  Meteor and bolide phenomena caused by the atmospheric ablation of incoming
meteoroids are predicted to occur at the planet Venus. Their systematic
observation would allow to measure and compare the sub-mm to m meteoroid flux
at different locations in the solar system. Using a physical model of
atmospheric ablation, we demonstrate that Venus meteors would be brighter,
shorter-lived, and appear higher in the atmosphere than Earth meteors. To
investigate the feasibility of meteor detection at Venus from an orbiter, we
apply the SWARMS survey simulator tool to sets of plausible meteoroid
population parameters, atmospheric models and instrument designs suited to the
task, such as the Mini-EUSO camera operational on the ISS since 2019. We find
that such instrumentation would detect meteors at Venus with a 1.5x to 2.5x
higher rate than at Earth. The estimated Venus-Earth detection ratio remains
insensitive to variations in the chosen observation orbit and detector
characteristics, implying that a meteor survey from Venus orbit is feasible,
though contingent on the availability of suitable algorithms and methods for
efficient on-board processing and downlinking of the meteor data to Earth. We
further show that a hypothetical camera onboard the upcoming EnVision mission
to Venus similar to the ISS instrument should detect many times more meteors
than needed for an initial characterisation of the large meteoroid population
at 0.7 au from the Sun.
