Abstract

A classical nova is a cataclysmic eruption from the surface of a white dwarf (WD) in a semi-detached binary system. Material accreted from the main sequence secondary star undergoes thermonuclear runaway (TNR) on the WD surface, which results in both the accreted material and the underlying surface layers of the WD being ejected into the surrounding interstellar medium at velocities ranging from 500-5000 km/s. The ejected material is highly enhanced in CNOMgNe and other elements due to both the TNR and mixing with the WD surface. In many novae, copious amounts of dust form in the ejecta, including carbon-grains,silicates, and hydrocarbon molecules. In this talk, I will present our recent work on classical novae, discuss the impact novae can have on Galactic and local scales, and examine new models of shock-induced dust formation. 

In addition, I will briefly discuss upcoming observing opportunities with the SOFIA observatory in conjunction with our UT Austin SOFIA Community Day being held on May 2nd.