S. N. Shore, G. M. Wahlgren, T. Augusteijn, T. Liimets, P. Koubsky, M. Slechta, V. Votruba
The nova outburst of V407 Cyg in 2010 Mar. 10 was the first observed for this
star but its close resemblance to the well known symbiotic-like recurrent nova
RS Oph suggests that it is also a member of this rare type of Galactic novae.
The nova was the first detected at $\gamma$-ray energies and is the first known
nova explosion for this system. The extensive multiwavelength coverage of this
outburst makes it an ideal comparison with the few other outbursts known for
similar systems. We extend our previous analysis of the Mira and the expanding
shock from the explosion to detail the time development of the photoionized
Mira wind, circumstellar medium, and shocked circumstellar environment to
derive their physical parameters and how they relate to large scale structure
of the environment, extending the previous coverage to more than 500 days after
outburst. Absorption lines of Fe-peak ions formed in the Mira wind were visible
as P Cyg profiles at low velocity before Day 69, around the time of the X-ray
peak and we identified many absorption transitions without accompanying
emission for metal lines. The H Balmer lines showed strong P Cyg absorption
troughs that weakened during the 2010 observing period, through Day 128. We
distinguish the components from the shock, the photoionized environment, and
the chromosphere and inner Mira wind using spectra taken more than one year
after outburst. The multiple shells and radiative excitation phenomenology are
similar to those recently cited for GRBs and SNIa (severely truncated)
View original:
http://arxiv.org/abs/1112.2247
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