One-dimensional multispecies magnetohydrodynamic models of the ramside ionosphere of Titan

Details One-dimensional multispecies magnetohydrodynamic models of the ramside ionosphere of Titan One-dimensional multispecies magnetohydrodynamic models of the ramside ionosphere of Titan

Apr 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994jgr....99.6511k&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 99, no. A4, p. 6511-6525

Physics

40

Magnetohydrodynamics, Planetary Ionospheres, Plasma-Particle Interactions, Satellite Atmospheres, Solar Wind, Titan, Daytime, Electron Density (Concentration), Mathematical Models, Photoionization, Planetary Magnetic Fields

Scientific paper

The interaction of the Saturnian magnetosphere with the ionosphere of Titan has much in common with the solar wind interaction with nonmagnetic bodies in general. A one-dimensional magnetohydrodynamic model was developed, for radial distances of 1.3 to 2 Titan radii (RT), to study the dynamics of H2CN(+), Cn Hm (+) (n, m greater than z), C2H5(+), and CH5(+), in the ramside ionosphere of Titan. For the case of a dayside ramside ionosphere (solar zenith angle of 60 degs) we found that the external magnetospheric plasma interacting with Titan's ionosphere produced a very broad region of ionospheric magnetic field whose peak field strength was approximately 26 nT. The ionosphere was magnetized well below the ionospheric peak, allowing ionizing Saturnian magnetospheric electrons access to this region. The sources of ionization and the electron temperature profiles incorporated into the model depend on the relative locations of Titan, Saturn, and the Sun. The calculated electron and ion density profiles as well as the magnetic field profile also depend on the relative positions of Titan, Saturn, and the Sun.

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