الفهرس 
Ionic escaping from Titan and VenusOnly 14 pages are availabe for public view
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Abstract
In chapter two, we studied the effect of the solar wind streams on the upper atmosphere of Titan moon. We considered three positive ion-fluids in the presence of the solar wind of electrons and protons. Then, we solved the system of equations using numerical method with the aid of Walfram computational code. Using a self-similar transformation, a numerical analysis is performed to characterize the plasma density, velocity, and electric potential during the expansion.
In chapter three, we studied the effect of the solar wind streams on the upper atmosphere of Venus using the self-similar technique to simulate the plasma expansion process within Venus’ ionosphere. We considered two positive ion fluids in the presence of the solar wind of electrons and protons, and solving this system with the aid of a computational code. The hydrodynamic approach proposed for plasma expansion in the present study comprises two populations of positive ions and the neutralizing electrons, which interact with the solar wind electrons and protons. The fluid equations describ- ing the plasma are solved numerically using a self-similar approach. The behavior of plasma density, velocity, and electric potential, as well as their reliance upon solar wind parameters have been examined.