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Abstract
Abstract. In the context of planetary space weather, we estimate the ion production rates in the Venusian atmosphere due to the interactions of solar energetic particles (SEPs) with gas. The assumed concept for our estimations is based on two cases of SEP events, previously observed in near-Earth space: the event in October 1989 and the event in May 2012. For both cases, we assume that the directional properties of the flux and the interplanetary magnetic field configuration would have allowed the SEPs' arrival at Venus and their penetration to the planet's atmosphere. For the event in May 2012, we consider the solar particle properties (integrated flux and rigidity spectrum) obtained by the Neutron Monitor Based Anisotropic GLE Pure Power Law (NMBANGLE PPOLA) model (Plainaki et al., 2010, 2014) applied previously for the Earth case and scaled to the distance of Venus from the Sun. For the simulation of the actual cascade in the Venusian atmosphere initiated by the incoming particle fluxes, we apply the DYASTIMA code, a Monte Carlo (MC) application based on the Geant4 software (Paschalis et al., 2014). Our predictions are afterwards compared to other estimations derived from previous studies and discussed. Finally, we discuss the differences between the nominal ionization profile due to galactic cosmic-ray–atmosphere interactions and the profile during periods of intense solar activity, and we show the importance of understanding space weather conditions on Venus in the context of future mission preparation and data interpretation.
Highlights
The atmosphere of Venus is exposed to photon and particle (solar wind, galactic cosmic ray and solar energetic particle (SEP)) radiations, covering a vast range of energies
As a first step in this process, we focus our attention on the ion pair production rates and the accurate estimation of the characteristics of the atmospheric cascades initiated by solar energetic particles (SEPs) bombarding the Venusian atmosphere
We investigate the response of the Venusian atmosphere to two different cases of SEP events, assuming that the directional properties of those solar particles allow their arrival and penetration to the gas
Summary
The atmosphere of Venus is exposed to photon and particle (solar wind, galactic cosmic ray and solar energetic particle (SEP)) radiations, covering a vast range of energies. The occasional penetration of solar cosmic rays in the atmosphere of Venus is a significant agent for planetary space weather (Lilensten et al, 2014; Plainaki et al, 2016) In this context, in the current paper, we investigate the Venusian atmosphere interactions with SEPs which, having suprathermal energies, follow trajectories that are influenced only slightly by the planet’s induced magnetic field. To study the effects in the Venusian atmosphere of an SEP event of the order of magnitude (in both energy and flux) of the event on 17 May 2012 we consider the solar particle properties (integrated flux and spectrum) obtained by the Neutron Monitor Based Anisotropic GLE Pure Power Law (NMBANGLE PPOLA) model (Plainaki et al, 2010, 2014) applied previously for the Earth case and scaled to the distance of Venus.
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