission s science threshold This instrument is the very broad band seismometer that is being developed at IPGP and which will make the first seismic measurements ever on the surface of Mars Data from this mission will constrain the size of the martian core determine if a solid inner core exists determine the thickness of the crust and search for seismic discontinuities in the mantle among other objectives The UnivEarthS project previously agreed to fund a LabEx postdoc and a co financed thesis student for seismic analysis related to the SELENE 2 mission and these resources will be redirected towards the InSight mission in this revised project In addition to our initial demand we ask the UnivEarthS LabEx for an additional co financed thesis student to help with the flood of data that will arrive when InSight lands on Mars in 2016 The proposed experimental approach aims at combining astrophysical models of planetary accretion with geochemical models of planetary differentiation and cosmochemical constraints provided by meteorites During the first two years funded by the UnivEarthS LabEx the young research group JE1 developed protocols to use the laser heated diamond anvil cell for studying the geochemical imprint of planetary core formation We have shown notably in a recent publication in Science that the partitioning of slightly siderophile elements V and Cr during core formation imply that accretion of the Earth could have occurred under conditions that were more oxidizing than previously thought In this way Earth can accrete from materials as oxidized as the most common meteorites i e ordinary or carbonaceous chondrites and imply large mixing of proto planetary materials in the inner solar system Similarly Ni and Co partitioning shows clearly that the core cannot form at pressures lower than 35 GPa nor can it form at pressure higher than 65 GPa bracketing for the first time the depth of the terrestrial magma ocean in the first 50 million years after the birth of the Solar System The research we propose to develop over the next 5 years will help us constrain and understand the primordial differentiation of terrestrial bodies in the Solar System We plan to understand the early evolution of Vesta by combining high precision isotope geochemistry with experimental geochemistry through the study of isotopic fractionation of siderophile and volatile elements Si Cr Ga Cu Zn Sn as well as moderately siderophile elements W Mo One of the aims is to understand the accretion of the so called Late Veneer on small planetary embryos These studies can be applied to understanding the Earth Moon system after the giant impact through the comparison between Apollo samples and experimental charges once again with a special focus on volatile elements and their isotropic fractionation We have access to a very large collection of SNCs and have plans to propose refined models of Martian differentiation to understand the processes that can occur in a very short timescale and compare it with the relatively long timescale of terrestrial accretion These studies all require a savvy mix of experiments and cosmochemical observation and access to rare samples and represent a perfect integration of the experimentalists in this proposal with the cosmochemists Planetary interfaces atmosphere surface interior interactions The atmosphere of planetary body with no plate tectonics mainly forms and survives through the release of volatiles from the mantle or ice shell by volcanism or cryovolcanism and the persistence of surface reservoirs for those volatiles The presence and survival of an atmosphere provides in that way a window into the evolution of the volcanic activity the atmospheric dynamics and composition climate and the geology and geodynamics of a planetary body The aim of research theme 3 is thus to study the strong coupling between planetary bodies interiors surfaces and atmospheres constraining their concomitant formation and evolution throughout the age of the Solar System This axis combines the joint characterization of the solid and fluid envelops of terrestrial planets satellites and exoplanets following a complete comparative planetology approach with Mars Titan and exoplanets with an atmosphere as archetypes in a multi disciplinary way This project will include analysis of planetary mission data numerical simulations and laboratory experiments Atmosphere interior habitability coupling on Mars The INSIGHT mission planned to land on Mars in 2016 will provide the first constraints on martian mantle discontinuities and better constrain the thickness and composition of the crust composition Constraints on the mantle size if coupled with better constraints on the thermodynamical properties of the mantle phase transitions can be used for better modeling and understanding of early martian mantle dynamics mantle convection rates of crustal production and evolution in basaltic composition Furthermore constraints on the crust and mantle melt density can be used to estimate the amount of melt that is stored within or below the crust relative to the amount of melt that reaches the surface and hence releases its volatiles into the atmosphere With the new data provided by the INSIGHT mission we thus aim to constrain the coupled interior atmosphere co evolution of Mars and its impact on the primitive habitability of the planet For this project we ask for a co financed thesis student to help in the analysis of the data that will be provided by InSight INSIGHT will also provide the first coupled geophysical and meteorological observatory on Mars We expect the mission to detect the micro seismic noise generated by the interaction of wind with the surface This will be used to monitor and constraint the structure of the atmospheric boundary layer dynamics and to constrainthe surface saltation processes Dune physics and the link with planetary climate During the last two years new collaborations have been established with the Chinese Academy of Science to develop a novel type of field experiment designed to examine the physics of sand dunes within their natural environment using controlled initial and boundary conditions This so called landscape scale experiment is a new and unique concept that is particularly well suited for validation and quantification purposes Given