Optical spectroscopic and polarization properties of 2011 outburst of the recurrent nova T Pyxidis. (arXiv:1901.00404v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Pavana_M/0/1/0/all/0/1">M. Pavana</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anche_R/0/1/0/all/0/1">Ramya M Anche</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anupama_G/0/1/0/all/0/1">G. C. Anupama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ramaprakash_A/0/1/0/all/0/1">A. N. Ramaprakash</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Selvakumar_G/0/1/0/all/0/1">G. Selvakumar</a>
We study the spectroscopic and ionized structural evolution of T Pyx during
its 2011 outburst, and also study the variation in degree of polarization
during its early phase. Optical spectroscopic data of this system obtained from
day 1.28–2415.62 since discovery, and optical, broadband imaging polarimetric
observations obtained from day 1.36–29.33 during the early phases of the
outburst are used in the study. The physical conditions and the geometry of the
ionized structure of the nova ejecta has been modelled for a few epochs using
the photo-ionization code, CLOUDY in 1D and pyCloudy in 3D. The spectral
evolution of the nova ejecta during its 2011 outburst is similar to that of the
previous outbursts. The variation in the line profiles is seen very clearly in
the early stages due to good coverage during this period. The line profiles
vary from P-Cygni (narrower, deeper and sharper) to emission profiles which are
broader and structured, which later become narrower and sharper in the late
post-outburst phase. The average ejected mass is estimated to be $7.03,
times, 10^{-6}, M_{odot}$. The ionized structure of the ejecta is found to
be a bipolar conical structure with equatorial rings, with a low inclination
angle of $14.75^circ, pm, 0.65^circ$.
We study the spectroscopic and ionized structural evolution of T Pyx during
its 2011 outburst, and also study the variation in degree of polarization
during its early phase. Optical spectroscopic data of this system obtained from
day 1.28–2415.62 since discovery, and optical, broadband imaging polarimetric
observations obtained from day 1.36–29.33 during the early phases of the
outburst are used in the study. The physical conditions and the geometry of the
ionized structure of the nova ejecta has been modelled for a few epochs using
the photo-ionization code, CLOUDY in 1D and pyCloudy in 3D. The spectral
evolution of the nova ejecta during its 2011 outburst is similar to that of the
previous outbursts. The variation in the line profiles is seen very clearly in
the early stages due to good coverage during this period. The line profiles
vary from P-Cygni (narrower, deeper and sharper) to emission profiles which are
broader and structured, which later become narrower and sharper in the late
post-outburst phase. The average ejected mass is estimated to be $7.03,
times, 10^{-6}, M_{odot}$. The ionized structure of the ejecta is found to
be a bipolar conical structure with equatorial rings, with a low inclination
angle of $14.75^circ, pm, 0.65^circ$.
http://arxiv.org/icons/sfx.gif
