The extreme, possible symbiotic Mira V 407 Cyg and its relevance to the OH/IR sources

Munari, U.; Margoni, R.; Stagni, R.

doi:10.1093/mnras/242.4.653

Cited by 66 publications

(132 citation statements)

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“…If we assume the absorption line strength was, in fact, constant throughout the outburst, then the change was due to a "contamination" by a masking continuum; thus the additional continuum accounted for ≈90% of the light at 6700 Å during the earliest observation (MJD 55286) and is consistent with the observed decrease of 3 mag in R during the interval. This is consistent with the simultaneous increase in the atomic and molecular absorption line spectra longward of 6700 Å, with the gradual approach to the pre-outburst spectrum shown in Munari et al (1990). The measurements are shown in Fig.…”

Section: I 6707 å and Non-photospheric Continuum Emissionsupporting

confidence: 85%

“…For both spectra, the luminosity at 2.7 kpc (Munari et al 1990) is approximately 1.2 × 10 34 erg s −1 for days 0-30 and 30-60. The day 60+ spectrum has a corresponding luminosity of about half this value, 6.4 × 10 33 erg s −1 .…”

Section: Swift Observations: Xrt and Uvotmentioning

confidence: 94%

“…The best match is to either M7 III or M8 III. The reported M6 III spectral classification of Munari et al (1990) was obtained at a different phase (0. p 1, around maximum light) of the Mira while the 2010 outburst occurred at 0. p 6 according to the Munari et al ephemeris. Fig.…”

Section: Interstellar Extinction and Spectral Type Of The Miramentioning

confidence: 99%

“…This is why the system is both unique and significant. V407 Cyg, a D-type symbiotic binary with a long period Mira RG (Munari et al 1990), underwent its first ever recorded explosive mass ejection on 2010 Mar. 10, reaching an unfiltered magnitude of 6.8 (Nishiyama & Kabashima 2010) and V magnitude peak of 7.9.…”

Section: Introductionmentioning

confidence: 99%

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The spectroscopic evolution of the symbiotic-like recurrent nova V407 Cygni during its 2010 outburst

Shore

Wahlgren

Augusteijn

et al. 2011

A&A

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Context. V407 Cyg was, before 2010 Mar., known only as a D-type symbiotic binary system in which the Mira variable has a pulsation period of approximately 750 days, one of the longest known. On 2010 Mar. 10, it was discovered in outburst, eventually reaching V < 8. This is the first recorded nova event for this system, but it closely resembles the spectroscopic development of RS Oph, the prototypical symbiotic-like recurrent nova. It was also detected by Fermi above 100 MeV and displayed strong, likely nonthermal centimeter wavelength radio emission. Aims. Unlike classical novae occurring in compact cataclysmic binary systems, for which the ejecta undergo free ballistic expansion, this explosion occurred within the dense, complex wind of a Mira variable companion. This paper concentrates on the development of the shock and its passage through the Mira wind. We also present some constraints on the binary system properties. Methods. Using medium and high resolution ground-based optical spectra, visual and Swift UV photometry, and Swift X-ray spectrophotometry, we describe the behavior of the high-velocity profile evolution for this nova during its first three months. Results. Using the diffuse interstellar bands visible in the high-resolution optical spectra, we obtain an extinction E(B − V) ≈ 0.45 ± 0.05. The spectral type of the red giant during this period, when the star was at R minimum, was no earlier than M7 III. The peak of the X-ray emission occurred at about day 40 with a broad maximum and decline after day 50. The main changes in the optical spectrum began at around that time. The He II 4686 Å line first appeared between days 7 and 14 and initially displayed a broad, symmetric profile that is characteristic of all species before day 60. The profile development thereafter depended on ionization state. Low-excitation lines remained comparatively narrow, with v rad,max of order 200-400 km s −1 . They were systematically more symmetric than lines such as [Ca V], [Fe VII], [Fe X], and He II, all of which showed a sequence of profile changes going from symmetric to a blue wing similar to that of the low ionization species but with a red wing extended to as high as 600 km s −1 . The [O I] 6300, 6364 doublet showed a narrow wind-emission component near the rest velocity of the system and a broad component, 200-300 km s −1 , whose relative intensity increased in time. Forbidden lines of N II and O III had two separate contributors to the profiles, a broad line that increased in strength and velocity width, exceeding 200 km s −1 , and narrow components from a surrounding ionized region at higher velocity than the Mira wind. The Na I D doublet developed a broad component with similar velocity width to the other low-ionization species. The O VI Raman features observed in recent outbursts of RS Oph were not detected. We interpret these variations as aspherical expansion of the ejecta within the Mira wind. The blue side is from the shock penetrating into the wind while the red wing is from the low-density peri...

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Section: I 6707 å and Non-photospheric Continuum Emissionsupporting

confidence: 85%

Section: Swift Observations: Xrt and Uvotmentioning

confidence: 94%

Section: Interstellar Extinction and Spectral Type Of The Miramentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

The spectroscopic evolution of the symbiotic-like recurrent nova V407 Cygni during its 2010 outburst

Shore

Wahlgren

Augusteijn

et al. 2011

A&A

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“…IR-type S - [117], D - [227] and also there is D' estimate in [112]. In [227] there • and an orbit orientation, Ω = 72 ± 6 • , derived from spectropolarimetry [269].…”

Section: =Cd−43 14304mentioning

confidence: 99%

A catalogue of symbiotic stars

Belczyński

Mikołajewska

Munari

et al. 2000

Astron. Astrophys. Suppl. Ser.

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379

407

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Abstract. We present a new catalogue of symbiotic stars. In our list we include 188 symbiotic stars as well as 30 objects suspected of being symbiotic. For each star, we present basic observational material: coordinates, V and K magnitudes, ultraviolet (UV), infrared (IR), X-ray and radio observations. We also list the spectral type of the cool component, the maximum ionization potential observed, references to finding charts, spectra, classifications and recent papers discussing the physical parameters and nature of each object. Moreover, we present the orbital photometric ephemerides and orbital elements of known symbiotic binaries, pulsational periods for symbiotic Miras, Hipparcos parallaxes and information about outbursts and flickering.

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