Ultraviolet Studies of Interacting Binaries

Gänsicke, B. T.; Martino, D. de; Marsh, T. R.; Haswell, C. A.; Knigge, Christian; Long, Knox S.; Shore, Steven N.

doi:10.1007/s10509-006-9264-z

Cited by 12 publications

(3 citation statements)

References 77 publications

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“…In this respect it is worth pointing out that, in contrast to the large number of UV (mostly IUE) and far-UV (mostly FUSE) studies for other classes of CVs (see, for example, Verbunt & Wade 1984;La Dous 1991;Mauche et al 1997;Araujo-Betancor et al 2005;Long 2006; Gänsicke et al 2006;Hamilton et al 2007;Sion et al 2008;Froning et al 2012), in the case of old novae, A&A 560, A49 (2013) the studies have been fairly preliminary (Gilmozzi et al 1994;Selvelli 2004) or limited to a subset of objects (Szkody et al 1991;Puebla et al 2007Puebla et al , 2011.…”

Section: Introductionmentioning

confidence: 99%

An archive study of 18 old novae

Selvelli

Gilmozzi

2013

A&A

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Aims. We present an overview of the UV spectral properties of old novae as a class. The data and results of this paper, together with data from the outburst phases, will be utilized in a follow-up study to determine statistical properties and to investigate correlations among the physical parameters of the quiescent and eruptive phases. Methods. All the available IUE, HST, and FUSE archive data for 18 old novae were used to derive accurate and homogeneous estimates of the reddening from the 2175 Å extinction bump and to determine the intrinsic spectral energy distribution corresponding to the utilization of both existing extinction curves. We also measured all the emission and absorption lines. Results. We have found good agreement between spectra taken at different epochs and by different instruments, a clear indication of the near constancy of the SED on timescales of several years. With the possible exception of GK Per, the dereddened UV continua are represented well by a single-curve power-law distribution F λ ∝ λ −α , with α in the range 0.32-2.55 for one curve and 0.35-2.88 for the other one. The extrapolation of the various UV power laws to the optical range yields values that are in good agreement with the V magnitudes. We interpret this result as evidence that the SED is dominated by the accretion disk in the UV and optical spectral regions. A detailed study of the emission spectrum has led to measuring and identifying more than one hundred features and to detecting several lines that are rather uncommon in other CVs and whose identification is uncertain.

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Section: Introductionmentioning

confidence: 99%

An archive study of 18 old novae

Selvelli

Gilmozzi

2013

A&A

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“…This is especially true in view of the large number of recent discoveries from the GALEX satellite, which require detailed UV follow-up (Bianchi et al 2006). We here report some of the results achieved by UV observations of CVs (for a comprehensive review also see Gänsicke et al 2006a) and highlight the importance of future observations.…”

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confidence: 86%

UV observations of Cataclysmic Variables

Martino

Gänsicke

2009

Astrophys Space Sci

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Cataclysmic Variables are the most abundant population of galactic compact interacting binaries. They represent test objects to improve our knowledge of accretion theory as well as evolution of low-mass close binary systems. The UV domain represents a key range, linking the high energy emission to that of the optical domain, to understand the complex interplay of accretion and outflow processes, as well as to infer the physical status of the accreting primaries. Some of the major results and future needs in this range are discussed.

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“…The ultraviolet also encompasses a wide range of low and high excitation lines of a large variety of chemical species which are tracers of different plasma conditions as well as of individual components within the binary system. To obtain an overview of the ultraviolet properties of cataclysmic variables see Pringle and Verbunt (1984); Szkody (1985); Cordova and Howarth (1986); Gansicke et al (2006); de Martino and Gänsicke (2009).…”

Section: Introductionmentioning

confidence: 99%

Ultraviolet spectroscopy of V Sagittae in high, intermediate and low states from HST and IUE satellites

Sanad

2015

Astrophys Space Sci

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We present the first phase resolved ultraviolet spectroscopic study of V Sge in high, intermediate and low states observed with the Hubble Space Telescope High Resolution Spectrograph (HST HRS) and International Ultraviolet Explorer (IUE) during the period 1978-1996 to diagnose the ultraviolet fluxes of C IV 1550 Å and He II 1640 Å emission lines originating in the accretion disk during different orbital phases. Different spectra showing the variations in line fluxes at different orbital phases are presented. The reddening of V Sge is determined from the 2200 Å feature. We concentrated on calculating the line fluxes of C IV & He II emission lines. From HST and IUE data, we derived an accretion luminosity and an accretion rate for V Sge. The average temperature of the outer rim of the accretion disk ∼10000 K. Our results show that there are variations in line fluxes, accretion luminosities and accretion rates with time for V Sge. These variations are attributed to the variations of both density and temperature as a result of a changing rate of mass transfer from the secondary star to the white dwarf. These results from the HST and IUE observations are consistent with the binary model consisting of a white dwarf, a disk around the white dwarf, and a lobe-filling main-sequence companion (Hachisu & Kato, Astrophys. J. 598:527H, 2003).

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Ultraviolet Studies of Interacting Binaries

Cited by 12 publications

References 77 publications

An archive study of 18 old novae

An archive study of 18 old novae

UV observations of Cataclysmic Variables

Ultraviolet spectroscopy of V Sagittae in high, intermediate and low states from HST and IUE satellites

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