On the new minimum of the symbiotic nova PU Vulpeculae

Kolotilov, E. A.; Munari, U.; Yudin, B. F.

doi:10.1093/mnras/275.1.185

Cited by 30 publications

(36 citation statements)

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“…Historically, V407 Cyg was first identified by its nova-like behavior in 1936 (Hoffmeister 1949;Meinunger 1966) in the m pg range 14 to 16.5, but with identified contributions to the light curve from the Mira variable. Since that time, it has been observed to periodically increase in brightness according to the long-period Mira, and minor, slowly developing outbursts, never becoming brighter than approximately V = 11.5 during the years 1984-1995(Kolotilov et al 1998. A slowdeveloping outburst in the late 1990s was identified from the light curve (Kolotilov et al 2003;Shugarov et al 2007), as it was claimed to become brighter than the outburst of 1936, but never being brighter than V ∼ 11.8.…”

Section: Introductionmentioning

confidence: 97%

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: Introductionmentioning

confidence: 97%

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

Shore

Wahlgren

Augusteijn

et al. 2011

A&A

View full text Add to dashboard Cite

show abstract

“…He II λ 4686 and λ 5412 appeared as a broad emission in around 1990 (Tomov et al, 1991) with a doublepeaked emission (Andrillat & Houziaux, 1995) and ex- hibited as a very broad emission in November 1994, when PU Vul was at the end of the second eclipse (Kolotilov et al, 1995). This indicates that the size of the region forming He II lines might be comparably larger than expected.…”

Section: Spectral Variationsmentioning

confidence: 87%

“…Triple (Andrillat & Houziaux, 1995;Kolotilov et al, 1995). The shell structures might be evolved slowly for such complex line shapes.…”

Section: Discussionmentioning

confidence: 99%

“…The emission of Hβ appeared in September of 1983 and the emission of H followed in December 1987 (Tomov et al, 1991). [O III] lines were enhanced in 1991 and had broad profiles in October 1994 (Kolotilov et al, 1995). .…”

Section: Spectral Variationsmentioning

confidence: 99%

“…In order to examine the photometric and spectroscopic characteristics of this symbiotic nova, PU Vul, a large amount of data was collected, at visible spectroscopic wavelengths (Yamashita et al, 1982(Yamashita et al, , 1983Iijima & Ortolani, 1984;Kenyon, 1986;Iijima, 1989;Kanamitsu et al, 1991;Kanamitsu, 1991;Tomov et al, 1991;Gochermann, 1991;Tamura et al, 1992;Klein et al, 1994;Andrillat & Houziaux, 1994, in the optical photometry (Nakagiri & Yamashita, 1980;Belyakina et al, 1982Belyakina et al, , 1984Belyakina et al, , 1989Kolotilov, 1989;Kolotilov et al, 1995), in UV and X-ray wavelengths (Vogel & Nussbaumer, 1992 ;Nussbaumer & Vogel, 1996;Hoard et al, 1996) and in IR wavelengths (Bensammar et al, 1991).…”

Section: Introductionmentioning

confidence: 99%

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