Abstract
We reexamine the properties of the recurrent nova T Pyxidis based on our own spectroscopic data accompanying with the photometric ones by VSOLJ (Variable Star Observers League in Japan) during 2011 outburst. One of the purpose of this paper is whether a missing outburst could be happen around 1988-1989. Comparing the 2011 outburst data with previous ones, we may conclude that any essential difference can not be found. Accordingly it is difficult to deny a small possibility of a ”missing” outburst from 1988 to 1989, taking into account the seasonal gap in its observation for northern hemisphere observers . The problem whether IM Normae belongs to be a member of T Pyx subclass or not is to be postponed by its next outburst taking into account of T Pyx’s peculiar spectral behavior.
Highlights
Recurrent novae (RNe hereafter), whose definite total number is just 10 (see Warner (2008) for example), are divided into three distinct subclass, namely T Pyx subclass, U Sco subclass and T CrB subclass
While detailed photometric observations were performed before 2011 outburst (see Schaefer (2010)), spectroscopic observations performed from early time were rather fragmentary
Recurrent nova IM Normae is a possible member of T Pyx subclass from the point of view of light curve and its orbital period (Schaefer (2010))
Summary
Recurrent novae (RNe hereafter), whose definite total number is just 10 (see Warner (2008) for example), are divided into three distinct subclass, namely T Pyx subclass, U Sco subclass and T CrB subclass. While detailed photometric observations were performed before 2011 outburst (see Schaefer (2010)), spectroscopic observations performed from early time were rather fragmentary. At the end of this section we summarize our results
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