the extreme conditions encountered in arid deserts and the time scales associated with the development of bedforms in situ experiments on aeolian sand dunes have to combine logistics facilities with long term measurements By successfully meeting these challenges in China thanks to the local climate and the field expertise of Chinese scientists we will be able to obtain new experimental evidences for the formation of dunes and their alignment in multimodal wind regimes The current ANR project EXODUNES provides financial support for the two first missions of fall 2013 and spring 2014 and no PhD grant on that topic Considering the timescale of Earth s aeolian dune dynamics this fieldwork needs to be extended over several years up to 2017 at least and will provides a huge amount of data which will require the recruiting of a thesis student Hence the main objective of the Ph D thesis will be to continue the landscape scale experiment from fall 2014 to spring 2017 carrying out the field measurements and all the statistical data analysis From this we will have a unique set of data to investigate dune morphodynamics which is intended to be put in close relation to dune morphodynamics and climate on Earth and other planetary bodies were dunes have been observed Mars and Saturn largest moon Titan Of the three new thesis topics that are being proposed for this project this topic is the project s highest priority Planetary sciences Publication Time evolution of snow regions and planet traps in an evolving protoplanetary disk 6 May 2015 14 39 K Baillié S Charnoz and E Pantin members of Interface Project From dust to stars publish their results in the newspaper Astronomy Astrophysics Their article is entitled Time evolution of snow regions and planet traps in an evolving protoplanetary disk En savoir plus Publication New look at the origin and the growth mechanism of Titan dunes 6 October 2014 14 02 Titan the largest satellite of Saturn has a thick atmosphere dominated by nitrogen and carbon compounds This satellite has many similarities with Earth including a very active weather cucle essentially controlled by methane and many landscapes with extremely familar faces in particular huge fields of linea dunes around the equator Such dune are observed in many terrestrial deserts and even on Mars and are witnesses of the wind regimes and sedimentary environment that shaped them En savoir plus 07 10 2014 PUBLICATIONS Sept 2013 Sept 2014 1 PUBLICATIONS AND BOOKS 26 papers published or under review in total since september 2013 in international peer reviewed journal 2 papers in Science accepted 2 papers in Nature Geoscience under review Theme 1 1 Baillié K Charnoz S Time Evolution of a Viscous Protoplanetary Disk with a Free Geometry Toward a More Self consistent Picture 2014 Apj 786 id 35 2 Tajeddine R N Rambaux Lainey S charnoz and 3 co authors Constraints on Mimas interior from Cassini ISS libration measurements Accepted in SCIENCE publication in Nov 2014 3 S Charnoz J Aléon N Chaumard E Tailliffet Formation of CAI by coagulation and fragmentation Submitted to Icarus Moderate revisions required 4 Baillié K Charnoz S Pantin E Evolution of front regions and planet traps in an evolving protoplanetary disk Submitted to A A 5 Charnoz S Michaut C Dynamical and thermodynamical evolution of the protoluar disk Submitted to Icarus 6 Chaussidon M Liu M C Early Solar System processes from nebular gas to the precursors of the Earth AGU Monograph Early Earth under revision 7 Furi E Chaussidon M Marty B accepté Evidence for an early nitrogen isotopic evolution in the solar nebula from volatile analyses of a CV3 CAI Geochim Cosmochim Acta 8 Luu T H Young E D Gounelle M Chaussidon M en révision A short time interval for condensation of high temperature silicates in the solar accretion disk Proc Nat Acad Sci 9 Mishra R Chaussidon M 2014 Fossil records of high level of 60 Fe in chondrules from unequilibrated chondrites Earth Planet Sci Lett 398 90 100 10 Moreira M Charnoz S The origin of the neon isotopes in chondrites and Earth Submitted to EPSL 11 Paul S Savage Heng Chen Igor S Puchtel Gregory Shofner J Siebert J Badro F Moynier Under review Nature Geoscience 12 Moynier F et Fegley B The Earth s building blocks AGU monograph accepted with revisions 13 Chen H Moynier F Humayun M Bishop MC Williams J Cosmogenic effects on Cu isotopes in IVB iron meteorites Implications for the Hf W chronometry Geochimica et cosmochimica acta Accepted with revisions Theme 2 1 Miljković K M A Wieczorek G S Collins M Laneuville G A Neumann H J Melosh S C Solomon R J Phillips D E Smith and M T Zuber 2013 Asymmetric distribution of lunar impact basins caused by variations in target properties Science 342 724 726 doi 10 1126 science 1243224 2 Laneuville M M A Wieczorek D Breuer and N Tosi 2013 Asymmetric thermal evolution of the Moon J Geophys Res Planets 118 1435 1452 doi 10 1002 jgre 20103 3 Thorey C and C Michaut 2014 A model for the dynamics of crater centered intrusion Application to lunar floor fractured craters J Geophys Res Planets 119 286 312 doi 10 1002 2013JE004467 4 Laneuville M M A Wieczorek D Breuer J Aubert G Morard T Ru ckriemen 2014 A long lived lunar dynamo powered by core crystallization Earth Planet Sci Lett 401 251 260 doi 10 1016 j epsl 2014 05 057 5 Miljkovic K M A Wieczorek G S Collins S C Solomon D E Smith M T Zuber Excavation of the lunar mantle by basin forming events on the Moon Earth Planet Sci Lett in revision 6 Price M C Ramkissoon N K McMahon S Miljkovic K Parnell J Wozniakiewicz P J Kearsley A T Blamey N J F Cole M J Burchell M J 2014 Limits on methane release and

    Original URL path: http://www.univearths.fr/en/i6-dust-planets?mini=node%2F333%2F2015-09 (2015-10-10)
    Open archived version from archive

  • I6: From dust to planets | UnivEarthS
