SCHNEITER ERNESTO MATIAS
Congresos y reuniones científicas
Título:
An MHD + test particle study of the solar wind-Mars interaction
Autor/es:
SCHNEITER, E. M.; VELAZQUEZ, P. F.; BLANCO-CANO, X.; ESQUIVEL, A
Lugar:
UBA
Reunión:
Workshop; TENTH J.J. GIAMBIAGI WINTER SCHOOL Principles and Applications of Fluid Dynamics; 2008
Institución organizadora:
Departamento de física de la escuela de ciencias de la Universidad de Buenos Aires
Resumen:
The solar wind interaction with Mars is very different to that of Earth because Mars lacks a
global magnetic field. Despite this fact, an induced magnetic boundary is formed due to the
interaction of the solar wind with the ionosphere, an a bow shock forms ahead of the planet,
much closer than in the case of our planet. Solar radiation ionizes Mars upper atmosphere and
later, due to the dynamical interaction between the solar wind and the newly ionized material,
some ions are swept away from the planet, i.e. picked up into the solar flow. These ions
form ring-beam distributions in velocity space making the plasma unstable to the generation
of ion cyclotron waves that have been previously reported. In this work use an MHD code to
simulate the solar wind interaction with Mars under various IMF geometries. We also inject
test particles, follow their trajectories, and build velocity distributions to sudy possible wave
growth due to these distributions.
global magnetic field. Despite this fact, an induced magnetic boundary is formed due to the
interaction of the solar wind with the ionosphere, an a bow shock forms ahead of the planet,
much closer than in the case of our planet. Solar radiation ionizes Mars upper atmosphere and
later, due to the dynamical interaction between the solar wind and the newly ionized material,
some ions are swept away from the planet, i.e. picked up into the solar flow. These ions
form ring-beam distributions in velocity space making the plasma unstable to the generation
of ion cyclotron waves that have been previously reported. In this work use an MHD code to
simulate the solar wind interaction with Mars under various IMF geometries. We also inject
test particles, follow their trajectories, and build velocity distributions to sudy possible wave
growth due to these distributions.
