2012A&A...540A..55S


C.D.S. - SIMBAD4 rel 1.7 - 2020.04.06CEST00:06:16

2012A&A...540A..55S - Astronomy and Astrophysics, volume 540A, 55-55 (2012/4-1)

The spectroscopic evolution of the symbiotic-like recurrent nova V407 Cygni during its 2010 outburst. II. The circumstellar environment and the aftermath.

SHORE S.N., WAHLGREN G.M., AUGUSTEIJN T., LIIMETS T., KOUBSKY P., SLECHTA M. and VOTRUBA V.

Abstract (from CDS):

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 γ-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. We use optical spectra obtained at high resolution with the Nordic Optical Telescope (NOT) the higher the excitation energy, the more closely the profiles resemble the HeII/Ca V-type high velocity shock profile discussed in Paper I (Shore et al., 2011A&A...527A..98S). This also accounts for the comparative development of the [NII] and [OIII] isoelectronic transitions: the [OIII] 4363Å profile does not show the low velocity peaks while the excited [NII] 5754Å does. If nitrogen is mainly N+3 or higher in the shock, the upper state of the [NII] nebular lines will contribute but if the oxygen is O+2 then this line is formed by recombination, masking the nebular contributor, and the lower states are collisionally quenched but emit from the low density surroundings. 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. The Fe-peak line profiles and flux variations were different for permitted and forbidden transitions: the E1 transitions were not visible after Day 128 but had shown a narrow peak superimposed on an extended (200km/s) blue wing, while the M1 and E2 transitions persisted to Day 529, the last observation, and showed extended redshifted wings up of the same velocity. 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.

Abstract Copyright:

Journal keyword(s): binaries: symbiotic - gamma-ray burst: general - novae, cataclysmic variables - stars: individual: V407 Cygni

Status at CDS:  

Simbad objects: 7

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Number of rows : 7

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 GRB 060418 gB 15 45 42.600 -03 38 20.00 15.73 16.19 14.98     ~ 320 1
2 V* T CrB Sy* 15 59 30.1619486506 +25 55 12.607985109 2.69 2.10 2.00     M3III+p 643 0
3 V* RS Oph No* 17 50 13.1592776879 -06 42 28.481553668   12.29 4.30     OB+M2ep 918 0
4 V* V745 Sco LP* 17 55 22.2273446574 -33 14 58.558723074     17.987   13.353 ~ 188 0
5 V* V3890 Sgr LP* 18 30 43.2881019064 -24 01 08.948570280   13.5 15.944   12.611 ~ 146 0
6 EM* AS 453 Sy* 21 02 09.8173494732 +45 46 32.736335364   16.04 14.68 11.38   Mep 233 0
7 BD+28 4211 HS* 21 51 11.0220905905 +28 51 50.366090892 8.922 10.25 10.58 10.656 10.831 sdO2VIIIHe5 730 0

    Equat.    Gal    SGal    Ecl

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2020.04.06-00:06:16

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