    experimental high pressure equilibrium volatilization condensation irradiation adsorption diffusion samples A new platform of experimental cosmochemistry is under construction at IPGP that aims to simulate some key physical processes regarding gas dust interaction Our approach will be developed in 5 tasks What do the age and composition of CAIs and chondrules really tell us about the formation of the solar system How can we constrain irradiation processes in the early solar system from analyses of lunar soil grains and meteoritic chondrules and CAIs Why and how did the isotopic composition of major volatiles elements O N and C change so rapidly in the inner accretion disk What is the origin of highly volatile elements in parent bodies from laboratory simulations of gas dust interactions How and when did the first planetesimals form As disk observations and laboratory measurements will provide constrains on the transport of solids it will be necessary to provide scenarios of large scale transport relying on the physics of gaseous and dusty protoplanetary disks based on numerical simulations On this side AIM is leading the development of a large modeling program focusing on the transport of the first solids in the protoplanetary disk and their incorporation into embryos including turbulent dynamics radiative effects and planet disk interactions Simple chemical and isotopic fractionation models will be included into simulations of turbulent dust transport in order to test different scenarios to interpret isotopic data Three important modeling tasks will be lead Development of a dust transport model in the protoplanetary disk taking into account turbulence and dust condensation refractories near the Sun and volatiles near the snow line Coupling of the dust transport model with a radiative transfer code in order to create synthetic images to space observation of disks Development of a protoplanetary disk thermodynamical model in order to constrain the condition of formation of dust in order to compare with laboratory data Estimation of the irradiation flux of dust in the disk in order to calibrate experiments of fractionation of dust under irradiation Beside the earliest phases of planet formation N body simulations of embryo transport in the disk in the frame of the Nice model will be lead to constrain the radial origin of the building blocks that assembled into the modern terrestrial planets This will lead naturally to interactions with research theme 2 that concerns itself with the initial differentiation and interior structure of the terrestrial planets Differentiation interior structure and geologic evolution of the terrestrial planets The processes that took place during the initial differentiation of the Earth are reasonable well understood the composition of the major chemical reservoirs crust mantle and core are relatively well known and the manner by which internal heat is lost to space via plate tectonics is understood from both observational of modeling perspectives For the other terrestrial planets however our understanding of these processes is considerably more limited and many first order questions remain unresolved For example What is the thickness and composition of the crust of Mercury the Moon and Mars At what depths do the major phase transitions occur in the mantles of Mars and Venus and how do these phase transitions affect mantle convection and plume dynamics What is the size of the metallic core of Mercury Mars and the Moon And what are the abundances of light alloying elements such as sulfur carbon and silicon in the liquid portion of their cores Do Mercury Mars and the Moon possess a solid inner core And is core crystallization the source of energy that is powering the dynamo generated magnetic field of Mercury today What was the energy source that powered the early dynamos of Mars and the Moon and why did their dynamos later shut off To address these and other question this project will rely upon a three pronged approach making use of geophysical data collected by planetary missions high pressure laboratory experiments and numerical and geophysical modeling Members of this research axe are currently involved in several NASA and ESA planetary missions at both the co investigator and principal investigator level including NASA s geophysical missions to the Moon GRAIL and Mars InSight and ESA s orbital missions to Mercury BepiColumbo and Jupiter JUICE Furthermore members of our project have recently finished the construction of a world class high pressure geo materials laboratory that is currently making its first measurements Together these datasets will offer us a unique perspective to unravel the above listed questions concerning the differentiation interior evolution and geologic evolution of the terrestrial planets The first two years of the UnivEarthS I1 project funded our analyses of lunar gravitational data acquired during the primary mission of the Gravity Recovery and Interior Laboratory GRAIL mission Results from our group have shown that the crust of the Moon is significantly thinner than once thought that the crust has been highly fractured by billions of years of impact cratering and that lateral variations in crustal temperature have had a dramatic influence on the morphology of giant impact basins During this initial stage of analysis the UnivEarthS funded a LabEx postdoc and contributed to the publications of two articles in the journal Science We now have at our disposal gravitational data from the extended mission which has a spatial resolution that is two times better than that acquired during the primary mission Over the following three years we aim to study processes that were previously beyond reach such as the gravitational signature of magnetic anomalies and magmatic intrusions and the subsurface structure of medium sized simple and complex impact craters For these studies we ask that the UnivEarthS LabEx fund a post doc in additional to our initial demand three years ago At the time the initial UnivEarthS proposal was selected our group anticipated on providing a seismometer to the Japanese lunar geophysical mission SELENE 2 with a launch near 2018 Since this time NASA selected the Martian geophysical mission InSight which will be launched and land on Mars in 2016 Members of our research group are providing at the principal investigator level the sole instrument that is above the mission s science threshold This instrument is the very broad band seismometer that is being developed at IPGP and which will make the first seismic measurements ever on the surface of Mars Data from this mission will constrain the size of the martian core determine if a solid inner core exists determine the thickness of the crust and search for seismic discontinuities in the mantle among other