Abstract
Aims. We aim to study the viscous interaction of the solar wind with the ionosphere of Venus in the magnetic polar regions by means of hydrodynamical computer simulations. Methods. We use a finite difference code developed for the solution of the Navier-Stokes, continuity and energy equations. Results. We have calculated the flow properties, the shape and location of the boundary layer and the shock formed as a consequence of the viscous interaction over the magnetic poles of the planet and advected downstream. By comparing our results to the flow properties measured by the Venera 10 and Mariner 5 spacecraft in the Venus ionosheath, we determine that a Reynolds number for the flow near the value Re = 20 is necessary to reproduce the position of the intermediate transition as well as the shock front. Also, on the basis of our results we predict the existence of a stagnation region for the solar wind flow extending considerably upstream from the viscous interaction region.
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
