Titan's interaction with the supersonic solar wind

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After 9 years in the Saturn system, the Cassini spacecraft finally observed Titan in the supersonic and super-Alfvénic solar wind. These unique observations reveal that Titan's interaction with the solar wind is in many ways similar to unmagnetized planets Mars and Venus and active comets in sp...

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Autor principal: Bertucci, César Luis Fermín
Otros Autores: Hamilton, D.C, Kurth, W.S, Hospodarsky, G., Mitchell, D., Sergis, N., Edberg, N.J.T, Dougherty, M.K
Formato: Capítulo de libro
Lenguaje:Inglés
Publicado: Blackwell Publishing Ltd 2015
Materias:
VENUS
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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100 1 |a Bertucci, César Luis Fermín 
245 1 0 |a Titan's interaction with the supersonic solar wind 
260 |b Blackwell Publishing Ltd  |c 2015 
270 1 0 |m Bertucci, C.; Instituto de Astronomía y Física Del Espacio (CONICET/UBA), Ciudad UniversitariaArgentina 
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504 |a Ulusen, D., Comparisons of Cassini flybys of the Titan magnetospheric interaction with an MHD model: Evidence for organized behavior at high altitudes (2012) Icarus, 217 (1), pp. 43-54 
504 |a Wei, H.Y., Russell, C.T., Dougherty, M.K., Neubauer, F.M., Ma, Y.J., Upper limits on Titan's magnetic moment and implications for its interior (2010) J. Geophys. Res., 115, p. E10007 
504 |a Zhang, T.L., Luhmann, J., Russell, C., The magnetic barrier at Venus (1991) J. Geophys. Res., 96, p. 11 
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506 |2 openaire  |e Política editorial 
520 3 |a After 9 years in the Saturn system, the Cassini spacecraft finally observed Titan in the supersonic and super-Alfvénic solar wind. These unique observations reveal that Titan's interaction with the solar wind is in many ways similar to unmagnetized planets Mars and Venus and active comets in spite of the differences in the properties of the solar plasma in the outer solar system. In particular, Cassini detected a collisionless, supercritical bow shock and a well-defined induced magnetosphere filled with mass-loaded interplanetary magnetic field lines, which drape around Titan's ionosphere. Although the flyby altitude may not allow the detection of an ionopause, Cassini reports enhancements of plasma density compatible with plasma clouds or streamers in the flanks of its induced magnetosphere or due to an expansion of the induced magnetosphere. Because of the upstream conditions, these observations may be also relevant to other bodies in the outer solar system such as Pluto, where kinetic processes are expected to dominate. © 2015. American Geophysical Union. All Rights Reserved.  |l eng 
536 |a Detalles de la financiación: Science and Technology Facilities Council, STFC, ST/K001051/1 
593 |a Instituto de Astronomía y Física Del Espacio (CONICET/UBA), Ciudad Universitaria, Buenos Aires, Argentina 
593 |a Physics Department, University of Maryland, College Park, MD, United States 
593 |a Department of Physics and Astronomy, University of Iowa, Iowa City, IA, United States 
593 |a Applied Physics Laboratory, Johns Hopkins University, Baltimore, MD, United States 
593 |a Office for Space Research, Academy of Athens, Athens, Greece 
593 |a Swedish Institute of Space Physics, Uppsala, Sweden 
593 |a Blackett Laboratory, Imperial College London, London, United Kingdom 
650 1 7 |2 spines  |a VENUS 
650 1 7 |2 spines  |a VENUS 
690 1 0 |a MARS 
690 1 0 |a SOLAR WIND 
690 1 0 |a TITAN 
690 1 0 |a INTERPLANETARY FLIGHT 
690 1 0 |a IONOSPHERE 
690 1 0 |a MAGNETOSPHERE 
690 1 0 |a PLANETS 
690 1 0 |a PLASMA DENSITY 
690 1 0 |a SOLAR WIND 
690 1 0 |a CASSINI SPACECRAFT 
690 1 0 |a INDUCED MAGNETOSPHERES 
690 1 0 |a INTERPLANETARY MAGNETIC FIELDS 
690 1 0 |a MARS 
690 1 0 |a OUTER SOLAR SYSTEM 
690 1 0 |a TITAN 
690 1 0 |a UPSTREAM CONDITIONS 
690 1 0 |a SOLAR SYSTEM 
690 1 0 |a COLLISION 
690 1 0 |a COMET 
690 1 0 |a MAGNETIC FIELD 
690 1 0 |a MAGNETOSPHERE 
690 1 0 |a PLANETARY ATMOSPHERE 
690 1 0 |a SATURN 
690 1 0 |a SOLAR WIND 
690 1 0 |a TITAN 
700 1 |a Hamilton, D.C. 
700 1 |a Kurth, W.S. 
700 1 |a Hospodarsky, G. 
700 1 |a Mitchell, D. 
700 1 |a Sergis, N. 
700 1 |a Edberg, N.J.T. 
700 1 |a Dougherty, M.K. 
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