objectives The UnivEarthS project previously agreed to fund a LabEx postdoc and a co financed thesis student for seismic analysis related to the SELENE 2 mission and these resources will be redirected towards the InSight mission in this revised project In addition to our initial demand we ask the UnivEarthS LabEx for an additional co financed thesis student to help with the flood of data that will arrive when InSight lands on Mars in 2016 The proposed experimental approach aims at combining astrophysical models of planetary accretion with geochemical models of planetary differentiation and cosmochemical constraints provided by meteorites During the first two years funded by the UnivEarthS LabEx the young research group JE1 developed protocols to use the laser heated diamond anvil cell for studying the geochemical imprint of planetary core formation We have shown notably in a recent publication in Science that the partitioning of slightly siderophile elements V and Cr during core formation imply that accretion of the Earth could have occurred under conditions that were more oxidizing than previously thought In this way Earth can accrete from materials as oxidized as the most common meteorites i e ordinary or carbonaceous chondrites and imply large mixing of proto planetary materials in the inner solar system Similarly Ni and Co partitioning shows clearly that the core cannot form at pressures lower than 35 GPa nor can it form at pressure higher than 65 GPa bracketing for the first time the depth of the terrestrial magma ocean in the first 50 million years after the birth of the Solar System The research we propose to develop over the next 5 years will help us constrain and understand the primordial differentiation of terrestrial bodies in the Solar System We plan to understand the early evolution of Vesta by combining high precision isotope geochemistry with experimental geochemistry through the study of isotopic fractionation of siderophile and volatile elements Si Cr Ga Cu Zn Sn as well as moderately siderophile elements W Mo One of the aims is to understand the accretion of the so called Late Veneer on small planetary embryos These studies can be applied to understanding the Earth Moon system after the giant impact through the comparison between Apollo samples and experimental charges once again with a special focus on volatile elements and their isotropic fractionation We have access to a very large collection of SNCs and have plans to propose refined models of Martian differentiation to understand the processes that can occur in a very short timescale and compare it with the relatively long timescale of terrestrial accretion These studies all require a savvy mix of experiments and cosmochemical observation and access to rare samples and represent a perfect integration of the experimentalists in this proposal with the cosmochemists Planetary interfaces atmosphere surface interior interactions The atmosphere of planetary body with no plate tectonics mainly forms and survives through the release of volatiles from the mantle or ice shell by volcanism or cryovolcanism and the persistence of surface reservoirs for those volatiles The presence and survival of an atmosphere provides in that way a window into the evolution of the volcanic activity the atmospheric dynamics and composition climate and the geology and geodynamics of a planetary body The aim of research theme 3 is thus to study the strong coupling between planetary bodies interiors surfaces and atmospheres constraining their concomitant formation and evolution throughout the age of the Solar System This axis combines the joint characterization of the solid and fluid envelops of terrestrial planets satellites and exoplanets following a complete comparative planetology approach with Mars Titan and exoplanets with an atmosphere as archetypes in a multi disciplinary way This project will include analysis of planetary mission data numerical simulations and laboratory experiments Atmosphere interior habitability coupling on Mars The INSIGHT mission planned to land on Mars in 2016 will provide the first constraints on martian mantle discontinuities and better constrain the thickness and composition of the crust composition Constraints on the mantle size if coupled with better constraints on the thermodynamical properties of the mantle phase transitions can be used for better modeling and understanding of early martian mantle dynamics mantle convection rates of crustal production and evolution in basaltic composition Furthermore constraints on the crust and mantle melt density can be used to estimate the amount of melt that is stored within or below the crust relative to the amount of melt that reaches the surface and hence releases its volatiles into the atmosphere With the new data provided by the INSIGHT mission we thus aim to constrain the coupled interior atmosphere co evolution of Mars and its impact on the primitive habitability of the planet For this project we ask for a co financed thesis student to help in the analysis of the data that will be provided by InSight INSIGHT will also provide the first coupled geophysical and meteorological observatory on Mars We expect the mission to detect the micro seismic noise generated by the interaction of wind with the surface This will be used to monitor and constraint the structure of the atmospheric boundary layer dynamics and to constrainthe surface saltation processes Dune physics and the link with planetary climate During the last two years new collaborations have been established with the Chinese Academy of Science to develop a novel type of field experiment designed to examine the physics of sand dunes within their natural environment using controlled initial and boundary conditions This so called landscape scale experiment is a new and unique concept that is particularly well suited for validation and quantification purposes Given the extreme conditions encountered in arid deserts and the time scales associated with the development of bedforms in situ experiments on aeolian sand dunes have to combine logistics facilities with long term measurements By successfully meeting these challenges in China thanks to the local climate and the field expertise of Chinese scientists we will be able to obtain new experimental evidences