Spatially Highly Resolved Solar-wind-induced Magnetic Field on Venus

The current work investigates the Venusian solar-wind-induced magnetosphere at a high spatial resolution using all Venus Express (VEX) magnetic observations through an unbiased statistical method. We first evaluate predictability of interplanetary field (IMF) during VEX's magnetospheric transits, and then map induced in cylindrical coordinate system under different IMF conditions. Our high-resolution mapping enables resolving structures on various scales, ranging from thin ionopause associated electric currents to classical global-scale draped IMF. also resolves two recently-reported structures, low ionospheric magnetization over terminator global "looping" structure near magnetotail, both which are not depicted draping configuration. In contrast reported IMF-independent our results illustrate their dependence. component is stronger hemisphere with upward solar wind ($E^{SW}$) than opposite hemisphere. Under downward $E^{SW}$, even breaks, attributable additional wrapping toward $-E^{SW}$. addition, suggest that these spatially overlapping each other. occurs very narrow region, about 87--95$^\circ$ zenith angle 190--210~km altitude, implying future simulation reproduce entails least 10 km. discuss this terms Cowling channel.