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Appendix A: V705 Cyg 1993 and discrete absorption systems on Na I D

The D lines have been found to display P Cyg profiles occasionally in the literature, notably during the first phase of the DQ Her 1934 outburst (see McLaughlin 1954, 1964). However, based on photographic, uncalibrated, and relatively low resolution spectra, this might be explained as variations in the complex of emission and absorption lines normally seen in the initial stage of the expansion. The first classical CO nova to show this phenomenon unambiguously after the advent of CCD detectors, V705 Cas 1993, is shown in Fig. A.1. This sequence shows the optically thick phase, during the first two weeks of the outburst. The line pairs shifted systematically to higher velocity with an increasing optical depth, indicated by the increase in the F(5895)/F(5889) ratio, with FWHM ≈ 300 km s^-1. The sequence ended quite early in the outburst, the nova forming dust about two months later (Shore et al. 1994), as did DQ Her and several other novae in which the Na I D multiple components and moving DACs were historically observed. The NOT sequence for T Pyx covered a longer interval. Similar behavior has recently been detailed by Sadakane et al. (2010) for V1280 Sco.

	Fig. A.1 V705 Cas (Ritter Observatory spectra of the optically thick stage of the CO nova Nova Cas 1993, Na I D line variations. Top: 1993 Dec. 27. Middle: 1993 Dec. 29, 1994. Bottom: 1994 Jan. 5 (see text for details)
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	Fig. B.1 Hγ profile variations, as in Fig. 2.
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© ESO, 2011