for the formation of dunes and their alignment in multimodal wind regimes The current ANR project EXODUNES provides financial support for the two first missions of fall 2013 and spring 2014 and no PhD grant on that topic Considering the timescale of Earth s aeolian dune dynamics this fieldwork needs to be extended over several years up to 2017 at least and will provides a huge amount of data which will require the recruiting of a thesis student Hence the main objective of the Ph D thesis will be to continue the landscape scale experiment from fall 2014 to spring 2017 carrying out the field measurements and all the statistical data analysis From this we will have a unique set of data to investigate dune morphodynamics which is intended to be put in close relation to dune morphodynamics and climate on Earth and other planetary bodies were dunes have been observed Mars and Saturn largest moon Titan Of the three new thesis topics that are being proposed for this project this topic is the project s highest priority Planetary sciences Publication Time evolution of snow regions and planet traps in an evolving protoplanetary disk 6 May 2015 14 39 K Baillié S Charnoz and E Pantin members of Interface Project From dust to stars publish their results in the newspaper Astronomy Astrophysics Their article is entitled Time evolution of snow regions and planet traps in an evolving protoplanetary disk En savoir plus Publication New look at the origin and the growth mechanism of Titan dunes 6 October 2014 14 02 Titan the largest satellite of Saturn has a thick atmosphere dominated by nitrogen and carbon compounds This satellite has many similarities with Earth including a very active weather cucle essentially controlled by methane and many landscapes with extremely familar faces in particular huge fields of linea dunes around the equator Such dune are observed in many terrestrial deserts and even on Mars and are witnesses of the wind regimes and sedimentary environment that shaped them En savoir plus 07 10 2014 PUBLICATIONS Sept 2013 Sept 2014 1 PUBLICATIONS AND BOOKS 26 papers published or under review in total since september 2013 in international peer reviewed journal 2 papers in Science accepted 2 papers in Nature Geoscience under review Theme 1 1 Baillié K Charnoz S Time Evolution of a Viscous Protoplanetary Disk with a Free Geometry Toward a More Self consistent Picture 2014 Apj 786 id 35 2 Tajeddine R N Rambaux Lainey S charnoz and 3 co authors Constraints on Mimas interior from Cassini ISS libration measurements Accepted in SCIENCE publication in Nov 2014 3 S Charnoz J Aléon N Chaumard E Tailliffet Formation of CAI by coagulation and fragmentation Submitted to Icarus Moderate revisions required 4 Baillié K Charnoz S Pantin E Evolution of front regions and planet traps in an evolving protoplanetary disk Submitted to A A 5 Charnoz S Michaut C Dynamical and thermodynamical evolution of the protoluar disk Submitted to Icarus 6 Chaussidon M Liu M C Early Solar System processes from nebular gas to the precursors of the Earth AGU Monograph Early Earth under revision 7 Furi E Chaussidon M Marty B accepté Evidence for an early nitrogen isotopic evolution in the solar nebula from volatile analyses of a CV3 CAI Geochim Cosmochim Acta 8 Luu T H Young E D Gounelle M Chaussidon M en révision A short time interval for condensation of high temperature silicates in the solar accretion disk Proc Nat Acad Sci 9 Mishra R Chaussidon M 2014 Fossil records of high level of 60 Fe in chondrules from unequilibrated chondrites Earth Planet Sci Lett 398 90 100 10 Moreira M Charnoz S The origin of the neon isotopes in chondrites and Earth Submitted to EPSL 11 Paul S Savage Heng Chen Igor S Puchtel Gregory Shofner J Siebert J Badro F Moynier Under review Nature Geoscience 12 Moynier F et Fegley B The Earth s building blocks AGU monograph accepted with revisions 13 Chen H Moynier F Humayun M Bishop MC Williams J Cosmogenic effects on Cu isotopes in IVB iron meteorites Implications for the Hf W chronometry Geochimica et cosmochimica acta Accepted with revisions Theme 2 1 Miljković K M A Wieczorek G S Collins M Laneuville G A Neumann H J Melosh S C Solomon R J Phillips D E Smith and M T Zuber 2013 Asymmetric distribution of lunar impact basins caused by variations in target properties Science 342 724 726 doi 10 1126 science 1243224 2 Laneuville M M A Wieczorek D Breuer and N Tosi 2013 Asymmetric thermal evolution of the Moon J Geophys Res Planets 118 1435 1452 doi 10 1002 jgre 20103 3 Thorey C and C Michaut 2014 A model for the dynamics of crater centered intrusion Application to lunar floor fractured craters J Geophys Res Planets 119 286 312 doi 10 1002 2013JE004467 4 Laneuville M M A Wieczorek D Breuer J Aubert G Morard T Ru ckriemen 2014 A long lived lunar dynamo powered by core crystallization Earth Planet Sci Lett 401 251 260 doi 10 1016 j epsl 2014 05 057 5 Miljkovic K M A Wieczorek G S Collins S C Solomon D E Smith M T Zuber Excavation of the lunar mantle by basin forming events on the Moon Earth Planet Sci Lett in revision 6 Price M C Ramkissoon N K McMahon S Miljkovic K Parnell J Wozniakiewicz P J Kearsley A T Blamey N J F Cole M J Burchell M J 2014 Limits on methane release and

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  • I6: From dust to planets | UnivEarthS
    from experimental high pressure equilibrium volatilization condensation irradiation adsorption diffusion samples A new platform of experimental cosmochemistry is under construction at IPGP that aims to simulate some key physical processes regarding gas dust interaction Our approach will be developed in 5 tasks What do the age and composition of CAIs and chondrules really tell us about the formation of the solar system How can we constrain irradiation processes in the early solar system from analyses of lunar soil grains and meteoritic chondrules and CAIs Why and how did the isotopic composition of major volatiles elements O N and C change so rapidly in the inner accretion disk What is the origin of highly volatile elements in parent bodies from laboratory simulations of gas dust interactions How and when did the first planetesimals form As disk observations and laboratory measurements will provide constrains on the transport of solids it will be necessary to provide scenarios of large