A multiwavelength study of Nova QU Vulpeculae 1984

Saizar, P; Starrfield, S.; Ferland, Gary J.; Wagner, R. M.; Truran, J. W.; Kenyon, Scott J.; Sparks, W. M.; Williams, Robert E.; Stryker, L. L.

doi:10.1086/171890

Cited by 59 publications

(52 citation statements)

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“…The weakness of [O III] lines in the nebular stage may have been due mainly to the high density in the ejecta. The abundance of neon is comparable to that of QU Vul and higher than those of the other novae, while QU Vul is classified as a neon nova; that is, its explosion is expected to have occurred on an O-Ne-Mg white dwarf (Saizar et al 1992;Schwarz 2002). The low abundance of argon of QU Vul, however, is not found in this nova.…”

Section: Abundances Of Heavy Elementsmentioning

confidence: 70%

“…At least, as we know, no slow nova showed the coronal line [Fe X] λ6375. Some infrared coronal lines, e.g., [Al IX] λ2.04 µm and [Si IX] λ3.92 µm, were detected on the spectra of a slow nova QU Vul (Greenhouse et al 1988), but the optical coronal line [Fe X] λ6375 was probably not detected or at most was very weak (Saizar et al 1992). It is noteworthy that we have only three well-observed extremely slow novae at the present time, but two of them, HR Del (e.g., Rafanelli & Rosino 1978) and V723 Cas (this paper), show the emission line of [Fe X] λ6375.…”

Section: Coronal Line [Fe X] λ6375mentioning

confidence: 99%

“…We assume that the electron temperature was stable until February 1999, because it is known that the electron temperatures of the ejecta of normal novae were nearly stable in the early nebular stage, as seen e.g. in V1500 Cyg (Ferland 1978;Lance et al 1988), QU Vul (Saizar et al 1992), and V1494 Aql (Paper II). The electron densities of the [O III] and [N II] regions were derived using the formulae of Seaton (1975) for the intensity ratios of the nebular to the auroral lines.…”

Section: Electron Temperature and Densitymentioning

confidence: 99%

“…The The derived abundances are given in Table 11 on a logarithmic scale relative to hydrogen N(H) = 12. The abundances of a fast nova V1425 Aql (Lyke et al 2001), a slow nova QU Vul (Saizar et al 1992;Schwarz 2002), and the extremely slow novae HR Del (Tylenda 1978) and RR Pic (Williams & Gallagher 1979) are also given in the table.…”

Section: Abundances Of Heavy Elementsmentioning

confidence: 99%

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Spectral evolution of the slowest classical nova V723 Cassiopeiae in the decline stage

Iijima

2006

A&A

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The spectral evolution of an extremely slow nova V723 Cas was monitored at Asiago Observatory for seven years. Observations in the long pre-maximum stage, which lasted more than four months, were reported in our previous paper. Here, we report the spectral evolution in the decline stage from January 1996 to December 2001. The spectra just after maximum luminosity showed prominent emission lines of H I, He I, Fe II, Ti II, Si II, Na I, etc. P Cygni type absorption components appeared on H I, He I, and Fe II lines about two months after maximum when the nova performed the second brightening. The radial velocities of the absorption components of H I and He I lines varied from −600 km s 01. The abundance of oxygen is not so different from those of usual classical novae, while a rather low abundance of nitrogen is noticed. The abundance of neon is roughly comparable to that of a neon nova QU Vul.

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Section: Abundances Of Heavy Elementsmentioning

confidence: 70%

Section: Coronal Line [Fe X] λ6375mentioning

confidence: 99%

Section: Electron Temperature and Densitymentioning

confidence: 99%

Section: Abundances Of Heavy Elementsmentioning

confidence: 99%

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Spectral evolution of the slowest classical nova V723 Cassiopeiae in the decline stage

Iijima

2006

A&A

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“…QU Vul is a neon nova and, according to Ritter et al (1991), it is believed that ONeMg white dwarfs tend to be massive stars. However estimates of the ejected mass of QU Vul by Saizar et al (1992) and others are consistent with a white dwarf mass of 1 M or less, and so an assumed value for the mass of the primary of 0.82 M was taken from Webbink (1990), who derived masses of the white dwarf primaries in CVs from a variety of methods. A gravity-darkening coefficient of 0.8 was chosen as this is the theoretical value for a convective envelope for the secondary star, and limb-darkening values were taken from Al-Naimiy (1978).…”

Section: Qu Vul Irradiationmentioning

confidence: 99%

The decline in irradiation from the white dwarf in old novae

Thomas

Naylor

Norton

2008

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Aims. We have investigated how a flux ratio analysis of the light curves of cataclysmic variables can be used to calculate the luminosity irradiating the secondary star in the classical novae QU Vul, V Per, DD Cir, DN Gem, V1432 Aql, and WY Sge. Methods. We undertook phase-resolved, near-infrared K band photometry of QU Vul and V Per. Using data from QU Vul we show how flux ratios taken between fiducial orbital phases in the light curves of irradiated CVs can be used to measure the degree of heating of the secondary star. We compared the heating effect obtained from flux ratio analysis with more formal modelling, or by measurements taken from the literature, and found good agreement. We used the results to determine how irradiation changes with time since the nova outburst.Results. The light curve of QU Vul shows the presence of two maxima in the K band, which are displaced from phase 0.25 towards the 0.5 phase position, as would be expected from heating of the inner face of the secondary star by radiation from hot primary. Nova V Per, on the other hand shows evidence for a hot spot on the accretion disc, and it would appear that heating of the inner face is not occurring. The results of the flux ratio analysis of the objects examined are plotted as a function of time since the nova explosions occurred. There is marginal evidence for a decline in flux with time since the outburst, superimposed on considerable scatter, which is likely to be caused by the different temperature reached in each nova explosion. The decline is consistent with the declines others have seen. We conclude that it is the decline in reprocessed irradiation from the cooling white dwarf alone, rather than a decline in mass transfer rate, that could be the cause of the decrease in optical brightness seen in old novae.

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