  This work reviews the long-term evolution of the atmosphere of Venus, and
modulation of its composition by interior-exterior cycling. The formation and
evolution of Venus's atmosphere, leading to contemporary surface conditions,
remain hotly debated topics, and involve questions that tie into many
disciplines. We explore these various inter-related mechanisms which shaped the
evolution of the atmosphere, starting with the volatile sources and sinks.
Going from the deep interior to the top of the atmosphere, we describe volcanic
outgassing, surface atmosphere interactions, and atmosphere escape.
Furthermore, we address more complex aspects of the history of Venus, including
the role of Late Accretion impacts, how magnetic field generation is tied into
long-term evolution, and the implications of geochemical and geodynamical
feedback cycles for atmospheric evolution. We highlight plausible end-member
evolutionary pathways that Venus could have followed, from accretion to its
present-day state, based on modeling and observations. In a first scenario, the
planet was desiccated by atmospheric escape during the magma ocean phase. In a
second scenario, Venus could have harbored surface liquid water for long
periods of time, until its temperate climate was destabilized and it entered a
runaway greenhouse phase. In a third scenario, Venus's inefficient outgassing
could have kept water inside the planet, where hydrogen was trapped in the core
and the mantle was oxidized. We discuss existing evidence and future
observations and missions required to refine our understanding of the planet's
history and of the complex feedback cycles between the interior, surface, and
atmosphere that have been operating in the past, present or future of Venus.
