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We study the solar wind induced oxygen ion escape from Venus' upper\udatmosphere and the Venus Express observations of the Venus-solar wind\udinteraction by the HYB-Venus hybrid simulation code. We compare the\udsimulation to the magnetic field and ion observations during an orbit of\udnominal upstream conditions. Further, we study the response of the induced\udmagnetosphere to the emission of planetary ions. The hybrid simulation is\udfound to be able to reproduce the main observed regions of the Venusian\udplasma environment: the bow shock (both perpendicular and parallel regions),\udthe magnetic barrier, the central tail current sheet, the magnetic tail\udlobes, the magnetosheath and the planetary wake. The simulation is found to\udbest fit the observations when the planetary \oxy~escape rate is in the range\udfrom 3×1024 s−1 to 1.5×1025 s−1. This range\udwas also found to be a limit for a test particle-like behaviour of the\udplanetary ions: the higher escape rates manifest themselves in a different\udglobal configuration of the Venusian induced magnetosphere

Oxygen ion escape from Venus in a global hybrid simulation: role of the ionospheric O&lt;sup&gt;+&lt;/sup&gt; ions

Oxygen ion escape from Venus in a global hybrid simulation: role of the ionospheric O<sup>+</sup> ions