Academic literature on the topic 'Corps planétaires'
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Journal articles on the topic "Corps planétaires":
Melucci, Alberto. "Rythmes internes et rythmes sociaux dans un monde planétaire." Les pratiques sociales d’ailleurs 10, no. 2 (January 28, 2008): 195–202. http://dx.doi.org/10.7202/301414ar.
Dionne, Jean-Claude. "Peulvast, Jean-Pierre et Vanney, Jean-René, 2001. Géomorphologie structurale : terre, corps planétaires solides ; Tome 1 : Relief et structure. Co-édition Gordon and Breach Science Publishers, Paris, Éditions du BRGM, Orléans, et Société géologique de France, Paris, 505 p., 436 fig., 14 tabl., 17 X 24,5 cm ; 45 m ; ISBN-2-88449-063-9." Géographie physique et Quaternaire 55, no. 2 (2001): 193. http://dx.doi.org/10.7202/008304ar.
Aloisi, Giovanni. "Les océans au bord de la crise d'asthme." La Météorologie, no. 125 (2024): 019. http://dx.doi.org/10.37053/lameteorologie-2024-0032.
Gagné, Karine. "Vital Bodies." Social Anthropology/Anthropologie Sociale 32, no. 1 (March 1, 2024): 13–29. http://dx.doi.org/10.3167/saas.2024.320103.
"Géomorphologie structurale. Terre, corps planétaires solides. Tome 1. Relief et structure Jean-Pierre Peulvast, Jean-René Vanney Gordon and Breach, 516 p., 295 F." Nature Sciences Sociétés 9, no. 3 (September 2001): 92. http://dx.doi.org/10.1016/s1240-1307(01)80079-0.
Canals, Roger. "Culte à María Lionza." Anthropen, 2016. http://dx.doi.org/10.17184/eac.anthropen.005.
Dissertations / Theses on the topic "Corps planétaires":
Sezestre, Elie. "Les poussières et petits corps des systèmes planétaires extrasolaires." Thesis, Université Grenoble Alpes (ComUE), 2019. http://www.theses.fr/2019GREAY022/document.
During my thesis, I numerically simulated the dynamical behaviour of dust and small grains around stars, applied to two ranges of stellar distance : debris disks and exozodis.Concerning debris disks, I focused on the fast moving arch-like structures observed over 15 years inside the disk of AU Mic. Supposing that they all come from a single parent body and that the dust composing the arches have the same dynamics, I showed that the parent body must be closer-in than the planetesimal belt (<25 au), on a circular orbit or static with respect to the observer. Grains must be submicronic in order to explain the apparent velocity of the arches, gained by means of stellar wind pressure. Large-scale magnetic field of the star is large enough to explain the vertical extent of the arches, but require further investigations.I also developped a numerical code in order to test the dynamical origin of dust composing exozodis, to compare its results to the observations. I showed that the classical PR-drag scenario involving grains drifting inward from a distant cold parent belt produce an excess flux in mid-infrared compared to the near-infrared, unbalanced by the pile-up. The cometary scenario, by producing dust very close to the star, emits less in mid-infrared. A ten of kilometric comets can reproduce the flux levels observed around all stars. This numerical code is also able to handle the DDE, the stellar wind pressure or the magnetic field.During my work, I showed that taking into account the dust dynamics can constrain the dust physical properties. I developped adaptative numerical tools that can handle the variety and complexity of dust observed around stars
Farago, François. "Quelques aspects de la dynamique des systèmes planétaires extrasolaires." Observatoire de Paris (1667-....), 2010. https://hal.science/tel-02094983.
The doctoral thesis presents analytical methods to study the dynamics of systems of bodies under their mutual gravitational interactions. It is motivated by the great diversity of properties and behaviors exhibited by extrasolar planetery systems. However, the methods which we present here can also apply in other contexts such as the study of multiple stellar systems or the study of stellar populations around compact objects in the galactic center. We widely use secular models because they allow a simplification in the equations as well as a considerable speed-up in numerical computations. This last aspect is critical when a large set of initial conditions must be explored. We first derive a semi-secular model which is adapted to the study of a system where one of the bodies is much closer to the central body than the other ones. This model is illustrated on the multi-planetary system around mu Arae. The vectorial formalism used throughout this doctoral work is also introduced. The second part of this thesis studies the quadripolar and secular three-body problem. Al ready explored by Ferrer and Osacar (1994), it is an integrable problem. We give a formulation of the problem which allows it to be very easily connected to its to extreme interior (Kozai, 1962) and exterior (Palacian, 2006) cases. We use this formulation to explain the results obtained by Verrier and Evans (2009). The last part of the thesis focuses on the addition of tidal interactions in systems dominated by Kozai's mechanism. We derive a model of this situation and apply it to the case of HD 80606b which is the most eccentric extrasolar planet discovered with an eccentricity of e=0. 93
Sonzogni, Yann. "Les inclusions magmatiques : des cinétiques de croissance cristalline à la formation des corps planétaires." Phd thesis, Université Blaise Pascal - Clermont-Ferrand II, 2011. http://tel.archives-ouvertes.fr/tel-00657302.
