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In the context of planetary space weather, we estimate the ion production\udrates in the Venusian atmosphere due to the interactions of solar energetic\udparticles (SEPs) with gas. The assumed concept for our estimations is\udbased on two cases of SEP events, previously observed in near-Earth\udspace: the event in October 1989 and the event in May 2012. For both cases,\udwe assume that the directional properties of the flux and the interplanetary\udmagnetic field configuration would have allowed the SEPs' arrival at Venus and\udtheir penetration to the planet's atmosphere. For the event in May 2012, we\udconsider the solar particle properties (integrated flux and rigidity\udspectrum) obtained by the Neutron Monitor Based Anisotropic GLE Pure Power Law (NMBANGLE PPOLA) model (Plainaki et al., 2010, 2014)\udapplied previously for the Earth case and scaled to the distance of Venus from\udthe Sun. For the simulation of the actual cascade in the Venusian atmosphere\udinitiated by the incoming particle fluxes, we apply the DYASTIMA code, a\udMonte Carlo (MC) application based on the Geant4 software (Paschalis et al.,\ud2014). Our predictions are afterwards compared to other estimations derived\udfrom previous studies and discussed. Finally, we discuss the differences\udbetween the nominal ionization profile due to galactic cosmic-ray–atmosphere\udinteractions and the profile during periods of intense solar activity, and we\udshow the importance of understanding space weather conditions on Venus in\udthe context of future mission preparation and data\udinterpretation

Solar energetic particle interactions with the Venusian atmosphere