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A high-resolution spectroscopic survey of postoutburst novae revealsshort-lived heavy element absorption systems in a majority of novae nearmaximum light, having expansion velocities of 400-1000 km/s and velocitydispersions between 35-350 km/s. A majority of systems are acceleratedoutwardly, and they all progressively weaken and disappear over timescales ofweeks. A few of the systems having narrow, deeper absorption reveal a richspectrum of singly ionized Sc, Ti, V, Cr, Fe, Sr, Y, Zr, and Ba lines. Analysisof the richest such system, in Nova LMC 2005, shows the excitation temperatureto be 104 K and elements lighter than Fe to have abundance enhancements oversolar values by up to an order of magnitude. The gas causing the absorptionsystems must be circumbinary and its origin is most likely mass ejection fromthe secondary star. The absorbing gas pre-exists the outburst and may representepisodic mass transfer events from the secondary star that initiate the novaoutburst(s). If SNe Ia originate in single degenerate binaries, such absorptionsystems could be detectable before maximum light

Transient Heavy Element Absorption Systems in Novae: Episodic Mass Ejection from the Secondary Star