Charnoz, Sébastien. "Contribution à l'étude des disques planétaires et protoplanétaires perturbés." Paris 7, 2000. http://www.theses.fr/2000PA077039.
Besserer, Jonathan. "Approche numérique du couplage par effets de marée entre transferts thermiques internes et évolution orbitale des corps planétaires." Nantes, 2012. https://archive.bu.univ-nantes.fr/pollux/show/show?id=f0de8511-7668-460e-824c-00b47c604729.
Tidal effects that occur in some objects of the Solar System, and probably in a great part of the extrasolar planets detected so far, associate the viscous friction induced by the periodic deformation of their internal, possibly external layers (atmosphere and oceans), to a change of their orbital parameters. Since tidal dissipation strongly depends on rheology, hence on temperature, there is a natural coupling between these effects and heat transfer inside planetary bodies. This thesis was devoted to the building of a numerical model that self-consistently simulates thermal convection in a compressible mantle with variable viscosity and subjected to heterogeneous tidal heating, and the orbital evolution of the body. Conservation equations for mantle dynamics are treated by a finite volume method based on the bi-dimensional spherical annulus geometry; this approach approximates three-dimensional heat transfer while keeping moderate computational time. In particular, a multigrid mechanical solver and a high resolution advection scheme for the heat equation were implemented. The dissipation of tidal energy, which influences orbital evolution, is then computed through a semi-analytical solution derived during this work. Two preliminary applications are presented to investigate, on one hand the influence of compressibility in the treatment of the convection problem coupled with tidal dissipation and, on the other hand the effect of this coupling on orbital evolution
Boyet, Maud. "Anomalies isotopiques du système 146Sm-142Nd : Evolution précoce et dynamique interne de la Terre et d'autres corps planétaires différenciés." Lyon, École normale supérieure (sciences), 2003. http://www.theses.fr/2003ENSL0258.
Morard, Guillaume. "Les systèmes Fe-FeS et Fe-S-Si à haute pression et haute température : implications pour les noyaux des corps planétaires." Paris, Institut de physique du globe, 2006. http://www.theses.fr/2006GLOB0011.
Niederman, Laurent. "Résonances et stabilité dans le problème planétaire : solutions de seconde espèce." Paris 6, 1993. http://www.theses.fr/1993PA066615.
Robutel, Philippe. "Contribution à l'étude de la stabilité du problème planétaire des trois-corps." Observatoire de Paris (1667-....), 1993. https://hal.science/tel-02153557.
Deligny, Cécile. "Origine des éléments volatils et chronologie de leur accrétion au sein du Système Solaire interne : Apport de l'analyse in-situ des achondrites." Electronic Thesis or Diss., Université de Lorraine, 2021. http://www.theses.fr/2021LORR0329.
Volatile elements such as hydrogen and nitrogen control the evolution of planetary bodies and their atmospheres, and are essential elements for the development of life on Earth. Nevertheless, the origin of volatile elements and the timing of their accretion by terrestrial planets formed in the inner solar system remains a subject of debate and controversy in planetary science. To answer these questions, the isotopic ratios of hydrogen (D/H) and nitrogen (15N/14N) are powerful tools to trace the origin (solar, chondritic or cometary) of volatile elements trapped in planetary bodies. Therefore, to constrain the source(s) of volatile elements trapped in rocky planets, we analyzed hydrogen and nitrogen contents and isotopic compositions by ion microprobe (LGSIMS) in achondrites that originate from asteroids or from planets that are assumed to have formed in the inner solar system. These meteorites preserve a record of the initial stages of the formation of their parent bodies and can constrain the early evolution of planetary volatile elements. In-situ analysis by SIMS is a quasi-non-destructive technique, which permits to measure the abundance and the isotopic composition of volatile elements of different phases in terrestrial, extraterrestrial and synthetic samples. The recent development of the protocol of nitrogen analysis in silicate samples by ion probe allows us to target tens of micron- sized objects (i.e., glassy melt inclusions). Volatile elements were measured in melt inclusions trapped in minerals and in interstitial glasses. Although the analysis of nitrogen in aubrites was unsuccessful, the analysis performed on Martian meteorites and angrites revealed the presence of a large amount of water and nitrogen within these meteorites. In particular, the study of angrites and more precisely the meteorite D'Orbigny allowed us to highlight the presence of water and nitrogen having isotopic composition similar to those of the primitive meteorites formed in the outer solar system (i.e., CM-like carbonaceous chondrites). These results imply that these volatile elements must have been present in the inner solar system within the first ~4 Ma after CAI formation (i.e., the first solids to form in the solar system) and may have been trapped by the terrestrial planets during their formation. Furthermore, the analysis of Martian meteorites and more particularly of Chassigny revealed the presence of nitrogen with an isotopic composition enriched in 15N compared to enstatite chondrites and terrestrial diamonds which are believed to record the most primitive value of nitrogen on Earth
Book chapters on the topic "Corps planétaires":
LAMY, Laurent. "L’interaction des corps du Système solaire avec le milieu interplanétaire." In Le Système solaire 1, 101–67. ISTE Group, 2021. http://dx.doi.org/10.51926/iste.9033.ch3.