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Electron density profiles of the Venus' ionosphere are inverted from theVenus Express (VEX) one-way open-loop radio occultation experiments carried outby Shanghai 25 m antenna from November 2011 to January 2012 at solar maximumconditions and by New Norcia 35 m antenna from August 2006 to June 2008 atsolar intermediate conditions. The electron density profile (from 110 km to 400km) retrieved from the X-band egress observation at Shanghai station, shows asingle peak near 147 km with a peak density of about $2 \times 10^4\rm{cm}^{-3}$ at a solar zenith angle of 94$^{\circ}$. As a comparison, the VEXradio science (VeRa) observations at New Norcia station were also examined,including S-, X-band and dual-frequency data in the ingress mode. The resultsshow that the electron density profiles retrieved from the S-band data are moreanalogous to the dual-frequency data in the profile shape, compared with theX-band data. Generally, the S-band results slightly underestimate the magnitudeof the peak density, while the X-band results overestimate that. Thediscrepancy in the X-band profile is probably due to the relatively largerunmodeled orbital errors. It is also expected that the ionopause height issensitive to the solar wind dynamical pressure in high and intermediate solaractivities, usually in the range of 200 km - 1000 km on the dayside and muchhigher on the nightside. Structural variations ("bulges" and fluctuations) canbe found in the electron density profiles in intermediate solar activity, whichmay be caused by the interaction of the solar wind with the ionosphere.Considerable ionizations can be observed in the Venus' nightside ionosphere,which are unexpected for the Martian nightside ionosphere in most cases.

Ionospheric inversion of the Venus Express radio occultation data observed by Shanghai 25 m and New Norcia 35 m antennas