Ultraviolet Emission‐line Ratios of Cataclysmic Variables

Mauche, Christopher W.; Lee, Y. Paul; Kallman, T. R.

doi:10.1086/303717

Cited by 45 publications

(51 citation statements)

References 33 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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“…With regard to this question, Mauche et al (1997) discussed the case of UV line ratios of CVs, which seem to be almost independent of the nature (magnetic or not) of CVs. Okada et al (2008) found from CHANDRA HETG (High Energy Transmission Grating) observations in SS Cyg that the spectrum in quiescence is dominated by H-like K α lines, and is dominated in outburst by He-like lines, which are as intense as H-like lines.…”

Section: Introductionmentioning

confidence: 99%

An intrinsic source of reddening in the cataclysmic variable SS Cygni

Gaudenzi

Giovannelli

Mandalari

et al. 2010

A&A

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By using the INES archive of the IUE satellite, we analyzed the spectra of SS Cygni in quiescence in order to determine the value of the reddening of the binary system. The reddening of the system is reported in the literature with values that vary significantly from one another. The results demonstrate that the reddening is comprised by two components: the first, interstellar in origin, with a value E(B − V) = 0.04 ± 0.02 mag, and the second, intrinsic to the binary system, with values up to E(B − V) = 0.16 ± 0.02 mag. The intrinsic value of the reddening is variable along the quiescent phase and with orbital phase.

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“…The exception is the large nitrogen to oxygen ratio in GK Per, mirroring the unusual UV line ratios (Mauche et al 1997), and may suggest an abundance anomaly for this system with an evolved secondary (Kraft 1964). As with the cooling flow cases, the He-like triplets again exhibit conversion of the forbidden to intercombination lines, suggesting high electron density and/or a strong, ambient UV radiation field.…”

Section: Photoionized Spectramentioning

confidence: 93%

Two Types of X-ray Spectra in Cataclysmic Variables

Mukai

Kinkhabwala

Peterson

et al. 2004

International Astronomical Union Colloquium

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We present Chandra HETG spectra of seven cataclysmic variables. We find that they divide unambiguously into two distinct types. Spectra of the first type are remarkably well fit by a simple cooling flow model, which assumes only steady-state isobaric radiative cooling. The maximum temperature, kT max , and the normalization, which provides a highly precise measurement of the accretion rate, are the only free parameters of this model. Spectra of the second type are grossly inconsistent with a cooling flow model. They instead exhibit a hard continuum, and show strong H-like and He-like ion emission but little Fe L-shell emission, which is consistent with expectations for line emission from a photoionized plasma. Using a simple photoionization model, we argue that the observed line emission for these sources can be driven entirely by the hard continuum. The physical significance of these two distinct types of X-ray spectra is also explored.

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Ultraviolet Emission‐line Ratios of Cataclysmic Variables

Cited by 45 publications

References 33 publications

An archive study of 18 old novae

An archive study of 18 old novae

An intrinsic source of reddening in the cataclysmic variable SS Cygni

Two Types of X-ray Spectra in Cataclysmic Variables

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