New Insights into the Evolution of Galactic Classical Novae

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Scientific paper

Classical novae (CNe) are violent thermonuclear explosions arising on the surface of white dwarfs in binary systems and are contributors to the chemical evolution of the interstellar medium through the production and ejection of copious amounts of metal-rich material. Observations and modeling of CNe eruptions illuminate numerous fundamental processes of astrophysical interest, including non-equilibrium thermonuclear runaway, radiative processes in dynamic nebular environments, binary star interaction, as well as dust condensation and grain growth. Here I summarize key findings of over 30 Galactic CNe obtained as part of a 5 year, panchromatic optical/infrared observing campaign using Spitzer, Gemini, and other ground based optical facilities. In particular, synoptic observations of V1065 Cen, V574 Pup, V2467 Cyg, and V458 Vul, which exhibit spectra rich in metals (e.g O, Ne, Mg, S, Ar, Ca, and Fe) produced during the thermonuclear runaway and through dredge up from the surface layers of the underlying WD, yield new estimates of WD progenitor masses and composition, ejecta masses, and absolute abundances. Dusty novae such as V1065 Cen, V2362 Cyg, and V2361 Cyg, produce a variety of grain types as revealed by emission features characteristic of silicates, hydrogenated amorphous carbon dust, and PAH-like molecules, often in the same system. Our data set is exceptional in that observations of many targets commence immediately after eruption and follow the development for hundreds of days post-outburst providing unique insight into the evolution of conditions within the ejecta including the complete cycle of growth, processing, and dissipation of dust grains. Support for this dissertation research was provided in part by the National Science Foundation and various JPL/Caltech contracts to the University of Minnesota.

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