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We discuss the central role that dust condensation plays in shaping theobservational appearance of outflows from coalescing binary systems. Asbinaries begin to coalesce, they shock-heat and expel material into theirsurroundings. Depending on the properties of the merging system, this materialcan expand to the point where molecules and dust form, dramatically increasingthe gas opacity. We use the existing population of Luminous Red Novae (LRNe) toconstrain the thermodynamics of these ejecta, then apply our findings to theprogressive obscuration of merging systems in the lead in to their coalescence.Compact progenitor stars near the main sequence or in the Hertzsprung gap alongwith massive progenitor stars have sufficiently hot circumstellar material toremain unobscured by dust. By contrast, more extended, low-mass giants shouldbecome completely optically obscured by dust formation in the circumbinaryenvironment. We predict that 30--50\% of stellar coalescence transients forsolar-mass stars will be dusty, infrared-luminous sources. Of these, theoptical transients may selectively trace complete merger outcomes while theinfrared transients trace common envelope ejection outcomes.

Dusty, Self-obscured Transients from Stellar Coalescence