scale transport relying on the physics of gaseous and dusty protoplanetary disks based on numerical simulations On this side AIM is leading the development of a large modeling program focusing on the transport of the first solids in the protoplanetary disk and their incorporation into embryos including turbulent dynamics radiative effects and planet disk interactions Simple chemical and isotopic fractionation models will be included into simulations of turbulent dust transport in order to test different scenarios to interpret isotopic data Three important modeling tasks will be lead Development of a dust transport model in the protoplanetary disk taking into account turbulence and dust condensation refractories near the Sun and volatiles near the snow line Coupling of the dust transport model with a radiative transfer code in order to create synthetic images to space observation of disks Development of a protoplanetary disk thermodynamical model in order to constrain the condition of formation of dust in order to compare with laboratory data Estimation of the irradiation flux of dust in the disk in order to calibrate experiments of fractionation of dust under irradiation Beside the earliest phases of planet formation N body simulations of embryo transport in the disk in the frame of the Nice model will be lead to constrain the radial origin of the building blocks that assembled into the modern terrestrial planets This will lead naturally to interactions with research theme 2 that concerns itself with the initial differentiation and interior structure of the terrestrial planets Differentiation interior structure and geologic evolution of the terrestrial planets The processes that took place during the initial differentiation of the Earth are reasonable well understood the composition of the major chemical reservoirs crust mantle and core are relatively well known and the manner by which internal heat is lost to space via plate tectonics is understood from both observational of modeling perspectives For the other terrestrial planets however our understanding of these processes is considerably more limited and many first order questions remain unresolved For example What is the thickness and composition of the crust of Mercury the Moon and Mars At what depths do the major phase transitions occur in the mantles of Mars and Venus and how do these phase transitions affect mantle convection and plume dynamics What is the size of the metallic core of Mercury Mars and the Moon And what are the abundances of light alloying elements such as sulfur carbon and silicon in the liquid portion of their cores Do Mercury Mars and the Moon possess a solid inner core And is core crystallization the source of energy that is powering the dynamo generated magnetic field of Mercury today What was the energy source that powered the early dynamos of Mars and the Moon and why did their dynamos later shut off To address these and other question this project will rely upon a three pronged approach making use of geophysical data collected by planetary missions high pressure laboratory experiments and numerical and geophysical modeling Members of this research axe are currently involved in several NASA and ESA planetary missions at both the co investigator and principal investigator level including NASA s geophysical missions to the Moon GRAIL and Mars InSight and ESA s orbital missions to Mercury BepiColumbo and Jupiter JUICE Furthermore members of our project have recently finished the construction of a world class high pressure geo materials laboratory that is currently making its first measurements Together these datasets will offer us a unique perspective to unravel the above listed questions concerning the differentiation interior evolution and geologic evolution of the terrestrial planets The first two years of the UnivEarthS I1 project funded our analyses of lunar gravitational data acquired during the primary mission of the Gravity Recovery and Interior Laboratory GRAIL mission Results from our group have shown that the crust of the Moon is significantly thinner than once thought that the crust has been highly fractured by billions of years of impact cratering and that lateral variations in crustal temperature have had a dramatic influence on the morphology of giant impact basins During this initial stage of analysis the UnivEarthS funded a LabEx postdoc and contributed to the publications of two articles in the journal Science We now have at our disposal gravitational data from the extended mission which has a spatial resolution that is two times better than that acquired during the primary mission Over the following three years we aim to study processes that were previously beyond reach such as the gravitational signature of magnetic anomalies and magmatic intrusions and the subsurface structure of medium sized simple and complex impact craters For these studies we ask that the UnivEarthS LabEx fund a post doc in additional to our initial demand three years ago At the time the initial UnivEarthS proposal was selected our group anticipated on providing a seismometer to the Japanese lunar geophysical mission SELENE 2 with a launch near 2018 Since this time NASA selected the Martian geophysical mission InSight which will be launched and land on Mars in 2016 Members of our research group are providing at the principal investigator level the sole instrument that is above the mission s science threshold This instrument is the very broad band seismometer that is being developed at IPGP and which will make the first seismic measurements ever on the surface of Mars Data from this mission will constrain the size of the martian core determine if a solid inner core exists determine the thickness of the crust and search for seismic discontinuities in the mantle among other objectives The UnivEarthS project previously agreed to fund a LabEx postdoc and a co financed thesis student for seismic analysis related to the SELENE 2 mission and these resources will be redirected towards the InSight mission in this revised project In addition to our initial demand we ask the UnivEarthS LabEx for an additional co financed thesis student to help with the flood of data that will arrive when InSight lands on Mars in 2016 The proposed experimental approach aims at combining