Abstract
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)
Highlights
The 2010 outburst of V407 Cyg, a previously classified Dtype symbiotic star (Munari 1990) whose historical variabilityBased on observations made with the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias.had been classified as “nova-like” by Hoffmeister (1949) and Meinunger (1966), developed photometrically and spectroscopically almost identically to the most recent eruptions of the symbiotic-like recurrent nova (SyRN) RS Oph (1985, 2006)
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
We use optical spectra obtained at high resolution with the Nordic Optical Telescope (NOT) (R ≈ 45 000 to 65 000) and medium resolution Ondrejov Observatory (R ≈ 12 000) data and compare the line variations with publicly available archival measurements at 30 GHz OVNR and at X-rays with Swift during the first four months of the outburst, through the end of the epoch of strong XR emission
Summary
The 2010 outburst of V407 Cyg, a previously classified Dtype symbiotic star (Munari 1990) whose historical variability. Had been classified as “nova-like” by Hoffmeister (1949) and Meinunger (1966), developed photometrically and spectroscopically almost identically to the most recent eruptions of the symbiotic-like recurrent nova (SyRN) RS Oph (1985, 2006) This event moved the system into that rare group of explosive cataclysmic variables. Ondrejov Observatory, Swift, and Fermi/LAT concentrating on the Mira properties and the time development of the shock propagating through the red giant (RG) wind. In this second paper, we focus on the evolution of the circumstellar environment that was photoionized and illuminated by the emission from the white dwarf (WD) and the shock. We extend the previous results to include additional proxies for the high energy excitation mechanisms
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