The solar wind and the solar XUV/EUV radiation constitute a permanent forcing of the upper
atmosphere of the planets in our solar system, thereby affecting the habitability and chances …

It is not yet entirely clear whether Mars began as a warm and wet planet that evolved
towards the present-day cold and dry body or if it always was cold and dry with just some …

When the supersonic solar wind reaches the neighborhood of a planetary obstacle it
decelerates. The nature of this interaction can be very different, depending upon whether …

Recent work has demonstrated that high levels of X-ray and UV activity on young M dwarfs
may drive rapid atmospheric escape on temperate, terrestrial planets orbiting within the …

This tutorial deals with the question of atmospheric escape on Mars. After a brief introduction
describing the general context of Mars escape studies, we will present in Section 2 a …

We present results from a new hybrid-Vlasov simulation code, Vlasiator, designed for global
magnetospheric simulations. Vlasiator represents ions by a six-dimensional distribution …

We present initial results from the first community-wide effort to compare global plasma
interaction model results for Mars. Seven modeling groups participated in this activity, using …

Intrinsic magnetic fields have long been thought to shield planets from atmospheric erosion
via stellar winds; however, the influence of the plasma environment on atmospheric escape …

The interaction of the solar wind with the Martian atmosphere and ionosphere is investigated
by using three-dimensional, global and multi-species hybrid simulations. In the present work …

Simulation has become a valuable tool that compliments more traditional methods used to
understand solar system plasmas and their interactions with planets, moons and comets …