The Detailed Photometric and Spectroscopic Study of the 2011 Outburst of   the Recurrent Nova T Pyxidis from 0.8 to 250 Days after Discovery
  We investigated the optical lightcurve of T Pyx during its 2011 outburst by compiling a database of SMEI and AAVSO observations. The SMEI lightcurve, providing unprecedented detail covering 1.5-49d post-discovery, was divided into four phases based on the idealised CN optical lightcurve; the initial rise (1.5-3.3d), the pre-maximum halt (3.3-13.3d), the final rise (14.7-27.9d), and the early decline (27.9d-). The SMEI lightcurve contains a strongly detected period of 1.44+/-0.05d during the pre-maximum phase. These oscillations resemble those found in TNR models arising from instabilities in the expanding envelope. No spectral variation mirroring the lightcurve periodicity was found. A marked dip at 22-24d just before maximum light (27.9d) may represent the same phenomenon seen in novae observed by SMEI. Spectra from the Liverpool Telescope and SMARTS 1.5m were obtained from 0.8-80.7 and 155.1-249.9d, covering the major phases of development. A distinct high velocity ejection phase was evident during the early rise (V~4000 km/s). A marked drop at 5.7d, and then a gradual increase occurred in the ejection velocity which stabilised at ~1500 km/s at the pre-maximum halt. Here we propose two stages of mass loss, a short-lived phase occurring immediately after outburst, lasting ~6d, followed by a steadily evolving and higher mass loss phase. The overall spectral development follows that typical of a CN and comparison with the photometric behaviour reveals consistencies with the evolving pseudo-photosphere model of a CN outburst. Comparing optical spectra to X-ray and radio lightcurves, weak [Fe X] 6375 Angstrom emission was marginally detected before the X-ray rise and was clearly present during the brightest phase of X-ray emission. If the onset of the X-ray phase and the start of the optical final decline are related to the cessation of significant mass loss, then this occurred at 90-110d. 
F. Surina (1), R. A. Hounsell (2), M. F. Bode (1), M. J. Darnley (1),   D. J. Harman (1), F. M. Walter (3) ((1) Astrophysics...
astro-ph.SR