Maya Shemesh
IA / FCUP

Abstract
When the magnetic field carried by the solar wind encounters a planet's magnetic field, it creates an obstruction for the solar wind.
This prevents the inflowing plasma from penetrating the magnetic field and forces it to flow around the planet, following the magnetopause a boundary separating the solar wind from the space dominated by the planet. As a result, a bow shock forms. Unlike Earth, Venus lacks a significant intrinsic global magnetic field, which means there is no primary magnetospheric obstacle around it. Consequently, the solar wind can directly reach Venus's ionosphere, allowing the ionospheric plasma to mingle with the solar wind plasma downstream of the shock. This leads to the escape of some heavy ions from the ionosphere. In this seminar, I will delve into the parameters governing the efficiency of this process and the characteristics of the escaping ion distribution.

2024 May 22, 13:30

IA/U.Porto
Centro de Astrofísica da Universidade do Porto (Classroom)
Rua das Estrelas, 4150-762 Porto