astrophysical models of planetary accretion with geochemical models of planetary differentiation and cosmochemical constraints provided by meteorites During the first two years funded by the UnivEarthS LabEx the young research group JE1 developed protocols to use the laser heated diamond anvil cell for studying the geochemical imprint of planetary core formation We have shown notably in a recent publication in Science that the partitioning of slightly siderophile elements V and Cr during core formation imply that accretion of the Earth could have occurred under conditions that were more oxidizing than previously thought In this way Earth can accrete from materials as oxidized as the most common meteorites i e ordinary or carbonaceous chondrites and imply large mixing of proto planetary materials in the inner solar system Similarly Ni and Co partitioning shows clearly that the core cannot form at pressures lower than 35 GPa nor can it form at pressure higher than 65 GPa bracketing for the first time the depth of the terrestrial magma ocean in the first 50 million years after the birth of the Solar System The research we propose to develop over the next 5 years will help us constrain and understand the primordial differentiation of terrestrial bodies in the Solar System We plan to understand the early evolution of Vesta by combining high precision isotope geochemistry with experimental geochemistry through the study of isotopic fractionation of siderophile and volatile elements Si Cr Ga Cu Zn Sn as well as moderately siderophile elements W Mo One of the aims is to understand the accretion of the so called Late Veneer on small planetary embryos These studies can be applied to understanding the Earth Moon system after the giant impact through the comparison between Apollo samples and experimental charges once again with a special focus on volatile elements and their isotropic fractionation We have access to a very large collection of SNCs and have plans to propose refined models of Martian differentiation to understand the processes that can occur in a very short timescale and compare it with the relatively long timescale of terrestrial accretion These studies all require a savvy mix of experiments and cosmochemical observation and access to rare samples and represent a perfect integration of the experimentalists in this proposal with the cosmochemists Planetary interfaces atmosphere surface interior interactions The atmosphere of planetary body with no plate tectonics mainly forms and survives through the release of volatiles from the mantle or ice shell by volcanism or cryovolcanism and the persistence of surface reservoirs for those volatiles The presence and survival of an atmosphere provides in that way a window into the evolution of the volcanic activity the atmospheric dynamics and composition climate and the geology and geodynamics of a planetary body The aim of research theme 3 is thus to study the strong coupling between planetary bodies interiors surfaces and atmospheres constraining their concomitant formation and evolution throughout the age of the Solar System This axis combines the joint characterization of the solid and fluid envelops of terrestrial planets satellites and exoplanets following a complete comparative planetology approach with Mars Titan and exoplanets with an atmosphere as archetypes in a multi disciplinary way This project will include analysis of planetary mission data numerical simulations and laboratory experiments Atmosphere interior habitability coupling on Mars The INSIGHT mission planned to land on Mars in 2016 will provide the first constraints on martian mantle discontinuities and better constrain the thickness and composition of the crust composition Constraints on the mantle size if coupled with better constraints on the thermodynamical properties of the mantle phase transitions can be used for better modeling and understanding of early martian mantle dynamics mantle convection rates of crustal production and evolution in basaltic composition Furthermore constraints on the crust and mantle melt density can be used to estimate the amount of melt that is stored within or below the crust relative to the amount of melt that reaches the surface and hence releases its volatiles into the atmosphere With the new data provided by the INSIGHT mission we thus aim to constrain the coupled interior atmosphere co evolution of Mars and its impact on the primitive habitability of the planet For this project we ask for a co financed thesis student to help in the analysis of the data that will be provided by InSight INSIGHT will also provide the first coupled geophysical and meteorological observatory on Mars We expect the mission to detect the micro seismic noise generated by the interaction of wind with the surface This will be used to monitor and constraint the structure of the atmospheric boundary layer dynamics and to constrainthe surface saltation processes Dune physics and the link with planetary climate During the last two years new collaborations have been established with the Chinese Academy of Science to develop a novel type of field experiment designed to examine the physics of sand dunes within their natural environment using controlled initial and boundary conditions This so called landscape scale experiment is a new and unique concept that is particularly well suited for validation and quantification purposes Given the extreme conditions encountered in arid deserts and the time scales associated with the development of bedforms in situ experiments on aeolian sand dunes have to combine logistics facilities with long term measurements By successfully meeting these challenges in China thanks to the local climate and the field expertise of Chinese scientists we will be able to obtain new experimental evidences for the formation of dunes and their alignment in multimodal wind regimes The current ANR project EXODUNES provides financial support for the two first missions of fall 2013 and spring 2014 and no PhD grant on that topic Considering the timescale of Earth s aeolian dune dynamics this fieldwork needs to be extended over several years up to 2017 at least and will provides a huge amount of data which will require the recruiting of a thesis student Hence the main objective of the Ph D