Abstract
We discuss the nebular phase emission during the 2011 outburst of the recurrent nova T Pyxidis and present preliminaryresults on the analysis of the line profiles. We also present some discussions about the binary system configurations and the X-ray emission, showing that the white dwarf mass should be larger than 0.8 M<sub>Θ</sub>.
Highlights
The 2011 outburst of the recurrent nova T Pyx shed more light on some interesting characteristics of this peculiar nova
We present some discussions about the binary system configurations and the X-ray emission, showing that the white dwarf mass should be larger than 0.8 M
The distance of T Pyx was determined from light echoes to be 4.8 ± 0.5 kpc [1], which is marginally consistent within the errors with the value of 3.5 ± 0.4, estimated from the application of the maximum magnitude versus rate of decline (MMRD) relation [2] to the light curve of the 1966 outburst [3]
Summary
The 2011 outburst of the recurrent nova T Pyx shed more light on some interesting characteristics of this peculiar nova. The optical evolution was not very different from the last (1966) outburst, showing the 8 days ’shoulder’ before the final rise to the maximum luminosity, which was reached ∼ 30 days from the initial outburst. In the previous work [6], we have presented the early spectral evolution, up to two months after the initial outburst. We present the optical observations of the nebular phase, which was marked by the onset of the supersoft X-ray source (SSS) emission which happened during the seasonal gap [7]. The optical observations presented here were obtained with the high-resolution spectrograph SARG, mounted on the 3.5m telescope Nazionale Galileo (TNG) located at La Palma. We briefly discuss the X-ray emission and we provide an updated scheme of the binary system configuration in T Pyx, taking into account the recent results
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