Search

Your search keyword '"Full kinetic model"' showing total 4 results
Start Over Descriptor "Full kinetic model"
4 results on '"Full kinetic model"'

2. Computational Plasma Physics

Author

Schneider, R., Kleiber, R., Beig, R., editor, Beiglböck, W., editor, Domcke, W., editor, Englert, B.-G., editor, Frisch, U., editor, Hänggi, P., editor, Hasinger, G., editor, Hepp, K., editor, Hillebrandt, W., editor, Imboden, D., editor, Jaffe, R. L., editor, Lipowsky, R., editor, Löhneysen, H. v., editor, Ojima, I., editor, Sornette, D., editor, Theisen, S., editor, Weise, W., editor, Wess, J., editor, Zittartz, J., editor, Dinklage, Andreas, editor, Klinger, Thomas, editor, Marx, Gerrit, editor, and Schweikhard, Lutz, editor

Published
2005
Full Text
View/download PDF

3. Modeling of Venus, Mars, and Titan.

Author

Kallio, Esa, Chaufray, Jean-Yves, Modolo, Ronan, Snowden, Darci, and Winglee, Robert

Subjects
*COMPUTER performance, *MONTE Carlo method, *PLASMA gases, *MAGNETOHYDRODYNAMICS, *MAGNETIC fields, *VENUS (Planet), *MARS (Planet), *TITAN (Satellite)
Abstract

Increased computer capacity has made it possible to model the global plasma and neutral dynamics near Venus, Mars and Saturn's moon Titan. The plasma interactions at Venus, Mars, and Titan are similar because each possess a substantial atmosphere but lacks a global internally generated magnetic field. In this article three self-consistent plasma models are described: the magnetohydrodynamic (MHD) model, the hybrid model and the fully kinetic plasma model. Chamberlain and Monte Carlo models of the Martian exosphere are also described. In particular, we describe the pros and cons of each model approach. Results from simulations are presented to demonstrate the ability of the models to capture the known plasma and neutral dynamics near the three objects. [ABSTRACT FROM AUTHOR]

Published
2011
Full Text
View/download PDF

4. Modeling of Venus, Mars, and Titan

Author

Darci Snowden, Jean-Yves Chaufray, Ronan Modolo, Robert Winglee, Esa Kallio, Finnish Meteorological Institute (FMI), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), 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)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Department of Earth and Space Sciences [Seattle], University of Washington [Seattle], European Union (EU), Agence Nationale de la Recherche (ANR), ANR-09-JCJC-0038,CAT,Physico-Chimie organique de l'atmosphère de Titan(2009), ANR-09-BLAN-0223,HELIOSARES,Relation Soleil ? Mars: description et analyse des échanges présents et passés entre magnétosphère et atmosphère(2009), European Project: 228319,EC:FP7:INFRA,FP7-INFRASTRUCTURES-2008-1,EUROPLANET RI(2009), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)

Subjects
Magnetohydrodynamic model, Planetary exospheres, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Monte Carlo method, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mars, Venus, Planetary magnetospheres, 7. Clean energy, 01 natural sciences, Astrobiology, symbols.namesake, Full kinetic model, Physics::Plasma Physics, Numerical modeling, 0103 physical sciences, Exosphere model, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Martian, Physics, biology, Astronomy and Astrophysics, Mars Exploration Program, biology.organism_classification, Planetary science, Space and Planetary Science, Physics::Space Physics, symbols, Astrophysics::Earth and Planetary Astrophysics, Magnetohydrodynamics, Titan, Titan (rocket family), Hybrid model, Exosphere
Abstract

International audience Increased computer capacity has made it possible to model the global plasma and neutral dynamics near Venus, Mars and Saturn's moon Titan. The plasma interactions at Venus, Mars, and Titan are similar because each possess a substantial atmosphere but lacks a global internally generated magnetic field. In this article three self-consistent plasma models are described: the magnetohydrodynamic (MHD) model, the hybrid model and the fully kinetic plasma model. Chamberlain and Monte Carlo models of the Martian exosphere are also described. In particular, we describe the pros and cons of each model approach. Results from simulations are presented to demonstrate the ability of the models to capture the known plasma and neutral dynamics near the three objects.

Published
2011

Catalog

Books, media, physical & digital resources
See catalog results