The induced magnetospheres of mars, venus, and titan

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This article summarizes and aims at comparing the main features of the induced magnetospheres of Mars, Venus and Titan. All three objects form a well-defined induced magnetosphere (IM) and magnetotail as a consequence of the interaction of an external wind of plasma with the ionosphere and the exosp...

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Autor principal: Bertucci, César Luis Fermín
Otros Autores: Duru, F., Edberg, N., Fraenz, M., Martinecz, C., Szego, K., Vaisberg, O.
Formato: Capítulo de libro
Lenguaje:Inglés
Publicado: 2011
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Acceso en línea:Registro en Scopus
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Biblioteca Central Dr. Luis F. Leloir (FCEN) de Universidad de Buenos Aires
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245 1 4 |a The induced magnetospheres of mars, venus, and titan 
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270 1 0 |m Bertucci, C.; Institute for Astronomy and Space Physics (IAFE), CONICET, UBA, Buenos Aires, Argentina; email: cbertucci@iafe.uba.ar 
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506 |2 openaire  |e Política editorial 
520 3 |a This article summarizes and aims at comparing the main features of the induced magnetospheres of Mars, Venus and Titan. All three objects form a well-defined induced magnetosphere (IM) and magnetotail as a consequence of the interaction of an external wind of plasma with the ionosphere and the exosphere of these objects. In all three, photoionization seems to be the most important ionization process. In all three, the IM displays a clear outer boundary characterized by an enhancement of magnetic field draping and massloading, along with a change in the plasma composition, a decrease in the plasma temperature, a deflection of the external flow, and, at least for Mars and Titan, an increase of the total density. Also, their magnetotail geometries follow the orientation of the upstream magnetic field and flow velocity under quasi-steady conditions. Exceptions to this are fossil fields observed at Titan and the near Mars regions where crustal fields dominate the magnetic topology. Magnetotails also concentrate the escaping plasma flux from these three objects and similar acceleration mechanisms are thought to be at work. In the case of Mars and Titan, global reconfiguration of the magnetic field topology (reconnection with the crustal sources and exits into Saturn's magnetosheath, respectively) may lead to important losses of plasma. Finally, an ionospheric boundary related to local photoelectron signals may be, in the absence of other sources of pressure (crustal fields) a signature of the ultimate boundary to the external flow. © 2011 Springer Science+Business Media B.V.  |l eng 
536 |a Detalles de la financiación: National Research Council of Science and Technology 
536 |a Detalles de la financiación: Consejo Nacional de Investigaciones Científicas y Técnicas 
536 |a Detalles de la financiación: Acknowledgements Authors thank the International Space Science Institute (ISSI) for supporting this work. CB is supported by the National Science and Technology Research Council (CONICET) and the Agency for the Promotion of Science and Technology of Argentina. 
536 |a Detalles de la financiación: NJTE was supported by the Swedish Institute of Space Physics through a grant from the Swedish Science Council (Vetenskapsrådet). 
593 |a Institute for Astronomy and Space Physics (IAFE), CONICET, UBA, Buenos Aires, Argentina 
593 |a Department of Astronomy, Unversity of Iowa, Iowa City, United States 
593 |a Swedish Space Science Institute, Uppsala, Sweden 
593 |a Max Planck Institute for Solar System Research, Klatenburg-Lindau, Germany 
593 |a KFKI-RMKI, Budapest, Hungary 
593 |a Space Research Institute, Russian Academy of Sciences, Moscow, Russian Federation 
650 1 7 |2 spines  |a VENUS 
650 1 7 |2 spines  |a VENUS 
690 1 0 |a BOUNDARIES 
690 1 0 |a DRAPING 
690 1 0 |a INDUCED MAGNETOSPHERES 
690 1 0 |a MARS 
690 1 0 |a MASSLOADING 
690 1 0 |a TITAN 
690 1 0 |a DRAPING 
690 1 0 |a INDUCED MAGNETOSPHERES 
690 1 0 |a MARS 
690 1 0 |a MASSLOADING 
690 1 0 |a TITAN 
690 1 0 |a INTERPLANETARY FLIGHT 
690 1 0 |a IONIZATION 
690 1 0 |a IONOSPHERE 
690 1 0 |a MAGNETIC FIELDS 
690 1 0 |a MAGNETOSPHERE 
690 1 0 |a SEMICONDUCTOR INSULATOR BOUNDARIES 
690 1 0 |a TOPOLOGY 
690 1 0 |a MAGNETOPLASMA 
700 1 |a Duru, F. 
700 1 |a Edberg, N. 
700 1 |a Fraenz, M. 
700 1 |a Martinecz, C. 
700 1 |a Szego, K. 
700 1 |a Vaisberg, O. 
773 0 |d 2011  |g v. 162  |h pp. 113-171  |k n. 1-4  |p Space Sci Rev  |x 00386308  |w (AR-BaUEN)CENRE-6897  |t Space Science Reviews 
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