thesis will be to continue the landscape scale experiment from fall 2014 to spring 2017 carrying out the field measurements and all the statistical data analysis From this we will have a unique set of data to investigate dune morphodynamics which is intended to be put in close relation to dune morphodynamics and climate on Earth and other planetary bodies were dunes have been observed Mars and Saturn largest moon Titan Of the three new thesis topics that are being proposed for this project this topic is the project s highest priority Planetary sciences Publication Time evolution of snow regions and planet traps in an evolving protoplanetary disk 6 May 2015 14 39 K Baillié S Charnoz and E Pantin members of Interface Project From dust to stars publish their results in the newspaper Astronomy Astrophysics Their article is entitled Time evolution of snow regions and planet traps in an evolving protoplanetary disk En savoir plus Publication New look at the origin and the growth mechanism of Titan dunes 6 October 2014 14 02 Titan the largest satellite of Saturn has a thick atmosphere dominated by nitrogen and carbon compounds This satellite has many similarities with Earth including a very active weather cucle essentially controlled by methane and many landscapes with extremely familar faces in particular huge fields of linea dunes around the equator Such dune are observed in many terrestrial deserts and even on Mars and are witnesses of the wind regimes and sedimentary environment that shaped them En savoir plus 07 10 2014 PUBLICATIONS Sept 2013 Sept 2014 1 PUBLICATIONS AND BOOKS 26 papers published or under review in total since september 2013 in international peer reviewed journal 2 papers in Science accepted 2 papers in Nature Geoscience under review Theme 1 1 Baillié K Charnoz S Time Evolution of a Viscous Protoplanetary Disk with a Free Geometry Toward a More Self consistent Picture 2014 Apj 786 id 35 2 Tajeddine R N Rambaux Lainey S charnoz and 3 co authors Constraints on Mimas interior from Cassini ISS libration measurements Accepted in SCIENCE publication in Nov 2014 3 S Charnoz J Aléon N Chaumard E Tailliffet Formation of CAI by coagulation and fragmentation Submitted to Icarus Moderate revisions required 4 Baillié K Charnoz S Pantin E Evolution of front regions and planet traps in an evolving protoplanetary disk Submitted to A A 5 Charnoz S Michaut C Dynamical and thermodynamical evolution of the protoluar disk Submitted to Icarus 6 Chaussidon M Liu M C Early Solar System processes from nebular gas to the precursors of the Earth AGU Monograph Early Earth under revision 7 Furi E Chaussidon M Marty B accepté Evidence for an early nitrogen isotopic evolution in the solar nebula from volatile analyses of a CV3 CAI Geochim Cosmochim Acta 8 Luu T H Young E D Gounelle M Chaussidon M en révision A short time interval for condensation of high temperature silicates in the solar accretion disk Proc Nat Acad Sci 9 Mishra R Chaussidon M 2014 Fossil records of high level of 60 Fe in chondrules from unequilibrated chondrites Earth Planet Sci Lett 398 90 100 10 Moreira M Charnoz S The origin of the neon isotopes in chondrites and Earth Submitted to EPSL 11 Paul S Savage Heng Chen Igor S Puchtel Gregory Shofner J Siebert J Badro F Moynier Under review Nature Geoscience 12 Moynier F et Fegley B The Earth s building blocks AGU monograph accepted with revisions 13 Chen H Moynier F Humayun M Bishop MC Williams J Cosmogenic effects on Cu isotopes in IVB iron meteorites Implications for the Hf W chronometry Geochimica et cosmochimica acta Accepted with revisions Theme 2 1 Miljković K M A Wieczorek G S Collins M Laneuville G A Neumann H J Melosh S C Solomon R J Phillips D E Smith and M T Zuber 2013 Asymmetric distribution of lunar impact basins caused by variations in target properties Science 342 724 726 doi 10 1126 science 1243224 2 Laneuville M M A Wieczorek D Breuer and N Tosi 2013 Asymmetric thermal evolution of the Moon J Geophys Res Planets 118 1435 1452 doi 10 1002 jgre 20103 3 Thorey C and C Michaut 2014 A model for the dynamics of crater centered intrusion Application to lunar floor fractured craters J Geophys Res Planets 119 286 312 doi 10 1002 2013JE004467 4 Laneuville M M A Wieczorek D Breuer J Aubert G Morard T Ru ckriemen 2014 A long lived lunar dynamo powered by core crystallization Earth Planet Sci Lett 401 251 260 doi 10 1016 j epsl 2014 05 057 5 Miljkovic K M A Wieczorek G S Collins S C Solomon D E Smith M T Zuber Excavation of the lunar mantle by basin forming events on the Moon Earth Planet Sci Lett in revision 6 Price M C Ramkissoon N K McMahon S Miljkovic K Parnell J Wozniakiewicz P J Kearsley A T Blamey N J F Cole M J Burchell M J 2014 Limits on methane release

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  • Publication : Time evolution of snow regions and planet traps in an evolving protoplanetary disk | UnivEarthS
    Earth as a living planet From the Big Bang to the future Universe Support au PCCP The transient catastrophic Universe Interface projects Geoparticles Fundamental physics and Geophysics in space From dust to planets Former Interface projects Formation and early evolution of Planetary systems The youth of cosmic rays and their emergence in the interstellar clouds Gamma ray instrumentation development Young team project Experimental geophysics Valorization project Data distribution visualisation and cloud computing PUBLICATIONS EDUCATIONAL Nanosatellite student project IGOsat UnivEarthS JOB OPPORTUNITY Experimental Dark Matter Search Post Doctoral Research Fellow IGOSat internship PhD position Effect of the North South dichotomy on the thermal structure and evolution of Mars Search this site October Mon Tue Wed Thu Fri Sat Sun 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31 Sign in Password forgotten Home OVERVIEW Scientific areas Publication Time evolution of snow regions and planet traps in an evolving protoplanetary disk 06 05 2015 K Baillié S Charnoz and E Pantin members of Interface Project From dust to stars publish their results in the newspaper Astronomy Astrophysics Their article is

    Original URL path: http://www.univearths.fr/en/publication-time-evolution-snow-regions-and-planet-traps-evolving-protoplanetary-disk (2015-10-10)
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