The nebular stage is that interval in the expansion of classical nova ejecta when the transparency of the matter permits a comprehensive view of the structure of the ejecta. We aim to study the radiative response of nova ejecta to illumination variations in the post-outburst white dwarf (WD). We used medium-resolution (R≈ 10⁴) optical spectra, a substantial fraction of which were flux-calibrated. Time series were obtained for profile and flux variations supplemented by Swift X-ray Telescope (XRT) spectrophotometry. The ejecta structure and density stratification were modeled assuming nebular conditions with biconical geometries, and densities were derived using the O III lines and scaled for ejecta expansion. Antiphase variations were observed for the C IV 5808Å recombination line and coronal transitions of Fe VII and Ca V coincident with X-ray flaring activity of the central WD. In the earlier transition stage to nebular conditions, similar profile and flux variations were observed for N II 5755Å, although no X-rays were detected during that time. We show that the profile variations map the density structure of the ejecta and are entirely due to changes in the hardness of the incident spectral distribution of the white dwarf. No dynamical explanation is required. Nebular stage line intensity and profile variations permit a comprehensive view of the development of the central white dwarf without recourse to other wavelength intervals, such as X-rays or the far-UV.
Giacomo et al. (Fri,) studied this question.
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