Revisiting the classics: on the evolutionary origin of the ‘Fe <scp>ii</scp>’ and ‘He/N’ spectral classes of novae
E. Aydi, Laura Chomiuk, Jay Strader, K. V. Sokolovsky, R. E. Williams, D. A. H. Buckley, A. Ederoclite, L. Izzo, Rebecca Kyer, Justin D. Linford, A. Y. Kniazev, Brian D. Metzger, J. Mikołajewska, P. Molaro, Isabel Molina, K. Mukai, U. Munari, Marina Orio, Teresa Panurach, B. J. Shappee, Ken J. Shen, J. L. Sokoloski, Ryan Urquhart, F. M. Walter
Abstract
ABSTRACT The optical spectra of novae are characterized by emission lines from the hydrogen Balmer series and either Fe ii or He/N, leading to their traditional classification into two spectral classes: ‘Fe ii’ and ‘He/N’. For decades, the origins of these spectral features were discussed in the literature in the contexts of different bodies of gas or changes in the opacity of the ejecta, particularly associated with studies by R. E. Williams and S. N. Shore. Here, we revisit these major studies with dedicated, modern data sets, covering the evolution of several novae from early rise to peak all the way to the nebular phase. Our data confirm previous suggestions in the literature that the ‘Fe ii’ and ‘He/N’ spectral classes are phases in the spectroscopic evolution of novae driven primarily by changes in the opacity, ionization, and density of the ejecta, and most if not all novae go through at least three spectroscopic phases as their eruptions evolve: an early He/N (phase 1; observed during the early rise to visible peak and characterized by P Cygni lines of He i and N ii/iii), then an Fe ii (phase 2; observed near visible peak and characterized by P Cygni lines of Fe ii and O i), and then a later He/N (phase 3; observed during the decline and characterized by emission lines of He i/ii, N ii/iii), before entering the nebular phase. This spectral evolution seems to be ubiquitous across novae, regardless of their speed class; however the duration of each of these phases differs based on the speed class of the nova.