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<jats:title>ABSTRACT</jats:title> <jats:p>Alice is a far-ultraviolet imaging spectrograph on board <jats:italic>Rosetta</jats:italic> that, among multiple objectives, is designed to observe emissions from various atomic and molecular species from within the coma of comet 67P/Churyumov–Gerasimenko. The initial observations, made following orbit insertion in 2014 August, showed emissions of atomic hydrogen and oxygen spatially localized close to the nucleus and attributed to photoelectron impact dissociation of H<jats:sub>2</jats:sub>O vapor. Weaker emissions from atomic carbon were subsequently detected and also attributed to electron impact dissociation, of CO<jats:sub>2</jats:sub>, the relative H <jats:sc>i</jats:sc> and C <jats:sc>i</jats:sc> line intensities reflecting the variation of CO<jats:sub>2</jats:sub> to H<jats:sub>2</jats:sub>O column abundance along the line of sight through the coma. Beginning in 2015 mid-April, Alice sporadically observed a number of outbursts above the sunward limb characterized by sudden increases in the atomic emissions, particularly the semi-forbidden O <jats:sc>i</jats:sc> <jats:italic>λ</jats:italic>1356 multiplet, over a period of 10–30 minutes, without a corresponding enhancement in long-wavelength solar reflected light characteristic of dust production. A large increase in the brightness ratio O <jats:sc>i</jats:sc> <jats:italic>λ</jats:italic>1356/O <jats:sc>i</jats:sc> <jats:italic>λ</jats:italic>1304 suggests O<jats:sub>2</jats:sub> as the principal source of the additional gas. These outbursts do not correlate with any of the visible images of outbursts taken with either OSIRIS or the navigation camera. Beginning in 2015 June the nature of the Alice spectrum changed considerably with CO Fourth Positive band emission observed continuously, varying with pointing but otherwise fairly constant in time. However, CO does not appear to be a major driver of any of the observed outbursts.</jats:p>